koutchmy

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Author name code: koutchmy
ADS astronomy entries on 2022-09-14
author:"Koutchmy, Serge L."

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Title: Refraction and scattering in the atmosphere of the planet
Venus: The Lomonossov arc
Authors: Koutchmy, Serge
2022arXiv220706760K Altcode:
The main observations of 1761 by M. Lomonossov and those that followed
are recalled by extending the discussion to other remarkable visual
observations of the passages, then with more and more powerful imagers
producing images in profusion. The modern treatment of parasitic
effects is briefly recalled by focusing on the expert observation of
1761 which has recently been widely commented on and criticized. It
included a spurious effect called the "black drop effect". The shell
or aureole or atmospheric ring of Venus observed outside the solar
disk is considered with reference to the today parameters of the Venus
atmosphere. The contacts during the transit are discussed taking into
account effects of scattering, absorption and the dominant effects of
the refraction at the small angular distances found to be comparable to
a fraction of the angular dimension of the planet. Modern observations
of the 2004 and the 2012 transit are tentatively discussed to elucidate
what is the arc of Lomonossov?

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Title: Polarimetric Studies of a Fast Coronal Mass Ejection
Authors: Mierla, Marilena; Inhester, Bernd; Zhukov, Andrei N.; Shestov,
Sergei V.; Bemporad, Alessandro; Lamy, Philippe; Koutchmy, Serge
2022SoPh..297...78M Altcode: 2022arXiv220604411M
In this work we performed a polarimetric study of a fast and wide
coronal mass ejection (CME) observed on 12 July 2012 by the COR1 and
COR2 instruments onboard the Solar TErrestrial RElations Observatory
(STEREO) mission. The CME source region was an X1.4 flare located at
approximately S15W01 on the solar disk, as observed from the Earth's
perspective. The position of the CME as derived from the 3D Graduated
Cylindrical Shell (GCS) reconstruction method was at around S18W00
at 2.5 solar radii and S07W00 at 5.7 solar radii, meaning that the
CME was deflected towards the Equator while propagating outward in
the corona. The projected speed of the leading edge of the CME also
evolved from around 200 km s−1 in the lower corona to
around 1000 km s−1 in the COR2 field of view. The degree
of polarisation of the CME is around 65% but it can go as high as 80%
in some CME regions. The CME showed deviation of the polarisation
angle from the tangential in the range of 10 - 15∘ (or
more). Our analysis showed that this is mostly due to the fact that the
sequence of three polarised images from where the polarised parameters
are derived is not taken simultaneously, but at a difference of a few
seconds in time. In this interval of time, the CME moves by at least
two pixels in the FOV of the instruments and this displacement results
in uncertainties in the polarisation parameters (degree of polarisation,
polarisation angle, etc.). We propose some steps forward to improve the
derivation of the polarisation. This study is important for analysing
the future data from instruments with polarisation capabilities.

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Title: Polar regions activity and the prediction of the height of
the solar cycle 25
Authors: Koutchmy, S.; Filippov, B.; Tavabi, E.; Noens, J-C.;
Wurmser, O.
2022arXiv220509089K Altcode:
The forthcoming solar cycle (SC) 25 was beleived to be rather low
when using the sunspot number (SN) as a measurement of the level of
activity. The most popular prediction was made by the panel of NASA in
2019, including works based on extrapolations of dynamo-type models. We
however discovered that using different observations to measure the
level of polar regions activity several years before the start of SC25
and also after the start of the SC25 in 2020, the height of the SC25
could be high. The polar regions activity we considered seems related
to the polar coronal holes (CH) activity and it is found significantly
higher before the SC25 that it was before the SC24 and accordingly,
we suggest that the SN cycle could indeed be much higher than during
the SC24 that was a low SN height cycle.

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Title: Predicting the height of the solar cycle 25 through polar
regions activity
Authors: Koutchmy, S.; Tavabi, E.; Noëns, J. -C.; Wurmser, O.;
Filippov, B.
2021sf2a.conf..238K Altcode:
We describe and discuss the reasons why we believe the forthcoming solar
cycle (SC) 25 will be significantly higher than what was predicted by
NASA in 2019.

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Title: Polarimetric Coronagraphy to record the initiation of CMEs
Authors: Koutchmy, S.; Sèvre, F.; Rochain, S.; Noëns, J. -C.;
Pitout, F.
2021sf2a.conf..298K Altcode:
A new type of polarimetric coronagraph is proposed for permitting
citizen Astronomers and Amateurs involved in $H\alpha$ and coronal
observations using the Pic du Midi (PdM) Observatory Facilities
(so-called CLIMSO) to apprehend and analyze the dynamical processes
inside the solar corona. It includes relevant for economic reasons
observations of the initiation phase of Coronal Mass Ejections (CMEs)
and of recurrent geo-active quasi-polar coronal holes (CHs).

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Title: Solar Total Eclipse of 21 August 2017: Study of the Inner
Corona Dynamical Events Leading to a CME
Authors: Filippov, Boris; Koutchmy, Serge; Lefaudeux, Nicolas
2020SoPh..295...24F Altcode: 2020arXiv200110203F
Total solar eclipse (TSE) coronal large- and small-scale events
were reported in the historical literature but a definite synoptic
coverage was missing for studying a relationship with the more
general magnetic context of the solar-disk. We here analyze temporal
changes in the solar corona before, during, and after the total
solar eclipse on 21 August 2017 from a set of ground-based and of
space-borne observations. High-quality ground-based white-light (W-L)
observations and a deep image processing allow us to reveal these
changes for the first time with a fraction of a minute temporal
resolution. Displacements of a number of fine coronal features
were measured for the first time at these small radial distances,
using a diffraction-limited instrument at a single site. The
comparison with space-based observations, including observations
from the Solar Terrestrial Relations Observatory (STEREO) mission,
showed that the features belong to a slow coronal mass ejection (CME)
propagating through the corona with the nearly constant speed of 250 km
s−1. Our TSE images provide the same typical velocity as
measured at a distance of one solar radius from the surface. The event
was initiated by coronal dynamics manifested by a prominence eruption
that started just before the eclipse observations and an ascent of
a U-shaped structure visible in the Atmospheric Imaging Assembly
(AIA) 171 Å channel, which we assume as the lower part of a coronal
cavity. The prominence material was observed draining down towards the
chromosphere along the prominence arch. While the prominence disappears
in the STEREO-A field-of-view at the height of about 6' above the limb,
the corresponding flux rope seems to continue towards the outer corona
and produces the slow CME with turbulent motion. The overall mass of
the moving features is evaluated based on absolute photometrical data
extracted from our best W-L eclipse image.

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Title: Total solar eclipse 2017 in USA: deep coronal spectra
Authors: Koutchmy, S.; Baudin, F.; Abdi, Sh.; Golub, L.; Sèvre, F.
2019sf2a.conf..363K Altcode:
Total eclipses permit a deep analysis of both the inner and the
outer parts of the solar corona using the Thomson scattered (inverse
Compton effect on free electrons at millions degrees T^{\circ} )
continuum White- Light (W-L) radiations and the spectrum of forbidden
emission lines from hot highly ionized ions of iron, nickel, argon,
etc. Spectra are largely affected by the superposition of the solar
light scattered and diffracted by the interplanetary dust particles
orbiting the Sun at large distances but intercepted along the line
of sight (los)\citep{1973ApJ...186..671K}. Sometimes the parasitic
light due to multiple scattering from the ground and from the Earth
atmosphere should be removed using the light observed on the Moon image
background. After sufficiently dispersing the W-L corona, the Fraunhofer
(F) spectrum of the dust corona appears with its absorption (dark)
lines of known equivalent widths and the continuum Thomson radiation
can be extracted. The identified emission (bright) lines of ions with
different degrees of ionization are studied to permit an evaluation
of i/ relative abundances (compared to photospheric abundances), ii/
temperatures, iii/ non-thermal velocities and the resulting from the
analysis of the departures from a Gaussian profile of net Doppler shifts
after integration along the los. 60 spectra were obtained during the
totality using a specially designed slit spectroscopic experiment for
providing an accurate analysis of the most typical "broadly averaged"
parts of the quasi-minimum of activity type corona. With the scanning
+/- 3 solar radii long slit a .072 nm FWHM effective resolution
was obtained in the range of 510 to 590 nm. The background sky was
exceptionally clear during this US total eclipse of Aug. 21, 2017
as observed from our site in Idaho; spectra are without significant
parasitic light on the Moon disk. The K+F continuum corona is well
exposed up to at least 1 solar radius (Rs) from the limb and further
out with a lower S/N ratio, showing several forbidden coronal emission
lines. The F-corona can be measured even at the solar limb where its
intensity reached near 6\% of the K-corona intensity. Streamers, active
region enhancements and polar coronal holes (CHs) are well measured on
each 1 sec exposure time coronal spectra see Fig. \ref{author1:fig1};
the 2^{nd} contact showing the chromospheric and the most inner layers
emission lines was observed with a fast sequence and exposure time 10
times shorter. New weak emission lines were also discovered and/or
confirmed see Fig. \ref{author1:fig2} ; their identifications are
proposed. The rarely observed high FIP ArX \citep{2018ApJ...852...52D}
line is recorded almost everywhere and a new nearby FeX line is
well identified; the classical low FIP FeXIV and NiXIII lines are
well recorded everywhere without over-exposure. For the 1st time hot
lines are also measured at low levels inside the CH regions, at both
poles. The radial variations of the corrected non-thermal turbulent
velocities of the lines do not show a great departure from the average
values. No significantly large Doppler shifts are seen nowhere in
the inner and the middle corona although the whole corona is almost
covered.\citep{Koutchmy} The corona is confirmed to be made of a mixing
of hot and less hot components everywhere around the Sun, due to the
yet unidentified magnetic origin heating processes reflected in our
spectra and in the line profiles. Coronal density variations are well
reflected by the K-corona continuum intensity variations the azimuthal
and radial direction variations will permit the interpretation of the
emission measures to be compared with the simultaneously obtained AIA
images from the SDO space mission. The W-L images taken simultaneously
shows a much better spatial resolution with images of bright background
well known stars that permit to deduce an excellent absolute calibration
needed to deduce the electron densities and to check our F-corona model,
see \ref{author1:fig3}.

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Title: Eclipse 2017: new results on the dynamical inner-corona
Authors: Koutchmy, S.; Filippov, B.; Lecleire, J. M.; Lefaudeux, N.;
Mouette, J.; Sèvre, F.; Tavabi, E.; Viladrich, Ch.; Abdi, Sh.
2019sf2a.conf..361K Altcode:
The total solar eclipse of 21 Aug. 2017 was observed by our teams in
excellent conditions for almost 1 hour (from Oregon at 17h12, Idaho
17h27, see Fig. 1, Wyoming 17h36 and Missouri, 18h12 U.T.). Excellent
images were recorded in white-light (W-L), including a very high
spatial-temporal resolution (HR) sequence covering faint dynamical
phenomena related to an exceptionally slow CME that evolved over the
E-limb. In addition: i) The overall polarized K-corona, from linearly
polarized images taken in 12 positions with a green filter, was
analyzed, to be compared to the latest quantitative magnetic dynamical
coronal modeling of the Mikic team \citep{mikic2018predicting}. The
complex fine scale structure reflecting the magnetic field topology is
analyzed using specially designed algorithms with suggestion of a more
turbulent field in the outer corona above r= 2Rs. ii) The more simple
Polar- cap Regions are considered to compare the impressive fine- scale
more linear W-L plumes with the EUV plumes simultaneously observed
in the lower corona with the AIA filtergrams of the SDO mission;
we integrate 60 successive AIA images taken with the 171, 193, 211
Å filters to improve the S/N ratio of EUV frames. The new view of
dynamical polar plumes is illustrated at different temperature regimes,
including a high temperature regime. Some evidence of fast propagating
transverse waves is obtained by comparing deep spatially Fourier-
filtered W-L images of plumes and jets separated by typically 1 min
of time; amplitudes are larger for larger radial distances, suggesting
that they reflect the propagation of alfvenic disturbances and possibly
their dissipation. iii) The most notable dynamic phenomenon is analyzed
at the E- limb: it is a slow CME that shows a constant 250 km/s velocity
from the LASCO (SoHO) observations. It is analyzed here in W-L with HR
eclipse images and with images from the SECCHI EUV filtergrams of the
STEREO mission and from the AIA of the SDO mission. Very small scale
and faint moving and curved W-L features at r= 1.7 Rs, possibly owning
to high disrupted loops, are analyzed for the 1st time with a 20 sec
temporal resolution movie; falling back remnants of the erupted high
latitude polar crown filament- prominence found at the feet of the CME
are detected in W-L, well after the eruption. It is suggested that
such processes are a component of the slow wind that is more easily
demonstrated at time of this minimum corona using eclipse images in
the r = 1.5 to 2 Rs region where instabilities grow and outwardly
propagate.( \citet{1997Kout} \citet{2018Tavabi})

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Title: New deep coronal spectra from the 2017 total solar eclipse
Authors: Koutchmy, S.; Baudin, F.; Abdi, Sh.; Golub, L.; Sèvre, F.
2019A&A...632A..86K Altcode: 2019arXiv191001372K
Context. The origin of the high temperature of the solar corona, in
both the inner bright parts and the more outer parts showing flows
toward the solar wind, is not understood well yet. Total eclipses
permit a deep analysis of both the inner and the outer parts of the
corona using the continuum white-light (W-L) radiations from electrons
(K-corona), the superposed spectrum of forbidden emission lines from
ions (E-corona), and the dust component with F-lines (F-corona). 
Aims: By sufficiently dispersing the W-L spectrum, the Fraunhofer (F)
spectrum of the dust component of the corona appears and the continuum
Thomson radiation can be evaluated. The superposed emission lines
of ions with different degrees of ionization are studied to allow the
measurement of temperatures, non-thermal velocities, Doppler shifts, and
abundances to constrain the proposed heating mechanisms and understand
the origin of flows that lead to solar wind. Methods: We describe
a slit spectroscopic experiment of high spectral resolution to provide
an analysis of the most typical parts of the quasi-minimum type corona
observed during the total solar eclipse of Aug. 21, 2017 from Idaho,
USA. Streamers, active region enhancements, and polar coronal holes
(CHs) are measured well using deep spectra. Results: Sixty
spectra are obtained during the totality with a long slit, covering ±3
solar radii in the range of 510 nm to 590 nm. The K+F continuum corona
is exposed well up to two solar radii. The F-corona can be measured
even at the solar limb. New weak emission lines were discovered or
confirmed. The rarely observed Ar X line is detected almost everywhere;
the Fe XIV and Ni XIII lines are clearly detected everywhere. For
the first time hot lines are also measured inside the CH regions. The
radial variations of the non-thermal turbulent velocities of the lines
do not show a great departure from the average values. No significantly
large Doppler shifts are seen anywhere in the inner or the middle
corona. The wings of the Fe XIV line show some non-Gaussianity. Conclusions: Deep slit coronal spectra offered an opportunity for
diagnosing several aspects of coronal physics during a well observed
total eclipse without extended investments. The analysis of the ionic
emission line profiles offers several powerful diagnostics of the
coronal dynamics; the precise measurement of the F-continuum component
provides insight into the ubiquitous dust corona at the solar limb.

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Title: Pointing the NTT at the Sun: Studying the Solar Corona During
the Total Eclipse
Authors: Dennefeld, M.; Koutchmy, S.; Sèvre, F.; Fathivavsari,
H.; Auchère, F.; Baudin, F.; Abdi, S.; Sinclaire, P.; Saviane, I.;
Labraña, F.; Schmidtobreick, L.
2019Msngr.177...54D Altcode:
No abstract at ADS

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Title: Chromospheric Peculiar Off-limb Dynamical Events from IRIS
Observations
Authors: Tavabi, E.; Koutchmy, S.
2019ApJ...883...41T Altcode: 2019arXiv190710960T
To study motions and oscillations in the solar chromosphere and at
the transition region level we analyze some extreme Doppler shifts
observed off-limb with the Interface Region Imaging Spectrograph
(IRIS). Raster scans and slit-jaw imaging observations performed in the
near-ultraviolet channels were used. Large transverse oscillations are
revealed by the far wings profiles after accurately removing the bulk
average line profiles of each sequence. Different regions around the Sun
are considered. Accordingly, the cool material of spicules is observed
in Mg II lines rather dispersed up to coronal heights. In the quiet Sun
and especially in a polar coronal hole, we study dynamical properties of
the dispersed spicules-material off-limb using high spectral, temporal,
and spatial resolutions IRIS observations. We suggest that numerous
small-scale jet-like spicules show rapid twisting and swaying motions
evidenced by the large distortion and dispersion of the line profiles,
including impressive periodic Doppler shifts. Most of these events
repeatedly appear in red and blueshifts above the limb throughout the
whole interval of the observation data sets, with an average swaying
speed of order ±35 km s-1 reaching a maximum value of 50 km
s-1 in the polar coronal hole region, well above the 2.2 Mm
heights. We identified for the first time waves with a short period of
order of 100 s, and less and transverse amplitudes of order of ±20-30
km s-1 with the definite signature of Alfvén waves. No
correlation exists between brightness and Doppler shift variations;
the phase speed of the wave is very large and cannot definitely be
determined from the spectral features seen along the quasi-radial
features. Even shorter periods waves are evidenced, although their
contrast is greatly attenuated by the overlapping effects along the
line of sight.

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Title: Atmospheric Emission Layers according to Photographic
Observations from the International Space Station
Authors: Platov, Yu. V.; Koutchmy, S.; Nikolayshvili, S. Sh.
2019Ge&Ae..59..351P Altcode:
No abstract at ADS

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Title: Polar Coronal Plumes as Tornado-like Jets
Authors: Tavabi, E.; Koutchmy, S.; Golub, L.
2018ApJ...866...35T Altcode: 2018arXiv180807322T
We examine the dynamical behavior of white-light polar-plume
structures in the inner corona that are observed from the ground
during total solar eclipses, based on their extreme ultraviolet (EUV)
hot and cool emission line counterparts observed from space. EUV
observations from Solar Dynamics Observatory/Atmospheric Imaging
Assembly (SDO/AIA) of a sequence of rapidly varying coronal hole
structures are analyzed. Evidence of events showing acceleration in
the 1.25 Mk line of Fe XII at 193 Å is given. The structures along
the plume show an outward velocity of about 140 km s-1
that can be interpreted as an upward propagating wave in the 304 Å
and 171 Å lines; higher speeds are seen in 193 Å (up to 1000 km
s-1). The ejection of the cold He II plasma is delayed
by about 4 minutes in the lowest layer and is delayed more than 12
minutes in the highest level compared to the hot 193 Å behavior. A
study of the dynamics using time-slice diagrams reveals that a large
amount of fast ejected material originates from below the plume, at
the footpoints. The release of plasma material appears to come from
a cylinder with quasi-parallel edge-enhanced walls. After the initial
phase of a longitudinal acceleration, the speed substantially reduces,
and the ejecta disperse into the environment. Finally, the detailed
temporal and spatial relationships between the cool and hot components
were studied with simultaneous multiwavelength observations, using
more AIA data. The outward-propagating perturbation of the presumably
magnetic walls of polar plumes supports the suggestion that Alfvén
waves propagate outwardly along these radially extended walls.

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Title: Evidence of cool prominence material embedded in CMEs from
polarization measurements
Authors: Lamy, Philippe; Floyd, Olivier; Koutchmy, Serge
2018cosp...42E1930L Altcode:
In white-light coronagraph images, cool prominence material is
sometimes observed as bright substructures or plasmoids in coronal mass
ejections (CMEs). Based on observations of a CME with the SECCHI/STEREO
coronagraphs on 31 August 2007, Mierla et al. (2011) have shown that
the emission from such bright patches is characterized by very low
polarization and was due to H-alpha radiation from cool prominence
material. We have examined several polarization images of CMEs obtained
with the LASCO-C2 coronagraph with its orange filter. This filter is
approximately centered on the HeI D3 line. This low excitation line
emission is superior to the H-alpha emission of HI because its FIP
is much higher. In several cases, we observe very low-polarization
components embedded in CMEs characterized by a much larger polarization
resulting from the Thomson scattering. They most likely present evidence
of cool prominence material carried by the CMEs.

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Title: Observation of galactic cosmic ray spallation events from
the SoHO mission 20-yr operation of LASCO
Authors: Koutchmy, S.; Tavabi, E.; Urtado, O.
2018MNRAS.478.1265K Altcode: 2018MNRAS.tmp.1151K; 2018arXiv180504930K
A shower of secondary cosmic ray (CR) particles is produced at high
altitudes in the Earth's atmosphere, so the primordial galactic cosmic
rays (GCRs) are never directly measured outside the Earth magnetosphere
and atmosphere. They approach the Earth and other planets in the
complex pattern of rigidity's dependence, generally excluded by the
magnetosphere. GCRs revealed by images of single nuclear reactions
also called spallation events are described here. Such an event was
seen on 2015 November 29 using a unique Large Angle and Spectrometric
Coronagraphs C3 space coronagraph routine image taken during the Solar
and Heliospheric Observatory (SoHO) mission observing uninterruptedly at
the Lagrangian L1 point. The spallation signature of a GCR identified
well outside the Earth's magnetosphere is obtained for the first
time. The resulting image includes different diverging linear `tracks'
of varying intensity, leading to a single pixel; this frame identifies
the site on the silicon CCD chip of the coronagraph camera. There was
no solar flare reported at that time, nor coronal mass ejection and
no evidence of optical debris around the spacecraft. More examples of
smaller CR events have been discovered through the 20 yr of continuous
observations from SoHO. This is the first spallation event from a CR,
recorded outside the Earth's magnetosphere. We evaluate the probable
energy of these events suggesting a plausible galactic source.

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Title: Proper Motions of Sunspots’ Umbral Dots at High Temporal
and Spatial Resolution
Authors: Goodarzi, Hadis; Koutchmy, Serge; Adjabshirizadeh, Ali
2018ApJ...860..168G Altcode: 2018arXiv180705531G
To deepen the analysis of the photometric properties of the umbra of a
sunspot, we study proper motions of small features such as umbral dots
(UDs) inside a single sunspot observed by the Solar Optical Telescope
of Hinode close to the disk center. We consider horizontal flows with
high precision and details to study the transient motion behavior
of UDs in short time intervals. Blue continuum images were first
deconvolved with the point-spread function, such that the stray light
is precisely removed and the original resolution is improved. Several
images were co-added to improve the signal-to-noise ratio, keeping
a reasonable temporal resolution and checking that the results are
reproducible. The Fourier local correlation tracking technique is
applied to the new corrected time sequence of images, and horizontal
velocity maps were obtained both for the whole umbra (16″ × 12″)
and for a high-resolution small region of the umbra (3.″5 × 3.″5)
to study the smallest details of the velocity fields. We used two
different Gaussian tracking windows (0.8 and 0.″2 ), which reveals two
types of horizontal motions for umbral features. First, a global inner
penumbra and peripheral umbra inward motion directed to the central
parts is revealed as an overall proper motion of bright peripheral fine
structures. Second, motions matching small cells inside the darkest
parts of the umbra with apparent sink and source areas are revealed,
suggesting possible upflows and downflows appearing in different bright
and dark locations without a definite answer regarding their brightness
identification with a convective or a buoyant cell.

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Title: Analysis of a Failed Eclipse Plasma Ejection Using EUV
Observations
Authors: Tavabi, E.; Koutchmy, S.; Bazin, C.
2018SoPh..293...42T Altcode: 2018arXiv180109222T
The photometry of eclipse white-light (W-L) images showing a moving
blob is interpreted for the first time together with observations from
space with the PRoject for On Board Autonomy (PROBA-2) mission (ESA). An
off-limb event seen with great details in W-L was analyzed with the
SWAP imager (Sun Watcher using Active pixel system detector and image
Processing) working in the EUV near 174 Å. It is an elongated plasma
blob structure of 25 Mm diameter moving above the east limb with coronal
loops under. Summed and co-aligned SWAP images are evaluated using a
20-h sequence, in addition to the 11 July, 2010 eclipse W-L images taken
from several sites. The Atmospheric Imaging Assembly (AIA) instrument on
board the Solar Dynamics Observatory (SDO) recorded the event suggesting
a magnetic reconnection near a high neutral point; accordingly, we also
call it a magnetic plasmoid. The measured proper motion of the blob
shows a velocity up to 12 kms−1. Electron densities of the
isolated condensation (cloud or blob or plasmoid) are photometrically
evaluated. The typical value is 108cm−3
at r =1.7 R⊙, superposed on a background corona of
107cm−3 density. The mass of the cloud
near its maximum brightness is found to be 1.6 ×1013 g,
which is typically 0.6 ×10−4 of the overall mass of
the corona. From the extrapolated magnetic field the cloud evolves
inside a rather broad open region but decelerates, after reaching its
maximum brightness. The influence of such small events for supplying
material to the ubiquitous slow wind is noticed. A precise evaluation
of the EUV photometric data, after accurately removing the stray light,
suggests an interpretation of the weak 174 Å radiation of the cloud
as due to resonance scattering in the Fe IX/X lines.

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Title: Preliminary optical design of the coronagraph for the ASPIICS
formation flying mission
Authors: Vivès, S.; Lamy, P.; Saisse, M.; Boit, J. -L.; Koutchmy, S.
2017SPIE10567E..1WV Altcode:
Formation flyers open new perspectives and allow to conceive
giant, externally-occulted coronagraphs using a two-component space
system with the external occulter on one spacecraft and the optical
instrument on the other spacecraft at approximately 100-150 m from
the first one. ASPIICS (Association de Satellites Pour l'Imagerie
et l'Interfromtrie de la Couronne Solaire) is a mission proposed
to ESA in the framework of the PROBA-3 program of formation flying
which is presently in phase A to exploit this technique for coronal
observations. ASPIICS is composed of a single coronagraph which performs
high spatial resolution imaging of the corona as well as 2-dimensional
spectroscopy of several emission lines from the coronal base out to
3 R. The selected lines allow to address different coronal regions:
the forbidden line of Fe XIV at 530.285 nm (coronal matter), Fe IX/X at
637.4 nm (coronal holes), HeI at 587.6 nm (cold matter). An additional
broad spectral channel will image the white light corona so as to derive
electron densities. The classical design of an externally occulted
coronagraph is adapted to the detection of the very inner corona as
close as 1.01 R and the addition of a Fabry-Perot interferometer using
a so-called "etalon". This paper is dedicated to the description of
the optical design and its critical components: the entrance optics
and the FabryPerot interferometer.

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Title: Stray light rejection in giant externally-occulted solar
coronagraphs: experimental developments
Authors: Venet, M.; Bazin, C.; Koutchmy, S.; Lamy, P.
2017SPIE10565E..1WV Altcode:
The advent of giant, formation-flight, externally-occulted solar
coronagraphs such as ASPIICS (Association de Satellites Pour l'Imagerie
et l'Interférométrie de la Couronne Solaire [1,2,3,4]) selected
by the European Space Agency (ESA) for its third PROBA (Project for
On-Board Autonomy) mission of formation flying demonstration (presently
in phase B) and Hi-RISE proposed in the framework of ESA Cosmic Vision
program, presents formidable challenges for the study and calibration of
instrumental stray light. With distances between the external occulter
(EO) and the optical pupil (OP) exceeding hundred meters and occulter
sizes larger than a meter, it becomes impossible to perform tests at
the real scale. The requirement to limit the over-occultation to less
than 1.05 Rsun, orders of magnitude to what has been achieved so far in
past coronagraphs, further adds to the challenge. We are approaching
the problem experimentally using reduced scale simulators and present
below a progress report of our work.

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Title: Improved SOT (Hinode mission) high resolution solar imaging
observations: 2—Photometric properties of sunspot umbral dots
Authors: Goodarzi, H.; Koutchmy, S.; Adjabshirizadeh, A.
2016Ap&SS.361..366G Altcode:
The origin and evolution of solar sunspots in deep photospheric layers
are not yet well understood. The case of a quasi-symmetric single
mature sunspot near the solar centre is selected for analysis. We use
the best available observations of the partial Sun free of turbulent
Earth atmospheric effects from the Solar Optical Telescope (SOT)
onboard the Hinode spacecraft, after greatly improving the resolution
with an optimum Max-likelihood deconvolution with the Point Spread
Function (PSF) deduced in a preceding paper. For several different
images both the smearing due to the instrumental diffraction effects
(PSF core) and the large angle stray light are removed. The selected
iterative processing depends on both the signal/noise ratio and on
the desired contrast of the ultimate details under examination. The
photometric properties of bright umbral dots (BUDs) are deduced from
corrected frames. Calibrated isophote maps are provided to show the
intensity variations around each UD across the background umbra and
the surrounding photospheric field, including the penumbra. We deduce
the typical photometrical properties of bright UDs that populate
the whole umbral surface down to sub-pixel scales of 0.05448”. The
analysis demonstrates the basic heterogeneous nature of the umbra,
similar to a network of minute bright and dark round or elongated
cells with a spacing of order of 0.35”. For the first time a complete
and detailed map of the color index and temperature deduced from the
analysis of deeply corrected continuum images is provided, showing
that tiny bright UDs can reach photospheric temperatures and even
higher for the peripheral BUDs. In the umbra, there are some very
dark small regions with temperatures as low as 3100 K. Close links
seemingly exist with bright UDs. Central BUDs and peripheral BUDs are
found to have similar properties but significantly different contrast
values. Photometric analysis shows a large dispersion that reflects
the broad range of dynamical phenomena involved in the umbra and its
periphery, suggesting that the small scale activity observed in the
deepest measured photospheric layers of the umbra determines the more
impressive rapid phenomena observed in higher layers.

---------------------------------------------------------
Title: Multiple Null Point Reconnections in a limb faint cool jet
ejection event
Authors: Tavabi, E.; Koutchmy, S.
2016aiaw.conf..127T Altcode:
Giant spicules and macro- spicules are an important extended
rather cool structure between the solar surface and the corona,
partly filling the space inside the chromosphere and surrounded by a
transition thin region. Their formation and dynamical properties are
still mysterious. In order to explain solar limb and disc periodic
recurrences of these events, a simulation model assuming quasi-
random positions of spicules above the solar limb was studied. We
allow a set number of spicules with different physical properties
(such as height, lifetime and tilt angle as shown by an individual
spicule) randomly occurring. It is assumed that after reaching a
maximum length, the spicules are less rapidly falling back to the
solar surface. This kind of limb event was often reported in the
literature (spike; giant spicule; Ha ejection event; spray etc) but no
serious quantitative analysis could be done. Indeed from ground-based
observations, it is impossible to deduce precised parameters because
the earth atmospheric turbulent effects makes impossible to make
small scale measurements. SOT space-borne observations we use are
unique in providing well reproducible observations permitting very
precise measurements. The study of X-ray jets is an important topic to
understand the heating of the solar corona and the origin of the fast
wind. The recently launched Hinode mission permitted to observe the cool
proxies of these jets with an unprecedented high spatial resolution of
120 km on the Sun. We selected a high cadence sequence of SOT (Hinode)
observations taken with both the HCaII and the Hα filter to look at the
details of the dynamics revealed by a large jet event. Both wavelet and
amplitude spectra analysis were used to analyze the observed kink wave
and the time variations of intensities during the event. The results
are discussed in the frame of different models implying reconnections
with the inference of the dynamical phenomena occurring in the vicinity
of several null points, including the oscillatory behavior.

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Title: An airborne infrared spectrometer for solar eclipse
observations
Authors: Samra, Jenna; Cheimets, Peter; DeLuca, Edward; Galeros,
John; Gauron, Thomas; Golub, Leon; Guth, Giora; Hertz, Edward; Judge,
Philip; Koutchmy, Serge; Marquez, Vanessa
2016SPIE.9908E..5US Altcode:
This paper presents the design of an innovative solar spectrometer
that will y on the NSF/NCAR Gulfstream V High-Performance Instrumented
Airborne Platform for Environmental Research (GV HIAPER) during the
2017 solar eclipse. The airborne infrared spectrometer (AIR-Spec) is
groundbreaking in two aspects: it will image infrared coronal emission
lines that have never been measured, and it will bring high resolution
imaging to GV HIAPER. The instrument development faces the challenges
of achieving adequate resolution and signal-to-noise ratio in a compact
package mounted to a noisy moving platform. To ensure that AIR-Spec
meets its research goals, the instrument is undergoing pre-flight
modeling and testing. The results are presented with reference to the
instrument requirements.

---------------------------------------------------------
Title: Prominence material embedded in coronal mass ejections as
observed with the LASCO-C2 coronagraph using polarization diagnostic
Authors: Lamy, Philippe; Boclet, Brice; Koutchmy, Serge
2016cosp...41E1107L Altcode:
Prominences are believed to be caused by the formation of a flux
rope low in the magnetic structure that eventually erupts to form
the CME. Indeed, many CME onset models (e.g., flux cancellation,
mass loading) require the presence or formation of a prominence
in order for the CME to erupt. The remnants of the cool prominence
material is often seen as recognizable twisted structures inside the
CME in the lines of He II at 304 Å, of D3 HeI at 587.5 nm, and of
Hα at 656 nm, sometime up to a distance of several solar radii from
the surface in the latter lines. The orange filter of the LASCO-C2
coronagraph includes the D3 HeI line and its presence in the core of
CMEs can be unambiguously detected on polarized images as polarization
allows disentangling the contributions from the hot coronal plasma
(the polarized Thomson scattered light by electrons) and from the
unpolarised emission of cool prominence material. This has been made
possible by an in-depth calibration that removes adverse instrumental
effects. We will show several examples of CME with embedded prominence
material and we will attempt to estimate the mass of this material to
be compared with that of the CME. We will also exploit the polarization
measurements to reconstruct the 3D geometry of the observed CMEs.

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Title: Photometric analysis of the corona during the 20 March 2015
total solar eclipse: density structures, hydrostatic temperatures
and magnetic field inference.
Authors: Bazin, C.; Vilinga, J.; Wittich, R.; Koutchmy, S.; Mouette,
J.; Nitschelm, C.
2015sf2a.conf..259B Altcode: 2015arXiv151006436B
We present some new accurate CCD photometry analysis of the white
light solar corona at the time of the last 20 March 2015 total eclipse
(airborne observations on a Falcon 7X and at ground-based- Svalbard). We
measured coronal brightness profiles taken along radial directions from
1.001 to 3 solar radii in the northern, southern and equatorial regions,
after removing the F-corona and the sky background. These studies
allow to evaluate the density gradients, structures and temperature
heterogeneity, by considering the Thomson scattering in white light
of the K- corona and also emissions of the EUV Fe XII 193A (1 to 2 MK)
and Fe XI 171/174 (lower temperature) simultaneously observed by SDO/AIA
and SWAP/Proba2 space missions. Some dispersion between the regions is
noticed. The limitation of the hydrostatic equilibrium assumption in
the solar atmosphere is discussed as well as the contribution of the
magnetic field pressure gradients as illustrated by a comparison with
the model stationary magnetic corona from Predictive Sc. Inc. These
results are compared with the results of the quieter 2010 total solar
eclipse corona analyzed with the same method. This photometric analysis
of the inner and intermediate white light corona will contribute to the
preparation of the Aspiics/Proba 3 flying formation future coronagraphic
mission of ESA for new investigation at time of artificial eclipses
produced in Space. Note that Aspiics will also observe in the He I D3
line at 5876 A, and will record intensities of the Fe XIV line 5303A
simultaneously with the analysis of the orange white- light continuum,
including precise polarimetry analysis. .

---------------------------------------------------------
Title: Limb Event Brightenings and Fast Ejection Using IRIS Mission
Observations
Authors: Tavabi, E.; Koutchmy, S.; Golub, L.
2015SoPh..290.2871T Altcode: 2015SoPh..tmp..118T; 2015arXiv150706794T
The Interface Region Imaging Spectrograph (IRIS) of the recently
commissioned NASA small explorer mission provides significantly more
complete and higher resolution spectral coverage of the dynamical
conditions inside the chromosphere and transition region (TR) than has
been available ever before. High temporal, spatial (0.3″)
and spectral resolution observations from the ultraviolet IRIS spectra
near the solar limb reveal high-energy limb event brightenings (LEBs)
at low chromospheric heights at about 1 Mm above the limb. They can be
characterized as explosive events producing jets. We selected two events
showing spectra of a confined eruption just off or near the quiet-Sun
limb, the jet part showing obvious moving material with short-duration
large Doppler shifts in three directions that were identified as
macrospicules on slit-jaw (SJ) images in Si IV and He II 304 Å. The
events were analyzed from a sequence of very close rasters taken near
the central meridian and the South Pole limb. We analyzed the processed
SJ images and the simultaneously observed fast spectral sequences, which
have large Doppler shifts, with a pair of redshifted elements together
with a faster blueshifted element from almost the same position. Shifts
correspond to velocities of up to 100 kms−1 in projection
on the plane of the sky. Erupting spicules and macrospicules from these
regions are visible in images taken before and after the spectra. The
cool low first ionization potential (FIP) element simultaneous line
emissions of the Mg II h and k resonance lines do not clearly show a
similar signature because of optical thickness effects, but the Si IV
broadband SJ images do. The bidirectional plasma jets ejected from a
small reconnection site are interpreted to be the result of coronal
loop-loop interactions that lead to reconnection in nearby sites.

---------------------------------------------------------
Title: A Novel Technique for Measuring the Solar Radius from Eclipse
Light Curves - Results for 2010, 2012, 2013, and 2015
Authors: Lamy, Philippe; Prado, Jean-Yves; Floyd, Olivier; Rocher,
Patrick; Faury, Guillaume; Koutchmy, Serge
2015SoPh..290.2617L Altcode: 2015SoPh..tmp..170L
We report on a novel technique for measuring the solar radius during
total solar eclipses that exploits light curves recorded just before
and after second and third contacts. The measurements are performed by
pre-programmed photometers that are deployed over the eclipse paths and
are operated without supervision. The recorded light curves are compared
to synthetic light curves calculated from high-accuracy ephemerides
and lunar-limb profiles constructed from the topographic model of the
Moon provided by the Kaguya lunar space mission. A minimization process
between the two sets of curves yields the solar radius. Altogether,
seventeen determinations have been obtained during the past four total
eclipses with the following averages (at a wavelength of 540 nm and
scaled to 1 AU): 959.94 ±0.02 arcsec on 11 July 2010, 960.02 ±0.04
arcsec on 13 November 2012, 959.99 ±0.09 arcsec on 3 November 2013, and
960.01 ±0.09 arcsec on 20 March 2015. Part of the differences between
these four values may be attributed to weather conditions. Averaging
the whole set of measurements yields a radius of 959.99 ±0.06 arcsec
(696 ,246 ±45 km), which agrees excellently well with the most recent
data and supports an upward revision of the standard IAU value, as
previously suggested.

---------------------------------------------------------
Title: Design and modelisation of ASPIICS optics
Authors: Galy, C.; Fineschi, S.; Galano, D.; Howard, R. A.; Kintziger,
C.; Kirschner, V.; Koutchmy, S.; Lamy, P.; Mazzoli, A.; Melich, R.;
Mestreau-Garreau, A.; Renotte, E.; Servaye, J. S.; Stockman, Y.;
Thizy, C.; Zhukov, A.
2015SPIE.9604E..0BG Altcode:
In the framework of development of ASPIICS (Association of Spacecraft
for Polarimetric and Imaging Investigation of the Corona of the Sun),
the Centre Spatial de Liege is responsible of the optical design of
the coronagraph and the optics will be manufactured by TOPTEC. The
particularity of this coronagraph is to have an external occulter
located 150 m ahead of the first imaging lens. This external occulter
is re-imaged on an internal occulter which function is - as in a
classical externally occulted Lyot coronagraph - to block the sun
light diffracted by the external occulter and to reduce the straylight
on the detector. The selection of this configuration is driven by the
requirement to observe the corona as close as possible to the solar limb
(i.e. 1 RSun) without imaging the limb itself. A requirement
of 1.08 RSun is specified at optical design level to grant
1.2 Rsun at instrument level. The coronograph instrument is
designed to have a field of view of 1.6° x 1.6° with a resolution of
less than 6 arcsec. Its performances are limited by diffraction in a
530 - 590 nm wavelength range. This paper presents the optical design
and demonstrates that by design the requirements are fulfilled within
the misalignment, manufacturing and thermo-elastic error contributions.

---------------------------------------------------------
Title: Design status of ASPIICS, an externally occulted coronagraph
for PROBA-3
Authors: Renotte, Etienne; Alia, Andres; Bemporad, Alessandro;
Bernier, Joseph; Bramanti, Cristina; Buckley, Steve; Capobianco,
Gerardo; Cernica, Ileana; Dániel, Vladimir; Darakchiev, Radoslav;
Darmetko, Marcin; Debaize, Arnaud; Denis, François; Desselle,
Richard; de Vos, Lieve; Dinescu, Adrian; Fineschi, Silvano;
Fleury-Frenette, Karl; Focardi, Mauro; Fumel, Aurélie; Galano,
Damien; Galy, Camille; Gillis, Jean-Marie; Górski, Tomasz; Graas,
Estelle; Graczyk, Rafał; Grochowski, Konrad; Halain, Jean-Philippe
A.; Hermans, Aline; Howard, Russ; Jackson, Carl; Janssen, Emmanuel;
Kasprzyk, Hubert; Kosiec, Jacek; Koutchmy, Serge; Kovačičinová,
Jana; Kranitis, Nektarios; Kurowski, Michał; Ładno, Michał; Lamy,
Philippe; Landini, Federico; Lapáček, Radek; Lédl, Vít.; Liebecq,
Sylvie; Loreggia, Davide; McGarvey, Brian; Massone, Giuseppe; Melich,
Radek; Mestreau-Garreau, Agnes; Mollet, Dominique; Mosdorf, Łukasz;
Mosdorf, Michał; Mroczkowski, Mateusz; Muller, Raluca; Nicolini,
Gianalfredo; Nicula, Bogdan; O'Neill, Kevin; Orleański, Piotr;
Palau, Marie-Catherine; Pancrazzi, Maurizio; Paschalis, Antonios;
Patočka, Karel; Peresty, Radek; Popescu, Irina; Psota, Pavel; Rataj,
Miroslaw; Rautakoski, Jan; Romoli, Marco; Rybecký, Roman; Salvador,
Lucas; Servaye, Jean-Sébastien; Solomon, Cornel; Stockman, Yvan;
Swat, Arkadiusz; Thizy, Cédric; Thomé, Michel; Tsinganos, Kanaris;
Van der Meulen, Jim; Van Vooren, Nico; Vit, Tomáš; Walczak, Tomasz;
Zarzycka, Alicja; Zender, Joe; Zhukov, Andrei
2015SPIE.9604E..0AR Altcode:
The "sonic region" of the Sun corona remains extremely difficult to
observe with spatial resolution and sensitivity sufficient to understand
the fine scale phenomena that govern the quiescent solar corona,
as well as phenomena that lead to coronal mass ejections (CMEs),
which influence space weather. Improvement on this front requires
eclipse-like conditions over long observation times. The space-borne
coronagraphs flown so far provided a continuous coverage of the external
parts of the corona but their over-occulting system did not permit to
analyse the part of the white-light corona where the main coronal mass
is concentrated. The proposed PROBA-3 Coronagraph System, also known
as ASPIICS (Association of Spacecraft for Polarimetric and Imaging
Investigation of the Corona of the Sun), with its novel design, will
be the first space coronagraph to cover the range of radial distances
between ~1.08 and 3 solar radii where the magnetic field plays a crucial
role in the coronal dynamics, thus providing continuous observational
conditions very close to those during a total solar eclipse. PROBA-3
is first a mission devoted to the in-orbit demonstration of precise
formation flying techniques and technologies for future European
missions, which will fly ASPIICS as primary payload. The instrument
is distributed over two satellites flying in formation (approx. 150m
apart) to form a giant coronagraph capable of producing a nearly perfect
eclipse allowing observing the sun corona closer to the rim than ever
before. The coronagraph instrument is developed by a large European
consortium including about 20 partners from 7 countries under the
auspices of the European Space Agency. This paper is reviewing the
recent improvements and design updates of the ASPIICS instrument as
it is stepping into the detailed design phase.

---------------------------------------------------------
Title: Improved SOT (Hinode mission) high resolution solar imaging
observations
Authors: Goodarzi, H.; Koutchmy, S.; Adjabshirizadeh, A.
2015Ap&SS.358...25G Altcode: 2015arXiv150608265G
We consider the best today available observations of the Sun free
of turbulent Earth atmospheric effects, taken with the Solar Optical
Telescope (SOT) onboard the Hinode spacecraft. Both the instrumental
smearing and the observed stray light are analyzed in order to improve
the resolution. The Point Spread Function (PSF) corresponding to the
blue continuum Broadband Filter Imager (BFI) near 450 nm is deduced
by analyzing (i) the limb of the Sun and (ii) images taken during the
transit of the planet Venus in 2012. A combination of Gaussian and
Lorentzian functions is selected to construct a PSF in order to remove
both smearing due to the instrumental diffraction effects (PSF core) and
the large-angle stray light due to the spiders and central obscuration
(wings of the PSF) that are responsible for the parasitic stray light. A
Max-likelihood deconvolution procedure based on an optimum number of
iterations is discussed. It is applied to several solar field images,
including the granulation near the limb. The normal non-magnetic
granulation is compared to the abnormal granulation which we call
magnetic. A new feature appearing for the first time at the extreme-
limb of the disk (the last 100 km) is discussed in the context of the
definition of the solar edge and of the solar diameter. A single sunspot
is considered in order to illustrate how effectively the restoration
works on the sunspot core. A set of 125 consecutive deconvolved images
is assembled in a 45 min long movie illustrating the complexity of
the dynamical behavior inside and around the sunspot.

---------------------------------------------------------
Title: Inferring the Structure of the Solar Corona and Inner
Heliosphere During the Maunder Minimum Using Global Thermodynamic
Magnetohydrodynamic Simulations
Authors: Riley, Pete; Lionello, Roberto; Linker, Jon A.; Cliver,
Ed; Balogh, Andre; Beer, Jürg; Charbonneau, Paul; Crooker, Nancy;
DeRosa, Marc; Lockwood, Mike; Owens, Matt; McCracken, Ken; Usoskin,
Ilya; Koutchmy, S.
2015ApJ...802..105R Altcode:
Observations of the Sun’s corona during the space era have led to
a picture of relatively constant, but cyclically varying solar output
and structure. Longer-term, more indirect measurements, such as from
10Be, coupled by other albeit less reliable contemporaneous
reports, however, suggest periods of significant departure from this
standard. The Maunder Minimum was one such epoch where: (1) sunspots
effectively disappeared for long intervals during a 70 yr period; (2)
eclipse observations suggested the distinct lack of a visible K-corona
but possible appearance of the F-corona; (3) reports of aurora were
notably reduced; and (4) cosmic ray intensities at Earth were inferred
to be substantially higher. Using a global thermodynamic MHD model,
we have constructed a range of possible coronal configurations for the
Maunder Minimum period and compared their predictions with these limited
observational constraints. We conclude that the most likely state of the
corona during—at least—the later portion of the Maunder Minimum was
not merely that of the 2008/2009 solar minimum, as has been suggested
recently, but rather a state devoid of any large-scale structure,
driven by a photospheric field composed of only ephemeral regions,
and likely substantially reduced in strength. Moreover, we suggest
that the Sun evolved from a 2008/2009-like configuration at the start
of the Maunder Minimum toward an ephemeral-only configuration by the
end of it, supporting a prediction that we may be on the cusp of a
new grand solar minimum.

---------------------------------------------------------
Title: Alfvénic waves in polar spicules
Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A.; Ahangarzadeh
Maralani, A. R.; Zeighami, S.
2015A&A...573A...4T Altcode: 2014arXiv1409.7654T
Context. For investigating spicules from the photosphere to coronal
heights, the new Hinode/SOT long series of high-resolution observations
from space taken in CaII H line emission offers an improved way
to look at their remarkable dynamical behavior using images free of
seeing effects. They should be put in the context of the huge amount of
already accumulated material from ground-based instruments, including
high- resolution spectra of off-limb spicules. Aims: Both the
origin of the phenomenon and the significance of dynamical spicules
for the heating above the top of the photosphere and the fuelling of
the chromospheric and the transition region need more investigation,
including of the possible role of the associated magnetic waves for
the corona higher up. Methods: We analyze in great detail the
proper transverse motions of mature and tall polar region spicules for
different heights, assuming that there might be Helical-Kink waves or
Alfvénic waves propagating inside their multicomponent substructure,
by interpreting the quasi-coherent behavior of all visible components
presumably confined by a surrounding magnetic envelop. We concentrate
the analysis on the taller CaII spicules more relevant for coronal
heights and easier to measure. Two-dimensional velocity maps of
proper motion were computed for the first time using a correlation
tracking technique based on FFTs and cross-correlation function
with a 2nd-order-accuracy Taylor expansion. Highly processed images
with the popular mad-max algorithm were first prepared to perform
this analysis. The locations of the peak of the cross-correlation
function were obtained with subpixel accuracy. Results:
The surge-like behavior of solar polar region spicules supports
the untwisting multicomponent interpretation of spicules exhibiting
helical dynamics. Several tall spicules are found with (i) upward
and downward flows that are similar at lower and middle levels,
the rate of upward motion being slightly higher at high levels; (ii)
the left- and righthand velocities are also increasing with height;
(iii) a large number of multicomponent spicules show shearing motion
of both left- and righthanded senses occurring simultaneously, which
might be understood as twisting (or untwisting) threads. The number
of turns depends on the overall diameter of the structure made of
components and changes from at least one turn for the smallest structure
to at most two or three turns for surge-like broad structures. The
curvature along the spicule corresponds to a low turn number similar
to a transverse kink mode oscillation along the threads. A
movie associated to Fig. 1 is available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201423385/olm">http://www.aanda.org</A>

---------------------------------------------------------
Title: The photosphere-corona Interface: enrichement of the corona
in low FIP elements and helium shells
Authors: Bazin, C.; Koutchmy, S.; Lamy, P.; Veselovski, I.
2014sf2a.conf..209B Altcode:
Slitless consecutive spectra were obtained during the contacts of
the last total solar eclipses (2008, 2009, 2010, 2012, et 2013). They
allowed to show that the overabundance of low First Ionisation Potential
(FIP) elements (Fe II, Ti II, Ba II) in the corona comes from the low
layers of the solar atmosphere, just near and above the temperature
minimum region of the high photosphere. All spectra are recorded
with a fast CCD/CMOS camera, with an equivalent radial resolution of
60 milliarcseconds, or 45 km in the solar atmosphere, above a solar
edge not affected by the parasitic light like it is outside of total
eclipse conditions. Many emission lines of low FIP elements appear in
regions situated between 200 to 600 km above the solar limb defined by
the true continuum measured between the lines. This continuum appears
at these altitudes where the beta of the plasma is near 1. The He I
4713 Å and He II 4686 Å (Paschen alpha line) shells appear at the
height of 800 km above the solar edge and higher. The light curve I =
f(h) of each ion is located at a particuliar altitude in the solar
atmosphere. The scale height corresponds to a density variation, which
allows to evaluate the temperature thanks to the hydrostatic equilibrium
assumption. Moreover, with ionised Titanium lines taken as markers,
we show a similarity between the photosphere-corona interface and
the prominence-corona interface. We discuss the role of the magnetic
field and the ambipolar diffusion for supplying the corona in mass,
without taking into account the role of spicules. The photo-ionisation
of the helium lines by the EUV coronal lines is illustrated thanks to
an extract of SDO/AIA coronal stacked image simultaneously obtained.

---------------------------------------------------------
Title: The June 6 2012 transit of Venus: Imaging and spectroscopic
analysis of the upper atmosphere emission
Authors: Bazin, C.; Zhi, X.; Valls-Gabaud, D.; Koutchmy, S.; Rocher,
P.; Zin, Z. Y.; Fu, Y.; Yang, L.; Liu, G. Q.; Liu, Z.; Ji, K.;
Goodarzi, H.
2014sf2a.conf...57B Altcode:
In the context of transiting exoplanets, the last June 6, 2012 Venus
transit was a unique opportunity to address important questions
regarding its atmosphere. The transit of Venus is indeed a particular
case of an Earth-like planet transit, and the inference one can
make about the upper layers of its atmosphere can be applied to other
exoplanets. To this aim, we designed a small spectrograph that we placed
at the focus of the New Vacuum Solar Telescope of Yunnan Observatory in
China (45 m focus and 1 m of aperture), coupled to a 4K×2K 14 bit CCD
detector, to measure low-resolution optical spectra of the refracted,
scattered and transmitted solar radiation in the upper layers of
the planet. It covered the 385-780 nm range when Venus was over the
disc, and 540-680 nm (including the O_2 terrestrial bands) during
the 18 minutes-long egress. The Hα and He I D3 lines were recorded
repeatedly. The atmospheric Lomonossov arc of Venus was simultaneously
imaged using Hα and TiO filters, allowing us to check the slit position
on the images of Venus and to locate the spectroscopic features on its
disc. The spectra show the signature of the Northern Pole horn part;
a second part was evidenced on the spectra taken near but outside the
limb. We studied the O_2, H_2O and Hα line profiles searching for
signatures arising from Venus and we compared the observed spectra
with synthetic models. The spectroscopic dataset can now be used by a
large community for discussing the properties of the upper atmosphere
of Venus and the future detection of Venus-like exoplanets. Finally,
the study is completed using a unique very high resolution deconvolved
image of the arc and Venus silhouetted at the limb of the Sun, from
the SOT of the Hinode space mission.

---------------------------------------------------------
Title: Spectral atlases of the Sun from 3980 to 7100 Å at the center
and at the limb
Authors: Fathivavsari, H.; Ajabshirizadeh, A.; Koutchmy, S.
2014Ap&SS.353..347F Altcode: 2014arXiv1407.5727F
In this work, we present digital and graphical atlases of spectra
of both the solar disk-center and of the limb near the Solar poles
using data taken at the UTS-IAP &amp; RIAAM (the University of Tabriz
Siderostat, telescope and spectrograph jointly developed with the
Institut d'Astrophysique de Paris and Research Institute for Astronomy
and Astrophysics of Maragha). High resolution and high signal-to-noise
ratio (SNR) CCD-slit spectra of the sun for 2 different parts of the
disk, namely for μ=1.0 (solar center) &amp; for μ=0.3 (solar limb)
are provided and discussed. While there are several spectral atlases of
the solar disk-center, this is the first spectral atlas ever produced
for the solar limb at this spectral range. The resolution of the spectra
is about R∼70 000 (Δ λ∼0.09 Å) with the signal-to-noise ratio
(SNR) of 400-600. The full atlas covers the 3980 to 7100 Å spectral
regions and contains 44 pages with three partial spectra of the
solar spectrum put on each page to make it compact. The difference
spectrum of the normalized solar disk-center and the solar limb is
also included in the graphic presentation of the atlas to show the
difference of line profiles, including far wings. The identification
of the most significant solar lines is included in the graphic
presentation of the atlas. Telluric lines are producing a definite
signature on the difference spectra which is easy to notice. At the
end of this paper we present only two sample pages of the whole atlas
while the graphic presentation of the whole atlas along with its ASCII
file can be accessed via the ftp server of the CDS in Strasbourg via
anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via this link:
http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/other/ApSS.

---------------------------------------------------------
Title: Oscillations in solar jets observed with the SOT of Hinode:
viscous effects during reconnection
Authors: Tavabi, E.; Koutchmy, S.
2014Ap&SS.352....7T Altcode: 2014arXiv1403.0814T
Transverse oscillatory motions and recurrence behavior in the
chromospheric jets observed by Hinode/SOT are studied. A comparison
is considered with the behavior that was noticed in coronal X-ray jets
observed by Hinode/XRT. A jet like bundle observed at the limb in Ca II
H line appears to show a magnetic topology that is similar to X-ray jets
(i.e., the Eiffel tower shape). The appearance of such magnetic topology
is usually assumed to be caused by magnetic reconnection near a null
point. Transverse motions of the jet axis are recorded but no clear
evidence of twist is appearing from the highly processed movie. The
aim is to investigate the dynamical behavior of an incompressible
magnetic X-point occurring during the magnetic reconnection in the jet
formation region. The viscous effect is specially considered in the
closed line-tied magnetic X-shape nulls. We perform the MHD numerical
simulation in 2-D by solving the visco-resistive MHD equations with the
tracing of velocity and magnetic field. A qualitative agreement with
Hinode observations is found for the oscillatory and non-oscillatory
behaviors of the observed solar jets in both the chromosphere and the
corona. Our results suggest that the viscous effect contributes to the
excitation of the magnetic reconnection by generating oscillations that
we observed at least inside this Ca II H line cool solar jet bundle.

---------------------------------------------------------
Title: VizieR Online Data Catalog: 398-710nm Sun spectral atlases
(Fathivavsari+, 2014)
Authors: Fathivavsari, H.; Ajabshirizadeh, A.; Koutchmy, S.
2014yCatp017035301F Altcode:
The "spectrum.pdf" file contains 44 pages of graphic presentation of
the solar disk-center vs. solar limb spectra with the identification of
most of the lines included. Each page contains 3 partial spectra. The
identification of lines is made using the reference atlas of Moore
et al. (1966). Each page contains three spectral windows, with each
window made up of two panels. The upper panel shows the spectrum of
the solar disk-center (black curve) on which the spectrum of the solar
limb is overplotted as red curve while the lower panel illustrates the
difference spectrum of the two. The difference spectrum of the lower
panel clearly indicates that the depth of the absorption lines taken at
the solar disk-center is usually deeper than those taken at the solar
limb (in this panel the two pink dashed lines indicate the residual
intensity of 0.05 above and below zero). Note that, in the solar limb
spectrum, the level of the continuum was put to the reference level
given in the "Astrophysical Quantities, 3rd Edition by C. W. Allen,
p. 169". (2 data files).

---------------------------------------------------------
Title: Observation of the prominence cavity region using slitless
eclipse flash spectra and space borne EUV filtergrams
Authors: Bazin, Cyrille; Koutchmy, Serge; Lamy, Philippe; Tavabi, Ehsan
2014IAUS..300..151B Altcode:
We used total solar eclipse free of parasitic light for studying the
prominence to corona interface, and the corresponding cavity in the
context of the coronal physics. We analysed the visible continuum
between the prominences to directly look at the electron density. We
demonstrate some enhanced heating in the cavity region. Some
similarities with the interface regions are shown: the photosphere
to the chromosphere and the prominence to the corona interface. The
optically thin neutral Helium at 4713 Å and the singly ionized Helium
4686 Å Paschen α lines are considered. We summed 80 slitless visible
eclipse flash spectra that we compare with simultaneously obtained
EUV SWAP/Proba2 174 Å images of ESA and AIA/SDO 171Å 193 Å 304 Å
and 131 Å filtergrams. Intensity profiles in a radial direction are
studied. We deduce the variation of the intensity ratio I(He I 4713)
/ I(He II 4686). Discussion: the temperature rises at the edge of the
prominences. We evaluate for the first time with spectrophotometric
accuracy the continuum modulations in prominence spectra. W-L intensity
deficits are observed near the prominence boundaries in both eclipse
spectra and in EUV images, confirming that the prominence -cavity
regions correspond to a relative depression of plasma density of the
surrounding corona. Conclusion: we demonstrate some enhanced heating
occurring in these regions assuming hydrostatic equilibrium.

---------------------------------------------------------
Title: 3D dynamical structuring of a high latitude erupting
prominence: I- Analysis of the cool plasma flows before the eruption
Authors: Koutchmy, Serge; Filippov, Boris; Tavabi, Ehsan; Bazin,
Cyril; Weiller, Sylvain
2014IAUS..300..430K Altcode:
Both the origin of the quiescent prominences and their eruption
related to CMEs are still a matter of extended studies. The small
scale dynamic aspects like vortex structures and counter- flows are
now seriously taken into account having in mind that the flows are a
good proxy of the line of force of the omnipresent but rather unknown
in detail force free or not magnetic field. Large scale vortex has
been detected in a high latitude prominence observed on November 13-
14, 2011 before its eruption.

---------------------------------------------------------
Title: 3D dynamical structuring of a high latitude erupting
prominence: II- Analysis of the coronal context and eruption
Authors: Koutchmy, Serge; Filippov, Boris; Tavabi, Ehsan; Bazin,
Cyrille; Weiller, Sylvain
2014IAUS..300..433K Altcode:
Both the origin of the quiescent prominences and their eruption related
to CMEs event are still a matter of extended studies. The case of high
latitudes quiescent prominences producing slow CMEs can be considered
as a potential component of the slow wind. A high latitude prominence
was observed on November 13 - 14, 2011. A schematic representation
of flux rope is proposed to describe the magnetic structure of the
prominence prior to its eruption.

---------------------------------------------------------
Title: Solar eruptive phenomena
Authors: Filippov, B.; Koutchmy, S.; Martsenyuk, O.; Platov, Y.
2013AIPC.1551..117F Altcode:
At the beginning of the 1990s, it was found out that the strongest
disturbances of space weather were associated with huge ejections
of matter from the solar corona, which took the form of the magnetic
clouds when moved from the Sun. It is the collisions of the magnetic
clouds with the Earth's magnetosphere that lead to strong, sometimes
to catastrophic, changes in space weather. The onset of a coronal
mass ejection (CME) is sudden and no reliable forerunners of CMEs have
been found till now. The problem of CME prediction is less developed
than the problem of solar flare prediction. The most probable initial
magnetic configuration of a CME is a flux rope consisting of twisted
field lines which fill the whole volume of a dark coronal cavity. Cold
dense prominence material can be collected in the lower parts of the
helical flux tubes. Filaments are then the best tracers of the flux
ropes in the corona, visible long before the beginning of the eruption.

---------------------------------------------------------
Title: Formation of a White-Light Jet Within a Quadrupolar Magnetic
Configuration
Authors: Filippov, Boris; Koutchmy, Serge; Tavabi, Ehsan
2013SoPh..286..143F Altcode: 2011arXiv1111.2150K; 2012SoPh..tmp....1F
We analyze multi-wavelength and multi-viewpoint observations of
a large-scale event viewed on 7 April 2011, originating from an
active-region complex. The activity leads to a white-light jet
being formed in the outer corona. The topology and evolution of the
coronal structures were imaged in high resolution using the Atmospheric
Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). In
addition, large field-of-view images of the corona were obtained using
the Sun Watcher using Active Pixel System detector and Image Processing
(SWAP) telescope onboard the PRoject for Onboard Autonomy (PROBA2)
microsatellite, providing evidence for the connectivity of the coronal
structures with outer coronal features that were imaged with the Large
Angle Spectrometric Coronagraph (LASCO) C2 on the Solar and Heliospheric
Observatory (SOHO). The data sets reveal an Eiffel-tower type jet
configuration extending into a narrow jet in the outer corona. The
event starts from the growth of a dark area in the central part of
the structure. The darkening was also observed in projection on the
disk by the Solar TErrestrial RElations Observatory-Ahead (STEREO-A)
spacecraft from a different point of view. We assume that the dark
volume in the corona descends from a coronal cavity of a flux rope that
moved up higher in the corona but still failed to erupt. The quadrupolar
magnetic configuration corresponds to a saddle-like shape of the dark
volume and provides a possibility for the plasma to escape along the
open field lines into the outer corona, forming the white-light jet.

---------------------------------------------------------
Title: Prominence Cavity Regions Observed Using SWAP 174 Å
Filtergrams and Simultaneous Eclipse Flash Spectra
Authors: Bazin, C.; Koutchmy, S.; Tavabi, E.
2013SoPh..286..255B Altcode: 2012arXiv1205.1325B; 2012SoPh..tmp..309B
SWAP images from PROBA2 taken at 174 Å in the Fe IX/X lines are
compared with simultaneous slitless flash spectra obtained during
the solar total eclipse of 11 July 2010. Myriad faint low-excitation
emission lines together with the He I and He II Paschen α chromospheric
lines are recorded on eclipse spectra where regions of limb prominences
are obtained with space-borne imagers. We analyzed a deep flash
spectrum obtained by summing 80 individual spectra to evaluate
the intensity modulations of the continuum. Intensity deficits are
observed and measured at the prominences boundaries in both eclipse
and SWAP images. The prominence cavities interpreted as a relative
depression of plasma density, produced inside the corona surrounding
the prominences, and some intense heating occurring in these regions,
are discussed. Photometric measurements are shown at different scales
and different, spectrally narrow, intervals for both the prominences
and the coronal background.

---------------------------------------------------------
Title: Helium shells and faint emission lines from slitless flash
spectra
Authors: Bazin, Cyril; Koutchmy, Serge
2013JAdR....4..307B Altcode:
At the time of the two last solar total eclipses of August 1st, 2008
in Siberia and July 11th, 2010 in French Polynesia, high frame rate
CCD flash spectra were obtained. These eclipses occurred in quiet Sun
period and after. The slitless flash spectra show two helium shells,
in the weak Paschen Î± 4686 Å line of the ionized helium HeII and
in the neutral helium HeI line at 4713 Å. The extensions of these
helium shells are typically 3 Mm. In prominences, the extension of
the interface with the corona is much more extended. The observations
and analysis of these lines can properly be done only in eclipse
conditions, when the intensity threshold reaches the coronal level,
and the parasitic scattered light is virtually zero. Under the layers
of 1 Mm above the limb, many faint low FIP lines were also seen
in emission. These emission lines are superposed on the continuum
containing absorption lines. The solar limb can be defined using the
weak continuum appearing between the emission lines at the time of
the second and third contact. The variations of the singly ionized
iron line, the HeI and HeII lines and the continuum intensity are
analyzed. The intensity ratio of ionized to neutral helium is studied
for evaluating the ionization rate in low layers up to 2 Mm and also
around a prominence.

---------------------------------------------------------
Title: Increasing the Fine Structure Visibility of the Hinode SOT
Ca II H Filtergrams
Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A.
2013SoPh..283..187T Altcode: 2012SoPh..tmp..107T; 2011arXiv1104.5580T
We present an image processing technique, the improved OMC filter
(also called Madmax), which selects maxima of convexities of intensity
modulations of an image. The filter computes second derivatives of
the image in multiple directions around each pixel. It is shown
to be efficient for pattern recognition, and bright hair-like or
small anisotropic features can be enhanced. The filter is tested on
artificially generated images, and the effect of a different number
of directions in which the second derivatives are calculated is
evaluated. Ca II H line images of spicules and prominences obtained
with Hinode/SOT are also used to illustrate its efficiency on real
data. It is shown how to make the choice of the sensitive parameters
to be used in improving the image visibility.

---------------------------------------------------------
Title: About the solar edge and solar diameter variation studies
Authors: Bazin, C.; Koutchmy, S.; Rocher, P.
2012sf2a.conf..495B Altcode:
Without spurious effects due to instrumental and/or Earth atmospheric
parasitic light, the true solar edge can only be correctly analyzed at
the time of solar total eclipses. We discuss the problems occurring
when using solar diameter measurements made outside of solar total
eclipses, including the possible limb effects related to different
sources of solar activity. Effects due to the PSF and to the scattered
light should be discussed with reference to coronagraphic methods used
to reduce the ultimate sources of parasitic light.

---------------------------------------------------------
Title: Photometric properties of new solar H alpha commercial
Fabry-Perot etalons. Application to the analysis of the chromospheric
fringe
Authors: Bazin, Cyril; Koutchmy, Serge
2012arXiv1209.1027B Altcode:
We consider the use of the commercially available Fabry-Perot etalons
(FP) for the imaging of the solar chromosphere in the H alpha line
of HI. Three etalons of 40, 60 and 90 mm diameter were accurately
analysed. At normal incidence the maximum transmission wavelength
as well as the finesse were evaluated. Polynomial curves precisely
fitting the transmitted central wavelength variations when using a
quasi-parallel beam from a point-like source are presented. Further
calibrations have been done with photometric accuracy using a laboratory
set-up comprising i/ a 16 bits CCD camera; ii/ a Littrow spectrograph
of a spectral power 110000 giving a linear dispersion of 0.0058
nm/pixel and iii/ an artificial Sun used as a light source and iv/
precisely adjustable in position optical components, including the F-P
etalons. In addition, a precise laboratory wavelength calibration was
performed using a low pressure deuterium 2D spectral lamp simultaneously
illuminating the adjustable entrance slit using a splitter before. The
variations of the FWHM of the spectral transmission variations as a
function of the incidence angle of a parallel beam are also given
for each etalon. Consequences resulting from the use of a low but
significant aperture/ratio are tentatively discussed for the first
time. An application to a precise photometric work of solar physics
interest when using limb filtergrams is illustrated and discussed,
with emphasis on the photometric accuracy resulting from the use
of such etalons put before the entrance aperture of an imaging
telescope. Monochromatic images of the solar chromosphere shell in the
vicinity of the polar and equatorial limbs were made using a small
telescope, in order to deduce the variation of the typical average
thicknesses at poles and equator interpreted as a prolateness effect
of the chromospheric shell observed during the last minimum of solar
activity (2009).

---------------------------------------------------------
Title: Prominence-cavity regions observed using SWAP 17.4 nm
filtergrams and simultaneous eclipse flash spectra
Authors: Bazin, C.; Koutchmy, S.; Tavabi, E.
2012arXiv1207.1857B Altcode:
SWAP images from PROBA2 taken at 174 Å in the Fe IX/X lines are
compared with simultaneous slitless flash spectra obtained during the
solar total eclipse of 11 July, 2010. Myriads of faint low excitation
emission lines together with the He I and He II Paschen {\alpha}
chromospheric lines are recorded on eclipse spectra where regions of
limb prominences are obtained with space-borne imagers. We analyzed
a deep flash spectrum obtained by summing 80 individual spectra to
evaluate the intensity modulations of the continuum. Intensity deficits
are observed and measured at the prominences boundaries in both eclipse
and SWAP images. The prominence cavities interpreted as a relative
depression of plasma density, produced inside the corona surrounding
the prominences, and some intense heating occurring in these regions,
are discussed. Photometric measurements are shown at different scales
and different, spectrally narrow, intervals for both the prominences
and the coronal background.

---------------------------------------------------------
Title: Detection of Chromospheric Alfven Waves in Solar Spicule
Authors: Ajabshirizadeh, Ali; Koutchmy, Serge; Tavabi, Ehsan
2012cosp...39...30A Altcode: 2012cosp.meet...30A
No abstract at ADS

---------------------------------------------------------
Title: Plasmoid Ejection at a Solar Total Eclipse
Authors: Koutchmy, S.; Bazin, C.; Berghmans, D.; De Groof, A.;
Druckmüller, M.; Tavabi, E.; Engell, A.; Filippov, B.; Golub, L.;
Lamy, Ph.; Linker, J.; Mikic, Z.; Mouette, J.; Nitschelm, Ch.; Seaton,
D.; Slemzin, V.
2012EAS....55..223K Altcode:
The existence of coronal plasmoids has been postulated for many years
in order to supply material to streamers and possibly to the solar
wind (SW). The W-L SoHO C2 Lasco coronagraph observations were made
under the 2.2 solar radii (R0) occulting disk to look at the ultimate
sources of the SW; EUV imagers are preferably devoted to the analysis
of the corona on and very near the solar disk. Here, in addition to
eclipse white-light (W-L) snapshots, we used the new SWAP space-borne
imager designed for the systematic survey of coronal activity in the
EUV lines near 17.4 nm, over a field of view (FOV) up to 2 R0. Using
summed and co-aligned images, the corona can then be evaluated for the
1st time up to the limit of this FOV. At the time of the July 11, 2010,
solar total eclipse a 20h continuous run of observations was collected,
including images taken during eclipse totality from several ground
observing locations where W-L data were collected. A plasmoid-like
off-limb event was followed using the SWAP summed

---------------------------------------------------------
Title: Homologous flares inducing EUV filament oscillations with
subsequent eruption
Authors: Bocchialini, K.; Koutchmy, S.; Solomon, J.; Tavabi, E.
2012EAS....55..335B Altcode:
We focus our analysis on an event which occurred at the W-limb on
May 30, 2003. The dynamical behavior of the filament, including
damped oscillations, was investigated with the CDS and EIT (SoHO)
experiments, as well as with Hα filtergrams (movies). The eruptive
phase is analyzed taking into account the approximate phasing with
other eruptive phenomena occurring at the same time or before, called
homologous flares and eruptions.

---------------------------------------------------------
Title: About the magnetic origin of Chromospheric Spicules and
Coronal Jets
Authors: Koutchmy, S.; Filippov, B.; Tavabi, E.
2012EAS....55..257K Altcode:
Observations of jet- like phenomena near the solar limb are reported
for a long time, first in Hα (Secchi observations of spicules in the
1870 ies), and after, from eclipse high resolution coronal images taken
in white-light (1920-1973) as spiky structures. EUV jets were reported
in the 70 ies from rocket and space-borne CIV filtergrams and finally
X-EUV jets were reported from SXT observations of Yohkoh and from
EIT and CDS SoHO observations. There is now little doubt that they
are of magnetic origin although no magnetic field measurements exist
for these regions and thermo-dynamical models are still work out. New
observations of both spicules and jets with the SOT/SXT of Hinode were
subjected to an analysis showing the influence of the null point(s) of
the magnetic field. The collective behavior of the H CaII SOT(Hinode)
time sequences of processed with the Madmax operator images of limb
spicules show the torsional effects which were partly suggested before
from the interpretation of high resolution limb spectra taken on Russian
coronagraphs and the VTT at SacPeak. 100 s and shorter period waves
are recorded. We propose a reconnection process occurring at the top of
an emerging twisted flux tube for explaining some peculiarities of the
spicular eruptions and possibly, as a viable mechanism for explaining
the SXR jet eruptions. The result of a numerical 3D modeling illustrates
this erupting mechanism although the behavior of the magneto-plasma
structure near a null point, as shown by coronal filtergrams, does
not necessary imply reconnections, especially the case of jets making
a long coronal ray we observed in white-light with Lasco C2.

---------------------------------------------------------
Title: Prominence-cavity regions observed in 2010 eclipse flash
spectra and SWAP images
Authors: Bazin, C.; Koutchmy, S.; Tavabi, E.
2012EAS....55..185B Altcode:
Images from the SWAP (Proba 2 mission) taken in the Fe IX/X coronal
line emission are compared to simultaneous slitless flash spectra
taken during the total solar eclipse of July, 11th 2010. Many faint
low excitation emission lines together with the HeI and the HeII
Paschen α (Pα) chromospheric lines are recorded in the regions of
limb prominences observed in space. We consider a deep flash spectrum
obtained by summing 80 individual spectra to show the intensity
modulations of the continuum between HeI and HeII lines. Intensity
depressions are observed around the prominences in both eclipse and
SWAP images. The prominence cavities are interpreted as a relative
depression of plasma density produced inside the corona surrounding
the prominences, and some evidence of intense heating occuring in the
region around the prominence is discussed.

---------------------------------------------------------
Title: solar spicules and jets
Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A.
2012EAS....55...71T Altcode:
In order to clear up the origin and possibly explain some solar limb and
disc spicule quasi-periodic recurrences produced by overlapping effects,
we present a simulation model assuming quasi- random positions of
spicules. We also allow a set number of spicules with different physical
properties (such as: height, lifetime and tilt angle as shown by an
individual spicule) occurring randomly. Results of simulations made
with three different spatial resolutions of the corresponding frames
and also for different number density of spicules, are analyzed. The
wavelet time/frequency method is used to obtain the exact period
of spicule visibility. Results are compared with observations of the
chromosphere from i/ the Transition Region and Coronal Explorer (TRACE)
filtergrams taken at 1600 angstrom, ii/ the Solar Optical Telescope
(SOT) of Hinode taken in the Ca II H-line and iii/ the Sac-Peak Dunn's
VTT taken in H? line. Our results suggest the need to be cautious when
interpreting apparent oscillations seen in spicule image sequences
when overlapping is present, i.e.; when the spatial resolution is not
enough to resolve individual components of spicules.

---------------------------------------------------------
Title: New Technology Solar Coronagraphs
Authors: Koutchmy, S.; Bazin, C.; Damé, L.; Rochain, S.; Tavabi, E.
2012EAS....55..375K Altcode:
We present the Mirror Advanced technology Coronagraph (MAC) as a
new generation solar telescope to be put at suitable high altitude
coronal sites in order to resolve modern problems of solar physics,
like the origin of the heating of the chromosphere and of the corona,
the analysis of the mesospheric layers of the solar atmosphere and the
effects of shearing the photospheric magnetic fields on the dynamics
of the upper coronal layers.

---------------------------------------------------------
Title: SOHO observations of oscillatory motions in an eruptive
filament: Intensity and velocity variations
Authors: Bocchialini, K.; Koutchmy, S.; Solomon, J.
2011sf2a.conf..369B Altcode:
The variations in intensity and velocity inside an eruptive filament,
observed on May 30, 2003 with CDS and EIT on-board SOHO, are analysed
in the transition region He I line and the coronal Mg X line. Vertical
oscillating motions of the filament with damped velocity oscillations
before its disappearance are revealed. The link between theses
oscillations, the flaring regions nearby and the filament eruption
is investigated.

---------------------------------------------------------
Title: The helium shells of HeI and HeII at solar minimum: New
results from eclipse flash spectra of 2008- 2010
Authors: Bazin, C.; Koutchmy, S.; Lamy, P.
2011sf2a.conf..203B Altcode:
Flash spectra taken at high frame rate during the total solar
eclipse of August 1st 2008 in Siberia and during the July 11th 2010
in French Polynesia are compared in the context of the quiet Sun near
the minimum of activity. They both reveal the weak Paschen α 468.6
nm ionized helium line, seen as a helium shell in layers up to the
8 Mm heights. The preliminary evaluated effective height of the He
I 4713 shell is 1.8 Mm and it is approximately 2.0 Mm for the He II
4686 emissions outside polar regions. These lines can be measured
only in eclipse conditions, when the parasitic scattered light is
negligible for very low solar fluxes corresponding to the coronal
levels. Many faint lines are also seen in emission such as Ba +, Ti +,
Fe +, but with a much lower radial extension. They were observed to be
superposed to F-lines when defining the solar limb using the continuum
background. A cartoon is proposed to describe the structuration of
these low layers and to illustrate the contribution of the magnetic
field. These observations are important new insights for understanding
(i) the magnetic field inference in the very low layers of the solar
transition region and (ii) the ionisation mechanisms producing the
big jump of the temperature towards the corona, including the source
of heating.

---------------------------------------------------------
Title: The Three-Dimensional Behavior of a Twisted Flux Tube Expanding
in the Corona: Reconnection, Writhe, and Jets
Authors: Tavabi, Ehsan; Koutchmy, Serge; Ajabshirizadeh, Ali
2011ITPS...39.2436T Altcode: 2011arXiv1103.3814T
We discuss some aspects of magnetic reconnection which could help in
understanding many aspects of magnetic plasma interactions. We will show
that the helical structure often observed in polar jets is a natural
consequence of magnetic helicity conservation in 3D reconnection driven
by a collision of two parts of an emerging flux tube within the single
emerged loop. We perform 3D simulations by solving the time-dependent,
ideal MHD equations with a uniform initial twist. We deduce that the
emergence of highly twisted magnetic flux introduces several null
points, which in turn causes reconnection between opposite directions
of magnetic field within a single loop at nearest part and the release
of the trapped twist in the form of a helical jet-like emission.

---------------------------------------------------------
Title: Oscillatory motions observed in eruptive filaments
Authors: Bocchialini, K.; Baudin, F.; Koutchmy, S.; Pouget, G.;
Solomon, J.
2011A&A...533A..96B Altcode: 2011arXiv1107.0596B
Context. The origin of the variable component of the solar wind is of
great intrinsic interest for heliophysics and spaceweather, e.g. the
initiation of coronal mass ejections and the problem of mass loss
of all stars. It is also related to the physics of coronal neutral
sheets and streamers, which occur above lines of magnetic polarity
reversal. Filaments and prominences correspond to the cool coronal
component of these regions. Aims: We examine the dynamical
behaviour of these structures where reconnection and dissipation
of magnetic energy in the turbulent plasma are occurring. The link
between the observed oscillatory motions and the eruption occurrence
is investigated in detail for two different events. Methods:
Two filaments were analysed using two different datasets: time series of
spectra using a transition region line (He I at 584.33 Å) and a coronal
line (Mg X at 609.79 Å) measured with CDS on-board SOHO, observed on
May 30, 2003, and time series of intensity and velocity images from
the NSO/Dunn Solar Telescope in the Hα line on September 18, 1994
for the other. The oscillatory content was investigated using Fourier
transform and wavelet analysis and compared to different models. Results: In both filaments, oscillations are clearly observed,
in intensity and velocity in the He I and Mg X lines, in velocity in
Hα, with similar periods from a few minutes up to 80 min, with a main
range from 20 to 30 min, simultaneously with eruptions. Both filaments
exhibit vertical oscillating motions. For the filament observed in
the UV (He I and Mg X lines), we provide evidence of damped velocity
oscillations, and for the filament observed in the visible (Hα line),
we provide evidence that parts of the filament are oscillating, while
the filament is moving over the solar surface, before its disappearance.

---------------------------------------------------------
Title: A statistical analysis of the SOT-Hinode observations of
solar spicules and their wave-like behavior
Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A.
2011NewA...16..296T Altcode: 2010arXiv1004.1692T
Spicules are an important very dynamical and rather cool structure
extending between the solar surface and the corona. They are partly
filling the space inside the chromosphere and they are surrounded by
a transition thin layer. New space observations taken with the SOT of
the Hinode mission shed some light on their still mysterious formation
and dynamics. Here we restrict the analysis to the most radial and
the most interesting polar spicules situated at the base of the fast
solar wind of coronal holes. We consider a first important parameter
of spicules as observed above the solar visible limb: their apparent
diameter as a function of the height above the limb which determines
their aspect ratio and leads to the discussion of their magnetic origin
using the flux tube approximation. We found that indeed spicules
show a whole range of diameters, including unresolved "interacting
spicules" (I-S), depending of the definition chosen to characterize
this ubiquitous dynamical phenomenon occurring into a low coronal
surrounding. Superposition effects along the line of sight have to be
taken into account in order to correctly measure individual spicules
and look at I-S. We take advantage of the so-called mad-max operator
to reduce these effects and improve the visibility of these hair-like
features. An excellent time sequence of images obtained above a polar
region with the Hinode SOT through the HCaII filter with a cadence
of 8 s was selected for analysis. 1-D Fourier amplitude spectra
(AS) made at different heights above the limb are shown for the
first time. A definite signature in the 0.18-0.25 Mm range exists,
corresponding to the occurrence of the newly discovered type II
spicules and, even more impressively, large Fourier amplitudes are
observed in the 0.3-1.2 Mm range of diameters and spacing, in rough
agreement with what historical works were reporting. Additionally,
some statistically significant behavior, based on AS computed for
different heights above the limb, is discussed. "Time slice or x-
t diagrams" revealing the dynamical behavior of spicules are also
analyzed. They show that most of spicules have multiple structures
(similarly to the doublet spicules) and they show impressive transverse
periodic fluctuations which were interpreted as upward kink or Alfven
waves. Evidence of the helical motion in spicules is now well evidenced,
the typical periods of the apparent oscillation being around 120 s. A
fine analysis of the time-slice diagram as a function of the effective
heights shows an interesting new feature near the 2 Mm height. We
speculate on the interpretation of this feature as being a result of
the dynamical specificities of the spicule helical motion as seen in
these unprecedented high resolution HCaII line emission time series.

---------------------------------------------------------
Title: Null-Point Oscillations of Chromospheric Large Cool Jets
Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A.
2011AIPC.1356...99T Altcode:
In addition of the whip-like behavior, null-point motions in the
reconnection site can excite transversal oscillation along the magnetic
dense jets, which was called the kink mode wave, and also this mode can
evolve into Alfven wave after its propagation into the more homogeneous
medium. The study of X-ray jets is an important topic to understand
the heating of the solar corona and the origin of the fast wind. The
recently launched Hinode mission permitted to observe the cool proxies
of these jets with an unprecedented high spatial resolution of 120
km on the Sun. We selected a high cadence sequence of SOT (Hinode)
observations taken with both the HCaII and the Hα filter to look at the
details of the dynamics revealed by a large jet event. Both wavelet and
amplitude spectra analysis were used to analyze the observed kink wave
and the time variations of intensities during the event. The results
are discussed in the frame of different models implying reconnections
with the inference of the dynamical phenomena occurring in the vicinity
of several null points including the oscillatory behavior.

---------------------------------------------------------
Title: Contribution to the modeling of solar spicules
Authors: Tavabi, E.; Koutchmy, S.; Ajabshirizadeh, A.
2011AdSpR..47.2019T Altcode: 2011arXiv1101.2520T
Solar limb and disk spicule quasi-periodic motions have been reported
for a long time, strongly suggesting that they are oscillating. In order
to clear up the origin and possibly explain some solar limb and disk
spicule quasi-periodic recurrences produced by overlapping effects,
we present a simulation model assuming quasi-random positions of
spicules. We also allow a set number of spicules with different physical
properties (such as: height, lifetime and tilt angle as shown by an
individual spicule) occurring randomly. Results of simulations made
with three different spatial resolutions of the corresponding frames
and also for different number density of spicules, are analyzed. The
wavelet time/frequency method is used to obtain the exact period
of spicule visibility. Results are compared with observations of the
chromosphere from (i) the Transition Region and Coronal Explorer (TRACE)
filtergrams taken at 1600 Å, (ii) the Solar Optical Telescope (SOT)
of Hinode taken in the Ca II H-line and (iii) the Sac-Peak Dunn's VTT
taken in Hα line. Our results suggest the need to be cautious when
interpreting apparent oscillations seen in spicule image sequences
when overlapping is present, i.e., when the spatial resolution is not
enough to resolve individual components of spicules.

---------------------------------------------------------
Title: The He I and He II chromospheric shells and the Transition
Region
Authors: Bazin, Cyril; Koutchmy, Serge; Tavabi, Ehsan
2010arXiv1008.0404B Altcode:
Total eclipse observations were performed in 2008 and 2009 to study
the He I and He II shells near the 1 Mm heights above the solar
limb. They suggest that the corona penetrates deep into the chromosphere
following magnetic chanels. Thanks to the use of a fast CCD camera,
the observation of a second ionized helium shell is evidenced for the
first time. The transition region is then seen at very low altitude
where spicules are emerging. Spicule feet are also discussed, using
the best resolution SOT/Hinode HCaII images processed with the non
linear operator Madmax to look at details of this ubiquitous part of
the solar atmosphere.

---------------------------------------------------------
Title: Coronal Fine Linear Rays: Are They Fast Streams From Active
Regions?
Authors: Koutchmy, Serge; Lamy, Philippe; Viladrich, Christian;
Filippov, Boris; Nikoghossian, Arthur; Golub, Leon
2010AIPC.1216..339K Altcode:
Eclipse observations of the W-L corona show linear rays above active
regions at times of solar maximum. We show that these linear rays are
also observed in the field-of-view of the C2-LASCO coronagraph, in
perfect correspondence with the eclipse results. A selected prominent
case taken from the 2001 eclipse observation in Angola is analysed
with several different methods, including the use of a synoptic map
constructed using SoHO/LASCO C2 images. A clear signature of time
variations near the eclipse observation is detected, suggesting that
at least some parts of the beam are collimated. These observations
strongly suggest high speed streams that apparently ignore the potential
large scale coronal magnetic field rooted rather low in the corona. A
possible origin is the neutral magnetic points located above the
active region. Several mechanisms exist to explain how the plasma is
accelerated in these regions to large quasi-relativistic velocities,
possibly related to the occurrence of type III radio bursts. We point
out a curious analogy with phenomena occurring inside coronal holes.

---------------------------------------------------------
Title: Is there a flare-like precursor of EUV waves and CMEs ?
Authors: Filippov, Boris; Podladhikova, Olena; Golub, Leon; Koutchmy,
Serge
2010cosp...38.2889F Altcode: 2010cosp.meet.2889F
Filament eruptions with a flux rope are usually considered the cause
of CMEs. It is however not clear why after reaching some critical
height, the filament suddenly erupts and whether or not we always have
a one to one correspondence. Additional factors can be considered,
starting with the ubiquitous chromospheric (in H) and/or coronal
running disturbances or waves seen with EUV and SXR filtergrams
collected by different missions, including the newly operated SWAP
of Proba-2, the GOES 14 SXR patrol instrument and the high resolution
XRT of Hinode. The eruptions seem to be induced by a well focused but
large explosive event originating from an unresolved region presumably
situated rather low in the atmosphere, near the chromosphere-corona
interface. A similar picture can be drawn from a new type of coronal
flare observed with the XRT of Hinode outside of any active region
and without any precursor. Both the quasi-thermal coronal flare and
the large dynamical phenomenon originate or start from a very small
unresolved region. We discuss the difference in mass, momentum and
amount of energy involved for 2 selected events (25 Dec 2006 with
XRT and 5 Feb 2010 with SWAP and other instruments) that are well
documented. We want to examine at what height in the atmosphere these
events are triggered and what is the relevance to the CME phenomenon,
without speculating on the unresolved magnetic field context. The
events were observed at solar activity minimum without any complication
resulting from numerous active regions being present on the disk.

---------------------------------------------------------
Title: 5 min loop oscillations and propagating waves in the upper
solar atmosphere
Authors: Veselovsky, Igor; Koutchmy, Serge
2010cosp...38.2942V Altcode: 2010cosp.meet.2942V
Solar resonant P-mode oscillations in the 5min range are excited by the
convective motions under its visible surface. Those oscillations are
mostly known to be trapped acoustic Eigen-modes and waves propagating
near the temperature minimum. They are readily observed in velocity
and temperature (intensity) variations at the photospheric level,
but not too often in the chromosphere and the corona, where they are
documented only under some specific favor-able conditions when waves
are guided and transformed by the concentrated magnetic field. Their
quantitative role in the physics of the solar atmosphere, its heating
and plasma acceler-ation is still unclear. It is due to their mode
transformation, reflection and dissipation during the propagation
from the source regions which are also not well determined. Estimates
of the propagating and standing parts are still not certain. Those
estimates are needed for the en-ergy budget evaluations in the solar
atmosphere. Observations of 5-min oscillations in the solar corona are
scarce and puzzling because of the poor knowledge of many relevant
physical param-eters. We discuss the suggested interpretations of
available "Hinode" data as well as of recent observations onboard the
"Coronas -Photon" satellite in 2009 and indicate their insufficiency for
obtaining correct one-valued solutions. We point out the impossibility
to identify and split the modes in the inhomogeneous and time variable
solar atmosphere because of non-linearity in many instances. Finally,
we analyze the question of the role of other waves and non-wave
structures linking the levels in the solar atmosphere and conclude
that this role is generally increasing with the height. This also
means that quasi-steady models of the solar wind outflow formation
are of very limited usefulness.

---------------------------------------------------------
Title: Jet phenomena above null points of the coronal magnetic field
Authors: Filippov, B.; Koutchmy, S.; Golub, L.
2009Ge&Ae..49.1109F Altcode:
Short-lived plasma jets of various scales, from giant X-ray jets more
than 300 Mm in extent to numerous small jets with sizes typical of
macrospicules, are the phenomena observed in the solar corona in extreme
ultraviolet and X-ray emission. Small jets are particularly prominent
in polar coronal holes. They are close neighbors of tiny bright loops
and coincide in time with their sudden brightening and increase in
size. The geometric shape of the jets and their location suggest
that they arise near singular null points of the coronal magnetic
field. These points appear in coronal holes due to the emergence
of small bipolar or unipolar magnetic structures within large-scale
unipolar cells. Polar jets show a distinct vertical plasma motion in
a coronal hole that introduces significant momentum and mass into the
solar wind flow. Investigating the dynamics of polar jets can elucidate
certain details in the problem of fast solar wind acceleration.

---------------------------------------------------------
Title: Propriétés photométriques d'étalons fabry-pérot pour la
raie halpha. application à l'analyse de la frange chromosphérique
du soleil.

---------------------------------------------------------
Title: Propriétés photométriques d'étalons
fabry-pérot pour la raie halpha. application à l'analyse de la
frange chromosphérique du soleil.

---------------------------------------------------------
Title: Photometric properties
of solar halpha fabry-perot etalons. application to the analysis of
the chromospheric fringe.
Authors: Bazin, C.; Koutchmy, S.
2009O&T....74....2B Altcode:
We consider the use of the commercially available Fabry-Perot etalons
(FP) for the imaging of the solar chromosphere in the Ha line of
hydrogen. Three etalons of 40, 60 and 90 mm of diameter were evaluated
and accurately analysed. At normal incidence the maximum transmission
wavelength is 656.285 nm for the 60 and 40 mm etalons FP. The finesse
has been found to be 13.3 for the FP 60mm, 8.7 for the FP 40 and 13.9
for the FP 90 mm. Shifts of the central wavelength as a function
of the incidence angle were accurately measured. Polynomial curves
giving the variation of the transmitted central wavelength when using a
quasi-parallel beam from a point-like source are presented. Calibrations
were done with a photometric accuracy using i/ a 16 bits CCD camera; ii/
a Littrow spectrograph of a spectral power 110000, a linear dispersion
giving a .0058 nm/ pixel resolution and iii/ an artificial Sun with
different angular extension used as a light source and iv/ adjustable
in position optical components. The precise laboratory wavelength
calibration was performed using a low pressure deuterium spectral lamp
simultaneously illuminating the entrance slit. The variations of the
FWHM of the transmission curves as a function of the incidence angle
are also given for a typical etalon. Consequences resulting from the
use of a significant aperture/ratio are tentatively discussed for
the first time. An application to a precise solar photometric work
using filtergrams is illustrated, with emphasis on the photometric
accuracy resulting from the use of such etalons put before the entrance
aperture of the imaging telescope. Monochromatic images of the solar
chromospheric shell near the limbs were made, in order to deduce the
variation of its thickness at poles and equator in order to measure the
prolateness effect during this current minimum of solar activity (2009).

---------------------------------------------------------
Title: Isolated quasi-axisymmetric sunspots
Authors: Koutchmy, Serge; Le Piouffle, Vincent
2009IAUS..259..227K Altcode:
We briefly review the question of the origin, during a sunspot cycle,
of well isolated sunspots. This includes big sunspots like the one
observed in Nov. 2006. An overall axi-symmetric morphology is not
perfectly observed when the morphological details of both the umbra
and of the penumbra are considered. This is especially the case of
umbral dots always present inside the core of a sunspot and also of
penumbral filaments with non radial parts. However, the distribution
of the surrounding fields, including deep layers, the occurrence
of persistent coherent running penumbral waves, the magnetic moat
behavior, the bright ring phenomena, etc. seem to justify a revival
of the naive former but revised (converging motions are considered)
Larmor model of a sunspot (as suggested by Lorrain et al. 2006). To
discuss the “emergence” of single isolated sunspots from deep layers
we performed a quasi-statistical analysis limited to cycle 23. It
is based on MDI data taken in the continuum, using the accompanying
magnetograms to check our assertion. Surprisingly, single sunspots
are definitely and preferably found to occur at low latitude and
during the descending branch of the cycle. To explain our observations
we speculate about the behavior of the deeply seated magnetic loop,
following the original idea of H. Alfven (with whirl rings which follow
the global dipolar field when approaching the surface). It could
lead to a closed loop approximately orthogonal to the local radius,
similar to “smoke rings” arriving at the surface of the Sun and
sometimes also called a plasmoid. The ring will only very weakly feel
the destabilizing Coriolis force, when emerging at very low latitudes,
which seems consistent with our observations.

---------------------------------------------------------
Title: Scientific requirements for future spatially resolved
white-light and broad-band high-cadence observations of the Sun
Authors: Veselovsky, Igor S.; Koutchmy, Serge
2009AdSpR..43..995V Altcode:
Several important issues are open in the field of solar variability and
they wait their solution which up to now was attempted using critical
ground-based instrumentations. However, accurate photometric data
are attainable only from space. New observational material should be
collected with high enough spatial and spectral resolution, covering
the whole visible range of the electromagnetic spectrum as well
infrared and ultraviolet to reconstruct the total solar irradiance:
(1) the absolute contributions of different small-scale structural
entities of the solar atmosphere from the white light flares and from
micro-flares are still poorly known; (2) we do not know the absolute
contributions of different structural elements of the solar atmosphere
to the long-term and to the cyclic variations of the solar irradiance,
including features of the polar regions of the Sun; (3) the variations
of the chromospheric magnetic network are still poorly evaluated; (4)
only scarce information is available about the spectral variations of
different small-scale features in the high photosphere. Variability of
the Sun in white light can be studied with higher spectral, spatial and
time resolution using space-born telescopes, which are more appropriate
for this purpose than ground based observatories because of better
seeing conditions, no interference of the terrestrial atmosphere and a
more precise calibration procedure. Scientific requirements for such
observations and the possible experimental tools proposed for their
solution. Suggested solar studies have broader astrophysical importance.

---------------------------------------------------------
Title: ASPIICS, a giant externally occulted coronagraph for the
PROBA-3 formation flying mission
Authors: Vivès, S.; Lamy, P.; Koutchmy, S.; Arnaud, J.
2009AdSpR..43.1007V Altcode:
Formation flying opens new perspectives for coronal physics, and
allow to conceive giant, externally occulted coronagraphs using a
two-component space system with the external occulter on one spacecraft
and the optical instrument on the other spacecraft. ASPIICS (Association
de Satellites Pour l'Imagerie et l'Interférométrie de la Couronne
Solaire) is a mission proposed to ESA in the framework of the PROBA-3
program of formation flying which is presently in phase A, to exploit
this technique for coronal observations. ASPIICS is composed of a
single coronagraph which performs high spatial resolution imaging of
the corona as well as 2-dimensional spectroscopy of several emission
lines from the coronal base out to 3 R⊙. The selected
lines allow to address different coronal regions: the forbidden
line of Fe XIV at 530.285 nm (coronal matter), Fe IX/X at 637.4 nm
(coronal holes), HeI at 587.6 nm (cold matter). An additional broad
spectral channel will image the white light corona so as to derive
electron densities. The classical design of an externally occulted
coronagraph is adapted to the detection of the very inner corona
as close as 1.01 R⊙ and the addition of a Fabry-Perot
interferometer using a so-called " étalon". This paper is dedicated
to the description of the optical design and its critical components:
the entrance optics and the Fabry-Pérot interferometer. ASPIICS will
address the question of coronal heating and of the role of waves by
characterizing propagating fluctuations (waves and turbulence) in the
solar wind acceleration region and by looking for oscillations in the
intensity and Doppler shift of spectral lines. The combined imaging
and spectral diagnostics capabilities available with ASPIICS will
allow to map the velocity field of the corona both in the sky plane
(directly on the images) and along the line-of-sight by measuring
the Doppler shifts of emission lines. We will attempt to determine
how the different components of the solar wind, slow and fast are
accelerated. ASPIICS will observe the corona during the maximum of
solar activity, insuring the detection of many Coronal Mass Ejections
(CMEs). By rapidly alternating high resolution imaging and spectroscopy,
CMEs will be thoroughly characterized. In addition, ASPIICS will attempt
to characterize the topology of the magnetic field in the corona.

---------------------------------------------------------
Title: X-Ray Jet Dynamics in a Polar Coronal Hole Region
Authors: Filippov, Boris; Golub, Leon; Koutchmy, Serge
2009SoPh..254..259F Altcode: 2007arXiv0711.4320F
New X-ray observations of the north polar region taken from the X-ray
Telescope (XRT) of the Hinode spacecraft are used to analyze several
time sequences showing small loop brightenings with a long ray above. We
focus on the formation of the jet and discuss scenarios to explain
the main features of the events: the relationship with the expected
surface magnetism, the rapid and sudden radial motion, and possibly the
heating, based on the assumption that the jet occurs above a null point
of the coronal magnetic field. We conclude that 2-D reconnection models
should be complemented in order to explain the observational details
of these events and suggest that alternative scenarios may exist.

---------------------------------------------------------
Title: Magneto-acoustic wave oscillations in solar spicules
Authors: Ajabshirizadeh, A.; Tavabi, E.; Koutchmy, S.
2009Ap&SS.319...31A Altcode: 2008arXiv0806.1418A
Some observations suggest that solar spicules show small amplitude
and high frequency oscillations of magneto-acoustic waves, which
arise from photospheric granular forcing. We apply the method of MHD
seismology to determine the period of kink waves. For this purposes,
the oscillations of a magnetic cylinder embedded in a field-free
environment is investigated. Finally, diagnostic diagrams displaying
the oscillatory period in terms of some equilibrium parameters are
provided to allow a comparison between theoretical results and those
coming from observations.

---------------------------------------------------------
Title: Une grande éclipse totale de soleil le 22 juillet 2009 Title:
Une grande éclipse totale de soleil le 22 juillet 2009 Title:
The great total eclipse of july 22, 2009;
Authors: Koutchmy, S.; Mouette, J.; Bazin, C.
2008O&T....71....2K Altcode:
Planning observations of the Total Eclipse of July 22, 2009. We shortly
review the circumstances of this forthcoming big Solar Total Eclipse,
giving references, ephemeris and maps to show the sites where to go for
observing it in good conditions. The probabilities of a clear sky at
time of totality are discussed using 2 different sources of statistical
analysis and the conditions for making an enjoyable eclipse trip are
commented. We also briefly review what can be done during the totality,
taking into account the scientific priorities existing in coronal
physics and using an example of what has been outstandingly done at
the last 2008 eclipse as well as the general interest of the eclipse
phenomenon. Finally we give in Annexe an overview of the post-eclipse
projected international conference organized by the Chinese Academy of
Sciences, which will take place in Souzhou, including its preliminary
scientific program.

---------------------------------------------------------
Title: Causal relationships between eruptive prominences and coronal
mass ejections
Authors: Filippov, B.; Koutchmy, S.
2008AnGeo..26.3025F Altcode: 2007arXiv0711.4752F
A close association between eruptive prominences and CMEs, both
slow and fast CMEs, was reported in many studies. Sometimes it was
possible to follow the material motion starting from the prominence
(filament) activation to the CME in the high corona. Remnants of the
prominence were found in the bright core of the CME. However, detailed
comparisons of the two phenomena reveal problems in explaining CMEs as
a continuation of filament eruptions in the upper corona. For example,
the heliolatitudes of the disappeared filaments and subsequent coronal
ejections sometimes differ by tens of degrees. In order to clear up
the problems appearing when considering this association EP-CME, we
tentatively analyse the more general question of the dynamics of the
generic magnetic flux rope. Prominences and filaments are the best
tracers of the flux ropes in the corona long before the beginning of
the eruption. A twisted flux rope is held by the tension of field lines
of photospheric sources until parameters of the system reach critical
values and a catastrophe happens. We suggest that the associated flux
rope height above the photosphere is one of these parameters and that
it is revealed by the measured height of the filament. 80 filaments
were analysed and we found that eruptive prominences were near the
so-called limit of stability a few days before their eruptions. We
suggest that a comparison of actual heights of prominences with the
calculated critical heights from magnetograms could be systematically
used to predict filament eruptions and the corresponding CMEs.

---------------------------------------------------------
Title: Small-scale Coronal Jets
Authors: Koutchmy, S.; Filippov, B.; Golub, L.
2008ESPM...12.2.93K Altcode:
Jet-like events are observed on different scales in the solar corona
in EUV and X-rays. They range from gigantic coronal X-ray jets greater
than 300 Mm in length to small but numerous jetlets. Polar coronal holes
show a significant activity manifested in small loop brightenings and
jetlet formation. Geometrical shape of the jetlets and their position
indicate that they appear near the singular points of the magnetic
field, namely, null points or X-points. These nulls arise due to the
interaction between new emerging small dipoles and large-scale magnetic
field of the coronal hole. The jetlets reveal some real observable
vertical mass motion inside the coronal hole. It is difficult to measure
the radial velocity of plasma within the jetlets but it seems large
enough to significantly contribute as a large momentum into the solar
wind. Finally jetlets could serve as injectors to the process of the
solar fast wind acceleration. We believe that similar but even smaller
processes could very often happen at smaller scale in the chromosphere
near emerging magnetic ephemeral regions forming numerous jetlets of
the upper chromosphere. They form the upper chromosphere and follow
the direction of the surrounding magnetic field. At the epoch of low
activity, the difference in the large-scale structure of the polar
magnetic field and that of the low latitude quiet region magnetic
field results in a prolateness of the chromosphere.

---------------------------------------------------------
Title: Resolution Effect in the Solar Spicules Oscillations
Authors: Ajabshirizadeh, A.; Koutchmy, S.; Tavabi, E.
2008ESPM...12.2.44A Altcode:
In order to explain solar limb spicule periodic recurrence, we have
adopted a simulation model based on random position of spicule on the
Sun limb, we allow a set number of spicules with different physical
properties (such as height, lifetime and tilt angle) randomly occur
along the Z-axis and after reaching the maximum length falling back
to the solar surface. This simulation has been applied for three
different resolutions of frames and then analysis spicule visibility
using the wavelet time/frequency method to obtain the exact period
for them. Finally, the simulation results have been compared
with observations. This investigation is prompted by observations of
chromosphere from the Transition Region and Coronal Explorer (TRACE)
at 1600 Ångstrom , Solar Optical Telescope (SOT) on Hinode revealing
at Ca II H-line and Sac-Peak H-alpha line.

---------------------------------------------------------
Title: About Isolated Quasi-axi-symetric Sunspots: Description,
Statistical Analysis and Theoretical Modelling
Authors: Koutchmy, S.; Le Piouffle, V.
2008ESPM...12..3.6K Altcode:
We briefly review the question of the occurrence, during a sunspot
cycle, of well isolated sunspots. This includes big sunpots like
the one observed in Nov. 2006. We note that a quasi- axi-symmetric
morphology is clearly NOT observed when the morphological details of
both the umbra and penumbra are considered. However, the occurrence of
persistent coherent penumbral waves, the magnetic moat behavior, the
bright ring phenomena, etc. seem to justify a revival of the former
and revised Larmor model of a sunspot (the so-called the P. Lorrain
model). To discuss the "emergence" of single sunspots from deep
layers, we performed statistical analysis limited to cycle 23 based on
MDI images taken in the continuum and using magnetograms. Surprisingly,
single sunspots are definitely and preferably found to occur at low
latitude and during the descending branch of the cycle. To explain
our observations, we suggest the occurrence of magnetic loops orthogonal
to the local radius, similar to "smoke rings" arriving at the surface
of the Sun. The rings will only very slightly feel the Coriolis force
at low latitudes, which is consistent with our observations.

---------------------------------------------------------
Title: New perspectives in solar coronagraphy offered by formation
flying: from PROBA-3 to Cosmic Vision
Authors: Lamy, P.; Vivès, S.; Damé, L.; Koutchmy, S.
2008SPIE.7010E..1HL Altcode:
Formation flying opens new perspectives in solar physics, and allow to
conceive giant, externally-occulted coronagraphs using a two-component
space system with the external occulter on one spacecraft and the
optical instrument on the other spacecraft at a distance of hundred
meters. Conditions close to those of a solar total eclipse can then be
achieved offering the capability of imaging the solar corona down to the
limb at very high spatial resolution. ASPIICS (Association de Satellites
Pour l'Imagerie et l'Interférométrie de la Couronne Solaire) is a
mission proposed to ESA in the framework of its PROBA-3 demonstration
program of formation flying which is presently in phase A. ASPIICS is
a single coronagraph which will perform both high spatial resolution
imaging of the solar corona as well as 2-dimensional spectroscopy of
several emission lines from the coronal base out to 3 R\beye using
a Fabry-Pérot étalon interferometer. The classical design of an
externally-occulted coronagraph is adapted to the formation flying
configuration allowing the detection of the very inner corona as
close as 0.01 R\beye from the solar limb. Super-ASPIICS is an even
more ambitious instrument part of the scientific payload of HiRise,
the High Resolution Imaging and Spectroscopy Explorer proposed to
ESA in the framework of its Cosmic Vision program. With an increased
inter-satellite distance of 280 m, an aperture of 300 mm, a spectral
domain extending from the ultraviolet to the near-infrared, and
spectroscopic capabilities, Super-ASPIICS will offer unprecedented
diagnostic capabilities, including the measurement of coronal magnetic
fields.

---------------------------------------------------------
Title: Analysis and interpretation of a fast limb CME with eruptive
prominence, C-flare, and EUV dimming
Authors: Koutchmy, S.; Slemzin, V.; Filippov, B.; Noens, J. -C.;
Romeuf, D.; Golub, L.
2008A&A...483..599K Altcode: 2008arXiv0801.2746K
Aims: Coronal mass ejections or CMEs are large dynamical solar-corona
events. The mass balance and kinematics of a fast limb CME, including
its prominence progenitor and the associated flare, will be compared
with computed magnetic structures to look for their origin and
effect. Methods: Multi-wavelength ground-based and spaceborne
observations are used to study a fast W-limb CME event of December
2, 2003, taking into account both on and off disk observations. Its
erupting prominence is measured at high cadence with the Pic du Midi
full Hα line-flux imaging coronagraph. EUV images from SOHO/EIT and
CORONAS-F/SPIRIT space instruments are processed including difference
imaging. SOHO/LASCO images are used to study the mass excess and
motions. Computed coronal structures from extrapolated surface
magnetic fields are compared to observations. Results: A fast
bright expanding coronal loop is identified in the region recorded
slightly later by GOES as a C7.2 flare, followed by a brightening and
an acceleration phase of the erupting material with both cool and hot
components. The total coronal radiative flux dropped by ~7% in the
19.5 nm channel and by 4% in the 17.5 nm channel, revealing a large
dimming effect at and above the limb over a 2 h interval. The typical
3-part structure observed 1 h later by the Lasco C2 and C3 coronagraphs
shows a core shaped similarly to the eruptive filament/prominence. The
total measured mass of the escaping CME (~1.5×1016 g from
C2 LASCO observations) definitely exceeds the estimated mass of the
escaping cool prominence material although assumptions made to analyze
the Hα erupting prominence, as well as the corresponding EUV darkening
of the filament observed several days before, made this evaluation
uncertain by a factor of 2. This mass budget suggests that the event
is not confined to the eruption region alone. From the current free
extrapolation we discuss the shape of the magnetic neutral surface
and a possible scenario leading to an instability, including the small
scale dynamics inside and around the filament.

---------------------------------------------------------
Title: En attendant l'éclipse totale de soleil du 1er août 2008

---------------------------------------------------------
Title: Planning to observe the total solar eclipse of aug. 1st 2008
Authors: Koutchmy, S.
2008O&T....69...36K Altcode:
We shortly review the circumstances of this forthcoming 2008 Solar
Total Eclipse, giving ephemeris, references and maps to show the sites
where to go for observing it in good conditions. The probabilities
of a clear sky at time of totality are discussed. We also briefly
review what can be done during the totality, taking into account i/ the
scientific priorities existing in coronal physics and Heliophysics; ii/
the general interest of the eclipse phenomenon. References to planned
scientific "2008-eclipse" meetings in China and Russia are given.

---------------------------------------------------------
Title: Magneto-Acoustic Wave (KINK) Oscillations In Solar Spicules
Authors: Ajabshirizadeh, A.; Tavabi, E.; Koutchmy, S.
2008mear.confE..22A Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Wavelet analysis of solar macro-spicule recurrences
Authors: Ajabshirizadeh, A.; Tavabi, E.; Koutchmy, S.
2008NewA...13...93A Altcode:
We looked at the temporal behavior of intensity variations of spicules
and macro-spicules observed at the solar limb by TRACE (transition
region and coronal explorer) EUV telescope in the 1600 Å channel. Using
wavelet analysis technique we got evidence of spicule oscillations. The
time-frequency analysis provided by the wavelet analysis shows a
temporal behavior of spicules with recurrences at periods of about
210-260 s with a typical lifetime of 10 min. Finally, we shortly discuss
two scenarios regarding the possible origin of spicule oscillations.

---------------------------------------------------------
Title: The dynamic solar Corona : violent phenomena of Sun.
Authors: Koutchmy, S.
2008LAstr.122c..16K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Solar Astrophysics, Interferometry, and Coronagraphy at
DomeC/Concordia
Authors: Damé, L.; Amans, J. -P.; Dournaux, J. -L.; Koutchmy, S.;
Lamy, P.; Preumont, A.
2008EAS....33..105D Altcode:
Excellent seeing, coronal conditions, and very low IR thermal
background are qualities of the Dome C/Concordia station site that
will allow unique solar astrophysics science. We review the science
case for inner corona observations (onset of the coronal heating
mechanism still poorly understood) and the promises of high angular
resolution to disentangle the possible mechanisms at work between
waves, convection, and reconnection in this particularly magnetically
structured solar atmosphere between the high chromosphere and inner
corona. For coronagraphy, IR and high resolution possibilities, Dome
C is a case by itself between classical ground-based sites and space
opportunities. Telescopes from 50 cm (coronagraphy oriented) to 4 m
(full high resolution advantage including IR access) are proposed to
benefit from these remarkable observing capabilities. Using 3×O50
cm off-axis telescopes, we first propose a medium size facility
(1.4 m equivalent telescope) for very high resolution access, ADSIIC
(Antarctica Demonstrator of Solar Interferometric Imaging &amp;
Coronagraphy), before the ultimate 9-telescope Solar Facility
equivalent to a 4 m diameter telescope: A-FOURMI (Antarctica 4 m
Interferometer). Finally, 30 m tower designs and their logistics using
standard containers and elementary elements of 6 m maximum length,
are presented and discussed. These towers are indeed of general
interest also for the other optical and IR telescopes intended for
Dome C/Concordia, allowing to get over most of the turbulent ground
layer and to reach the best possible permanent seeing conditions
(better than half an arcsec).

---------------------------------------------------------
Title: Old and New Aspects of Prominence Physics from Coronal
Observations
Authors: Koutchmy, S.; Filippov, B.; Lamy, P.
2007ASPC..368..331K Altcode:
Classical W-L eclipse observations at typical spatial resolution
of 10 arcsec show dark cavities surrounding prominences. Images at
higher spatial resolution processed with a spatial filter reveal
small dynamical cool clouds moving inside the inner corona around
prominences. More recently EIT/SoHO observations taken using the
304 Å channel showed He+ prominences sometimes not seen
in cooler lines. TRACE movies of the Fe IX and XI emissions where
prominences are seen in absorption also bring appreciable informations
on the dynamical surrounding of prominences, without showing obvious
correlations between prominence and coronal structures. Accordingly,
we re-examine the significance of the cavity and propose a possible
interpretation as magnetic interlaced 3-D flux ropes and loops
evacuating the corona, in addition to twisted flux ropes where the
prominence plasma is condensing. Future space missions like ASPIICS
should pay more attention to cavities and emptiness, to coronal dynamics
around prominences, in order to resolve the long-standing problem of
the origin of prominences and perhaps, perform a new diagnostic of
the erupting process responsible for many CMEs.

---------------------------------------------------------
Title: Coronagraphic Broad-Band Hα Observations 1998 -- 2000
Authors: Meunier, N.; Noëns, J. -C.; Romeuf, D.; Koutchmy, S.;
Jimenez, R.; Wurmser, O.; Rochain, S.
2007ASPC..368..351M Altcode:
Broad-band full-limb Hα images of the inner corona were obtained
since the beginning of the solar cycle 23 using one of the Pic-du-Midi
coronagraph. We developed a tool to process the complete set of stored
images and to automatically extract the properties and evolutions of the
observed cold H I coronal structures over a large range of sizes and
light fluxes, from small jets and/or spikes to large prominences. The
paper describes the recognition techniques implemented in our
software and discusses its use. Then we present some new results
following a statistical analysis of the occurrence of structure
parameters applied to a large sample of observations. It illustrates
the capabilities of this software when applied to our database. Strong
activity-asymmetries over the solar poles are shown, confirming similar
results from elsewhere. We also discuss the distribution of relative
light fluxes of these structures over a wide range of sizes. See also
http://bass2000.bagn.obs-mip.fr.

---------------------------------------------------------
Title: On the Dynamic Nature of the Prolate Chromosphere
Authors: Filippov, B.; Koutchmy, S.; Vilinga, J.
2007ASPC..368..177F Altcode:
The upper edge of the solar chromosphere looks not like a perfect circle
in some spectral lines. It is prolate in the South-North direction at
the epoch of minimum solar activity and nearly spherically symmetrical
at the maximum phase. We attribute the effect to the dynamical nature
of the upper chromosphere, which consists of a large number of small
cool jets (jetlets) ascending into the corona. A proposed simple
geometric model can explain the effect of the prolateness of the
solar chromosphere. Due to the dynamic nature of the solar atmosphere
above the 2 Mm level, the magnetic field is considered to play a
very important role in the density distribution with the height,
guiding the mass flows along the field lines. The difference of the
magnetic field topology in the polar and the equatorial regions leads
to different heights of the chromospheric limb. We could not resolve
a source region of an individual jetlet, however similar but larger
structures are visible in EUV coronal lines. We present an example
of the jet formation obtained by TRACE in the 171 Å channel. Field
aligned motion arises above the null point created in the corona by
the emerging magnetic bipole. The scale of bipole is large enough to
recognize the saddle structure around the 3D null point in the TRACE
images. We believe that similar but smaller processes could happen
very often at smaller scale in the chromosphere near emerging magnetic
ephemeral regions forming numerous jetlets of the upper chromosphere.

---------------------------------------------------------
Title: The Solar Eclipse of 2006 and the Origin of Raylike Features
in the White-Light Corona
Authors: Wang, Y. -M.; Biersteker, J. B.; Sheeley, N. R., Jr.;
Koutchmy, S.; Mouette, J.; Druckmüller, M.
2007ApJ...660..882W Altcode:
Solar eclipse observations have long suggested that the white-light
corona is permeated by long fine rays. By comparing photographs of
the 2006 March 29 total eclipse with current-free extrapolations of
photospheric field measurements and with images from the Solar and
Heliospheric Observatory (SOHO), we deduce that the bulk of these
linear features fall into three categories: (1) polar and low-latitude
plumes that overlie small magnetic bipoles inside coronal holes,
(2) helmet streamer rays that overlie large loop arcades and separate
coronal holes of opposite polarity, and (3) “pseudostreamer” rays
that overlie twin loop arcades and separate coronal holes of the
same polarity. The helmet streamer rays extend outward to form the
plasma sheet component of the slow solar wind, while the plumes and
pseudostreamers contribute to the fast solar wind. In all three cases,
the rays are formed by magnetic reconnection between closed coronal
loops and adjacent open field lines. Although seemingly ubiquitous
when seen projected against the sky plane, the rays are in fact rooted
inside or along the boundaries of coronal holes.

---------------------------------------------------------
Title: Chromospheric and Prominence Physics with the ASPIICS Formation
Flying Coronagraph
Authors: Lamy, P.; Vivès, S.; Koutchmy, S.; Arnaud, J.
2007ASPC..368..639L Altcode:
Classical externally-occulted coronagraphs are presently limited in
their performances by the distance between the external occulter and
the front objective. The diffraction fringe from the occulter and
the vignetted pupil which degrades the spatial resolution prevent
observing the inner corona inside typically 2--2.5 solar radii
(R⊙). Formation flying opens new perspectives and allow to
conceive giant, externally-occulted coronagraphs using a two-component
space system with the external occulter on one spacecraft and the
optical instrument on the other spacecraft. ASPIICS (Association
de Satellites Pour l'Imagerie et l'Interférométrie de la Couronne
Solaire) is a mission proposed to ESA in the framework of the PROBA-3
program of formation flying which is presently under study, to exploit
this technique for coronal observations. ASPIICS is composed of a
single coronagraph which performs high spatial resolution imaging of
the corona as well as 2-dimensional spectroscopy of several emission
lines (in particular the forbidden line of Fe XIV at 530.285 nm) from
the coronal base out to 3 R⊙. The classical design of an
externally occulted coronagraph is adapted to the detection of the very
inner corona, and the addition of a Fabry-Pérot interferometer. By
tuning the position of the occulter spacecraft, it will be possible to
reach the chromosphere and the upper part of the spicules. Filtergrams
on the helium D3 line or even better, the hydrogen Hβ line (which is
optically thin contrary to Hα) will give access to the “cold corona”,
and could allow measuring the chromospheric prolateness.

---------------------------------------------------------
Title: On the dynamic nature of the prolate solar chromosphere:
jet formation
Authors: Filippov, B.; Koutchmy, S.; Vilinga, J.
2007A&A...464.1119F Altcode:
Context: In "cool" spectral lines, the smoothed upper edge of the
solar chromosphere is prolate in the South-North direction at the
epoch of minimum solar activity and nearly spherically symmetric at
the maximum phase. We attribute the effect to the dynamical nature
of the upper chromosphere, which consists of a large number of small
jet-like structures ascending into the corona. We could not resolve
the source region of an individual jetlet, although similar but
larger structures are visible, especially in EUV coronal lines. Aims: We consider the problem of the formation of an individual
jet above the limb, assuming that a large number of jet-like events
is responsible for the prolate solar upper chromosphere. We then
assume that spicules, being the cool part of the phenomenon, behave
similarly, and we will mainly concentrate the analysis on the magnetic
origin of the event. Methods: Image processing is used to reveal
the displacement of magnetic field tubes filled with coronal plasma
and jet formation due to field aligned motion above the null point
created in the corona by the emerging magnetic bipole. Results:
The growth of the bipole leads to a reconnection of the field lines
and to a specific plasma motion in the vicinity of the null point
that results in a plasma flow along the spine line of the 3D null. We
assume that similar but smaller processes could happen very often at
a smaller scale in the chromosphere, near emerging magnetic ephemeral
regions, forming numerous jetlets in the upper chromosphere. As the
field aligned motion is guided by the magnetic field, at the epoch
of low activity the large-scale structure of the polar magnetic field
and the one of the quiet equatorial region is sufficiently different
to explain the prolateness of the chromosphere.

---------------------------------------------------------
Title: Analysis of broad-band Hα coronagraphic observations
Authors: Romeuf, D.; Meunier, N.; Noëns, J. -C.; Koutchmy, S.;
Jimenez, R.; Wurmser, O.; Rochain, S.; "Observateurs Associés" Team
2007A&A...462..731R Altcode:
Context: Daily broad-band full-limb Hα images of the inner corona were
obtained during solar cycle 23 (1994-2005) using the 15 cm Pic-du-Midi
coronagraph. Aims: We want to automatically extract the properties
and evolutions of the observed cool HI coronal structures over a wide
range of sizes and light fluxes, from small jets and/or spikes to
large prominences. Methods: A tool was developed to process the
complete set of stored images. This paper describes the recognition
techniques implemented in our software and discusses its use. It
includes the removal of the parasitic diffraction ring produced by
the set of different occulting disks used throughout the year. Results: We present and discuss selected results from a statistical
analysis of the occurrence of parameters characterizing the observed
structures applied to a large sample of observations. It illustrates
the capabilities of this software when applied to our database. Strong
asymmetries of the activity level over the solar poles become evident,
confirming similar results from previous works. We also discuss
the distribution of relative light fluxes of these structures over
a wide range of sizes. Conclusions: The complete series of
FITS and calibrated images, the list of the detected structures,
and their geometric and luminosity evolutions are stored in the
BASS2000 solar database catalogue (http://bass2000.bagn.obs-mip.fr)
and are made publicly available. The Hα HI structures observed over
the limb of the sun present statistical properties of great interest
for understanding its eruptive activity.

---------------------------------------------------------
Title: Analysis of broad-band Hα coronagraphic observations
Authors: Noëns, J. -C.; Romeuf, D.; Meunier, N.; Koutchmy, S.;
Jimenez, R.; Wurmser, O.; Rochain, S.; "O. A. " Team
2006sf2a.conf..557N Altcode:
Broad-band full-limb H-alpha images of the inner corona were obtained
since the beginning of the solar cycle 23 using one of the Pic-du-Midi
coronagraph. We developed a tool to process the complete set of stored
images and to extract automatically the properties and evolutions of
the observed cold HI coronal structures over a large range of sizes and
light fluxes, from small jets and/or spikes to large prominences. The
paper describes the recognition techniques implemented in our
software and discusses its use. Then we present some new results
following a statistical analysis of the occurrence of structure
parameters applied to a large sample of observations. It illustrates
the capabilities of this software when applied to our database. Strong
activity-asymmetries over the solar poles are shown, confirming similar
results from elsewhere. We also discuss the distribution of relative
light fluxes of these structures over a wide range of sizes. See also:
http://bass2000.bagn.obs-mip.fr.

---------------------------------------------------------
Title: Preliminary results from the March 29, 2006 total eclipse
observations in Egypt
Authors: Koutchmy, S.; Daniel, J. -Y.; Mouette., J.; Vilinga, J.;
Noëns, J. -C.; Damé, L.; Faurobert, M.; Dara, H.; Hady, A.; Semeida,
M.; Sabry, M.; Domenech, A.; Munier, J. -M.; Jimenez, R.; Legault,
Th.; Viladrich, Ch.; Kuzin, S.; Pertsov, A.; O. A. Team
2006sf2a.conf..547K Altcode:
A coordinated effort has been carried in the framework of
the French-Egyptian scientific cooperation to permit joined
simultaneous eclipse observations of the solar corona during the
total solar eclipse of March 29, 2006. Spaceborne EIT and Lasco (SoHO)
observations were also planned at the same time and were successfully
collected. Scientists from other countries collaborated on different
experiments. The synthetic image showing the magnetic coronal structure
of this quasi-minimum corona seen in W-L is given. Some preliminary
results are presented; a White Light (W.L.) movie has been also taken
during the totality.

---------------------------------------------------------
Title: ASPIICS, a giant externally occulted coronagraph for the
PROBA-3 formation flyer mission
Authors: Vivès, S.; Lamy, P.; Koutchmy, S.; Arnaud, J.
2006cosp...36.3063V Altcode: 2006cosp.meet.3063V
Formation flyers open new perspectives and allow to conceive giant
externally-occulted coronagraphs using a two-component space system with
the external occulter on one spacecraft and the optical instrument on
the other spacecraft at approximately 100 m from the first one ASPIICS
Association de Satellites Pour l Imagerie et l Interferometrie de la
Couronne Solaire is a mission proposed to ESA in the framework of the
PROBA-3 program of formation flyers which is presently in phase A to
exploit this technique for coronal observations ASPIICS is composed of
a single coronagraph which performs high spatial resolution imaging of
the corona as well as 2-dimensional spectroscopy of several emission
lines from the coronal base out to 3 Rs The selected lines allow to
address different coronal regions the forbidden line of FeXIV at 530
285 nm coronal matter Fe IX X at 637 4 nm coronal holes HeI at 587
6 cold matter An additional broad spectral channel will image the
white light corona and derive electron densities The classical design
of an externally occulted coronagraph is adapted to the detection
of the very inner corona as close as 1 01 Rs and the addition of
a Fabry-Perot interferometer using a so-called etalon ASPIICS will
address the question of the coronal heating and the role of waves by
characterizing propagating fluctuations waves and turbulence in the
solar wind acceleration region and by looking for oscillations in the
intensity and Doppler shift of spectral lines The combined imaging
and spectral diagnostics capabilities available with ASPIICS

---------------------------------------------------------
Title: On the solar white-light high resolution observations from
space
Authors: Veselovsky, I. S.; Koutchmy, S.
2006AdSpR..37.1576V Altcode:
Absolutely calibrated telescopic observations of the Sun in white-light
with a sufficiently high space-time resolution from space have
not been regularly performed. They are needed to resolve several
important problems in the solar physics. Contributions of different
morphological features to the total solar irradiance variations in
the broad range of time scales from seconds up to many years can
be definitely established in this manner for the first time. The
quantitative role of the white-light emission in the overall energy
balance of flares and eruptions on the Sun can be evaluated. More
adequate theoretical models of corresponding processes on the Sun can
be constructed using this new data.

---------------------------------------------------------
Title: Chromospheric Prolateness: Solar Cycle Variations
Authors: Vilinga, J.; Koutchmy, S.; Auchere, Fr.; Baudin, Fr.;
Filippov, B.; Noens, J. -C.
2006IAUS..233..240V Altcode:
The solar prolateness (also known as Ovalisation, a french origin name)
of the extended dynamical chromosphere is established from measurements
performed above 2 Mm heights during the years of solar minimum, using
the Hα, Ca II K and HeII 304 line emissions from both ground-based and
space-based observations. Coronal X-EUV emissions usually penetrate
deep enough into the chromosphere to completely mask this effect
on transition region lines and produce the so-called coronal hole
effect. However, cool lines like Hα and Ca II lines, do NOT show
this Coronal Hole (CH) effect. Coronal lines and HeI (D3; 1083 nm)
do show CHs but do not show the prolateness effect. We first briefly
review different methods which can potentially be used to measure
the prolateness. Further we note the similarity of the geometric
behaviour of the prolateness and its variation along the solar cycle
compared to the behaviour of the fast solar wind. It suggests the same
origin possibly related to the emergence of the small scale network and
internetwork magnetic field towards the corona and small scale magnetic
reconnections. A simple geometric model was proposed to explain the
effect of the prolateness of the solar chromosphere by considering
that the specific dynamical part of the solar atmosphere above the 2
Mm level, being a mixture of up and down moving jets of chromospheric
matter with the coronal plasma between them, is responsible for the
solar prolateness (Filippov and Koutchmy, 2000). We however note that
polar regions are also showing different types of activity in the low
corona, including small prominence eruptions seen e.g. in Hα and
linear jets seen in SXR and EUV as well as in W-L (eclipses). Some
kind of dynamical dissipation of the newly emerged magnetic field is
needed. More systematic measurements should be done to build a more
complete, possibly 3D, picture to explain the extended in the horizontal
direction lifting effect of a large part of the polar chromosphere.

---------------------------------------------------------
Title: SOLARNET &amp; LAIME: Imaging &amp; Spectroscopy in the
Far Ultraviolet
Authors: Damé, Luc; Koutchmy, Serge
2006IAUS..233..435D Altcode:
SOLARNET is a medium size high resolution solar physics mission proposed
to CNES and ESA for a new start in 2007 and a possible launch in 2012
(CNES) or later (ESA Cosmic Vision framework: 2015-2016). Partnerships
with India and China are under discussion, and several European
contributions are considered. At the center of the SOLARNET mission is
a 3-telescope interferometer of 1 meter baseline capable to provide 40
times the best ever spatial resolution achieved in Space with previous,
current or even planned solar missions: 20 mas - 20 km on the Sun in the
FUV. The interferometer is associated to an on-axis Subtractive Double
Monochromator coupled to an Imaging Fourier Transform Spectrometer
capable of high spectral (0.01 nm) and high temporal resolutions
(50 ms) on a field of view of 40 arcsec and covering the FUV and UV
spectral domains (from 117.5 to 400 nm). This will allow to access
process scales of magnetic reconnection, dissipation, emerging flux
and much more, from the chromosphere to the low corona with emphasis
on the transition zone where the magnetic confinement is expected
to be maximum. A whole new chapter of the physics of solar magnetic
field structuring, evolution and mapping from the photosphere to the
high atmosphere will be opened. The interferometer is completed by
instruments providing larger field of view and higher temperature
(EUV-XUV coronal imaging &amp; spectroscopy) to define the context
and extension of the solar phenomena. The 3-telescope interferometer
design results of an extensive laboratory demonstration program
of interferometric imaging of extended objects. We will review the
scientific program of SOLARNET, describe the interferometer concept
and design, present the results of the breadboard and give a short
overview of the mission aspects. In a different category, LAIME,
the Lyman Alpha Imaging-Monitor Experiment, is a remarkably simple
(no mechanisms) and compact full Sun imager to be flown with TESIS on
the CORONAS-PHOTON mission in 2008. It could be the only chromospheric
imager to be flown in the next years, supporting Solar-B, STEREO,
SDO and the Belgian LYRA Lyman Alpha flux monitor. We will give a
short description of this unique 60 mm aperture imaging telescope,
dedicated to the investigation of the UV sources of solar variability
and of the chromospheric and coronal disruptive events (Moreton waves,
prominences, CMEs, etc.).

---------------------------------------------------------
Title: The CME dynamics associated to the prominence eruption of
December 2, 2003
Authors: Slemzin, Vladimir A.; Koutchmy, S.; Noens, J. -C.; Romeuf, D.
2006IAUS..233..395S Altcode:
We report on a complex study of a typical large W-limb CME event
occurring on December 2, 2003 in the vicinity of AR 0508. It is
associated with a prominence eruption which has been observed with the
Pic du Midi Ha flux coronagraph as well as in EUV by both the SOHO/EIT
and the Coronas/SPIRIT space telescopes. The eruption started with the
emergence of a fast expanding loop between 9 and 10 UT, followed by
a heating and an acceleration of the erupted material and resulted in
three-part CME observed by LASCO after 10:50 UT. A temporal analysis
of the prominence motion and the EUV dimming light curve have shown
that both the frontal structure and the core of a CME were initiated
simultaneously with the peak of the X-ray C7.2 flare. The total mass
of the prominence including the Hα filament and EUV filament channel
is close to the mass of the core but significantly less than the total
CME mass.

---------------------------------------------------------
Title: Scientific requirements for future spatially resolved W-L
observations of the Sun
Authors: Veselovsky, I.; Koutchmy, S.
2006cosp...36..202V Altcode: 2006cosp.meet..202V
Several important issues are open in the field of solar variability and
they wait their solution which up to now was attempted using critical
ground-based instrumentations However precise photometric data are
attainable only from space The new observational material should be
collected with high enough spatial resolution starting with the visible
range of the electromagnetic spectrum 1 the absolute contributions of
different small-scale structural entities of the solar atmosphere from
the white light flares and from micro-flares are still poorly known 2 we
do not know the absolute contributions of different structural elements
of the solar atmosphere to the long-term and to the cyclic variations
of the solar irradiance including features of the polar regions of
the Sun 3 the variations of the chromospheric magnetic network are
still poorly evaluated 4 only scarce information is available about
the spectral variations of different small-scale features in the high
photosphere The variability of the Sun in white light can be studied
with higher spectral spatial and time resolution using space-born
telescopes which is much more appropriate for this purpose than ground
based observatories because of better seeing conditions no interference
of the terrestrial atmosphere and a more precise calibration procedure
We discuss the scientific requirements for such observations and the
possible experimental tools proposed for their solution The broader
astrophysical context of the suggested solar studies is also considered

---------------------------------------------------------
Title: The Lyman Alpha Imaging-Monitor Experiment (LAIME) for
TESIS/CORONAS-PHOTON
Authors: Damé, L.; Koutchmy, S.; Kuzin, S.; Lamy, P.; Malherbe,
J. -M.; Noëns, J. -C.
2006cosp...36.3524D Altcode: 2006cosp.meet.3524D
LAIME the Lyman Alpha Imaging-Monitor Experiment is a remarkably
simple no mechanisms and compact 100x100x400 mm full Sun imager to be
flown with TESIS on the CORONAS-PHOTON mission launch expected before
mid-2008 As such it will be the only true chromospheric imager to be
flown in the next years supporting TESIS EUV-XUV imaging SDO and the
Belgian LYRA Lyman Alpha flux monitor on the ESA PROBA-2 microsatellite
launch expected in September 2007 We will give a short description
of this unique O60 mm aperture imaging telescope dedicated to the
investigating of the magnetic sources of solar variability in the UV and
chromospheric and coronal disruptive events rapid waves Moreton waves
disparitions brusques of prominences filaments eruptions and CMEs onset
The resolution pixel is 2 7 arcsec the field of view 1 4 solar radius
and the acquisition cadence could be as high as 1 image minute The back
thinned E2V CCD in the focal plane is using frame transfer to avoid
shutter and mechanisms Further more the double Lyman Alpha filtering
allows a 40 AA FWHM bandwidth and excellent rejection yet providing
a vacuum seal design of the telescope MgF2 entrance window Structural
stability of the telescope focal length 1 m is preserved by a 4-INVAR
bars design with Aluminium compensation in a large pm 10 o around 20 o

---------------------------------------------------------
Title: The Chromospheric Prolateness and its Variations
Authors: Vilinga, J.; Koutchmy, S.
2005ASPC..346..269V Altcode:
The chromospheric prolateness (also called ovalisation) of the extended
dynamical chromosphere was established from measurements performed
above 2Mm heights during the years of solar minimum, using the Hα, Ca
II K and HeII 304 line emissions from both groundbased and spacebased
observations. Coronal X-EUV emissions usually penetrate deep enough
into the chromosphere to completely mask this effect on transition
region lines and produce the so-called coronal hole effect. However,
cool lines like Hα and Ca II lines, do not show this CH effect. Coronal
lines and HeI (D3; 1083 nm) do show coronal holes but no prolateness
effect. We briefly review different methods which can potentially be
used to measure the prolateness. Further we note the similarity of
the geometric behaviour of the prolateness and its variation along
the solar cycle compared to the behaviour of the fast solar wind. It
suggests the same origin related to the emergence of the small scale
network and internetwork magnetic field towards the corona. A simple
geometric model was proposed to explain the effect of the prolateness
of the solar chromosphere by considering that the specific dynamical
part of the solar atmosphere above the 2 Mm level, being a mixture of
up and down moving jets of chromospheric matter with the coronal plasma
between them, is responsible for the solar prolateness. We however note
that polar regions are showing different types of activity in the low
corona, including prominence eruptions seen in Hα and jets seen in
SXR and EUV. Some kind of dissipation of the newly emerged magnetic
field is needed. More systematic measurements should be done to build
a more complete, possibly 3D, picture to explain this lifting effect
of a large part of the chromosphere.

---------------------------------------------------------
Title: About the fe XIV 530.3 NM Line Emissions of the Middle Corona
Authors: Koutchmy, S.; Contesse, L.; Viladrich, Ch.; Vilinga, J.;
Bocchialini, K.
2005ESASP.600E..26K Altcode: 2005ESPM...11...26K; 2005dysu.confE..26K
No abstract at ADS

---------------------------------------------------------
Title: The Center Limb Behavior of Facular-Element Fluxes
Authors: Ajabshirizadeh, A.; Koutchmy, S.
2005ESASP.600E..76A Altcode: 2005dysu.confE..76A; 2005ESPM...11...76A
No abstract at ADS

---------------------------------------------------------
Title: 29 mars 2006 : éclipse totale sur 4 continents

---------------------------------------------------------
Title: 29
mars 2006 : éclipse totale sur 4 continents

---------------------------------------------------------
Title: March 29, 2006 :
total eclipse over four continents
Authors: Crussaire, D.; Durand, P.; Koutchmy, S.
2005O&T....60...28C Altcode:
We first shortly review the ephemerides of the forthcoming March 29,
2006 solar total eclipse, reminding some definitions for computing the
circumstances and providing maps of the eclipse path. The probabilities
for a clear sky is also considered. Further we review some of the
proposed eclipse imaging experiments which are of interest during the
totality, including monochromatic CCD imaging and the complementary
aspects with space experiments analysing the solar corona. High spatial
resolution images of coronal white-light structures are also of great
interest.

---------------------------------------------------------
Title: Formation flyers applied to solar coronal observations:
the ASPICS mission
Authors: Vives, S.; Lamy, P.; Auchere, F.; Vial, J. -C.; Koutchmy,
S.; Arnaud, J.; Prado, J. -Y.; Frassetto, F.; Naletto, G.
2005SPIE.5901..305V Altcode:
Classical externally-occulted coronagraphs are presently limited in
their performances by the distance between the external occulter and
the front objective. The diffraction fringe from the occulter and the
vignetted pupil which degrades the spatial resolution prevent observing
the inner corona inside typically 2-2.5 solar radii. Formation flyers
open new perspectives and allow to conceive giant, externally-occulted
coronagraphs using a two-component space system with the external
occulter on one spacecraft and the optical instrument on the
other spacecraft at approximately 100 m from the first one. ASPICS
(Association de Satellites Pour l'Imagerie Coronographique Solaire)
is a mission proposed to CNES in the framework of their demonstration
program of formation flyers which is presently under study to exploit
this technique for coronal observations. In the baseline concept,
ASPICS includes three coronagraphs operating in three spectral
domains: the visible continuum (K-corona brightness), the HI Lyman
alpha emission line at 121.6 nm, and the HeII emission line at 30.4
nm. Their unvignetted fields of view extend from 1.1 to 3.2 solar radii
with a typical spatial resolution of 3 arcsec. In order to connect
coronal activity to photospheric events, ASPICS further includes
two disk imagers. The first one is devoted to the HI Lyman alpha
emission line. The second one is a multi-channel instrument similar to
SOHO/EIT and devoted to the HeII (30.4 nm), FeIX/X (17.1 nm) and FeXII
(19.5 nm) emission lines. Two concepts of the space system are under
consideration: a symmetric configuration where the disk imagers and
the external occulter are on one spacecraft and the coronagraphs on
the other, an asymmetric configuration where the external occulter is
on one spacecraft and the scientific instruments are regrouped on the
other one.

---------------------------------------------------------
Title: Magnetic Configurations of Streamer Structures in the Solar
Atmosphere
Authors: Koutchmy, S. L.; Molodensky, M. M.
2005AstL...31..398K Altcode:
We consider two types of streamer structures observed in the solar
atmosphere. Structures of the first type are medium-scale configurations
with scale lengths comparable to the scale height in the corona, kT/mg
= 100 thousand km, which appear as characteristic plasma structures in
the shape of a dome surrounding the active region with thin streamers
emanating from its top. In configurations of this type, gravity plays no
decisive role in the mass distribution. The plasma density is constant
on magnetic surfaces. Accordingly, the structure of the configurations
is defined by the condition ψ = const, where ψ is the flux function
of the magnetic field. Structures of the second type are large-scale
configurations (coronal helmets, loops, and streamers), which differ
from the above structures in that their scale lengths exceed the scale
height in the corona. For them, gravity plays a decisive role; as a
result, instead of the magnetic surfaces, the determining surface
is BgradΦ = 0. We constructed three-dimensional images of these
structures. Some of the spatial curves called “visible contours”
of the B r = 0 surface are shown to be brightest in the corona. We
assume that the helmet boundaries and polar plumes are such curves.

---------------------------------------------------------
Title: Analysis of the radiation of coronal suprathermal streams
Authors: Koutchmy, S.; Nikoghossian, A. G.
2005Ap.....48...62K Altcode:
This paper reports on the first measurements of the color index of the
coronal suprathermal streams. Observations performed during the total
eclipse of 2001 in Angola imply that the color index of streams differs
markedly from that for adjacent parts of the surrounding corona taken
as reference. The registered drifts to the longwave and shortwave
domains of the spectrum are in agreement with theoretical results
obtained recently by the authors.

---------------------------------------------------------
Title: Solar origins of intense geomagnetic storms in 2002 as seen
by the CORONAS-F satellite
Authors: Panasenco, O.; Veselovsky, I. S.; Dmitriev, A. V.; Zhukov,
A. N.; Yakovchouk, O. S.; Zhitnik, I. A.; Ignat'ev, A. P.; Kuzin,
S. V.; Pertsov, A. A.; Slemzin, V. A.; Boldyrev, S. I.; Romashets,
E. P.; Stepanov, A.; Bugaenco, O. I.; Bothmer, V.; Koutchmy, S.;
Adjabshirizadeh, A.; Fazel, Z.; Sobhanian, S.
2005AdSpR..36.1595P Altcode:
We analyze solar origins of intense geomagnetic perturbations recorded
during 2002. All of them were related to coronal mass ejections
(CMEs). The initiation of CMEs was documented using the SPIRIT
instrument (SPectrohelIographic Soft X-Ray Imaging Telescope) onboard
the CORONAS-F satellite. Monochromatic full Sun images taken in the Mg
XII doublet at 8.418 and 8.423 Å showed the appearance of free energy
release sites at altitudes up to 0.4 solar radii. CMEs were initiated
at these sites and propagated in interplanetary space under appropriate
local conditions including the geometry of the magnetic fields.

---------------------------------------------------------
Title: Analysis of non-thermal velocities in the solar corona
Authors: Contesse, L.; Koutchmy, S.; Viladrich, C.
2004AnGeo..22.3055C Altcode:
Available from <A
href="http://www.copernicus.org/site/EGU/annales/22/8/3055.htm?FrameEngine=false;">http://www.copernicus.org/site/EGU/annales/22/8/3055.htm?FrameEngine=false;</A>

---------------------------------------------------------
Title: The August 11th, 1999 CME
Authors: Koutchmy, S.; Baudin, F.; Bocchialini, K.; Daniel, J. -Y.;
Delaboudinière, J. -P.; Golub, L.; Lamy, P.; Adjabshirizadeh, A.
2004A&A...420..709K Altcode:
We present here a set of observations, space borne and ground based,
at different wavelengths, of the solar corona at and after the time of
the total solar eclipse of August 11{th}. It is used to consider some
unusual features of the coronal dynamics related to a limb Coronal Mass
Ejection (CME) observed after the total eclipse. The complementary
aspect of simultaneous ground-based and space-borne observations
of the corona is used to produce an accurate composite image of the
White Light (W-L) corona before the CME. A high arch system (possibly
a dome-like structure, with large cavities inside but without a cusp
further out) which appeared on the eclipse W-L images, is suggested to
be a large-scale precursor of the CME, well preceding the eruption of
the top part of the brightest prominence recorded in W-L. This bright
prominence is shown as a filament in absorption using the Transition
Region And Corona Explorer (TRACE) images taken in different coronal
lines. The analysis of the images of the Large Angle and Spectrometric
Coronograph (LASCO) on board the Solar and Heliospheric Observatory
(SoHO), showing the progression of the CME, is discussed in an attempt
to make a connection with the surface event. A SoHO-EIT (Extreme
UV Imager Telescope) image sequence details the prominence eruption
and shows the sudden heating processes of the ejected parts. We found
that there is no reason to assume that the huge cavity is significantly
destabilised well before the eruption of the upper part of the low-lying
bright twisted filament which coincides with the position of one of
the legs of the high arch. Observations are still compatible with the
assumption of both the break-out model and of the flux rope erupting
model as a result of a shear or of an increasing poloıdal magnetic
flux from below. We stress the possible role of buoyancy of the giant
cavity as a destabilizing factor leading to the CME, noticing that some
motion of coronal material back toward the surface can be seen during at
least the first phase of the CME, from both EIT and LASCO observations.

---------------------------------------------------------
Title: Dynamics of the loop prominence and coronal mass ejection
observed on March 2, 2002
Authors: Panasenco, O.; Veselovsky, I. S.; Zhukov, A. N.; Yakovchouk,
O. S.; Koutchmy, S.; Delaboudiniere, J. -P.
2004cosp...35.2974P Altcode: 2004cosp.meet.2974P
SOHO/EIT and LASCO data are used for the case study of the coronal mass
ejection initiation and development. The shape, velocity and temperature
of the loop prominence before and during the ejection as well as the
new arcade formation are well documented. The prominence consisted of
two spirals interweaved on the semi-torus. Both spirals are clearly
seen during the initial stage of the expansion with a velocity about
300 km/s. Than, one of them is rapidly heated, when other remained
cool. The number of curls is conserved during the expansion. The
main axis of the torus is initially represented by the planar curve
resembling a semi-circle. After some time, the summit of the torus
is twisted in the manner that the main axis looks not planar at the
top in the field of view of LASCO C3 when the velocity attains about
1000 km/s. The topological connectivity of the loops to the Sun is
preserved for more than three hours even after the new arcade formation.

---------------------------------------------------------
Title: H/He+ intensity variations of the cool corona
Authors: Noens, J. -C.; Balestat, M. -F.; Jimenez, R.; Rochain, S.;
Romeuf, D.; Auchere, F.; Delaboudiniere, P.; Koutchmy, S.
2004IAUS..223..291N Altcode: 2005IAUS..223..291N
No abstract at ADS

---------------------------------------------------------
Title: Structure and Dynamics of the Solar Corona
Authors: Koutchmy, S.
2004IAUS..223..509K Altcode: 2005IAUS..223..509K
We briefly review several aspects of the quasi-stationary structure
of the corona in relation with the helio-sheet and, also, of the
more confined by the magnetic field structures, including streamers,
loops, jets, plumes and narrow linear rays. Both the temperature and
the density structures are tentatively considered. Flows deduced from
proper motions analysis are discussed. We did not include CMEs and
flares in this presentation but other more radial and possibly highly
impulsive beams with flows are discussed. We stress the importance of
the variations of the coronal magnetic field and inferred currents in
explaining the observed structures.

---------------------------------------------------------
Title: Wavelet Analysis of Umbral Oscillations
Authors: Christopoulou, E. B.; Skodras, A.; Georgakilas, A. A.;
Koutchmy, S.
2003ApJ...591..416C Altcode:
We study the temporal behavior of the intensity and velocity
chromospheric umbral oscillations, applying wavelet analysis techniques
to four sets of observations in the Hα line and one set of simultaneous
observations in the Hα and the nonmagnetic Fe I (5576.099 Å) line. The
wavelet and Fourier power spectra of the intensity and the velocity at
chromospheric levels show both 3 and 5 minute oscillations. Oscillations
in the 5 minute band are prominent in the intensity power spectra; they
are significantly reduced in the velocity power spectra. We observe
multiple peaks of closely spaced cospatial frequencies in the 3 minute
band (5-8 mHz). Typically, there are three oscillating modes present:
(1) a major one near 5.5 mHz, (2) a secondary near 6.3 mHz, and (3)
oscillations with time-varying frequencies around 7.5 mHz that are
present for limited time intervals. In the frame of current theories,
the oscillating mode near 5.5 mHz should be considered as a fingerprint
of the photospheric resonator, while the other two modes can be better
explained by the chromospheric resonator. The wavelet spectra show a
dynamic temporal behavior of the 3 minute oscillations. We observed
(1) frequency drifts, (2) modes that are stable over a long time
and then fade away or split up into two oscillation modes, and (3)
suppression of frequencies for short time intervals. This behavior
can be explained by the coupling between modes closely spaced in
frequency or/and by long-term variations of the driving source of the
resonators. Based on observations performed on the National Solar
Observatory/Sacramento Peak Observatory Richard B. Dunn Solar Telescope
(DST) and on the Big Bear Solar Observatory Harold Zirin Telescope.

---------------------------------------------------------
Title: Chromospheric Evershed flow
Authors: Georgakilas, A. A.; Christopoulou, E. B.; Skodras, A.;
Koutchmy, S.
2003A&A...403.1123G Altcode:
We studied the chromospheric Evershed flow from filtergrams obtained
at nine wavelengths along the Hα profile. We computed line-of-sight
velocities based on Becker's cloud model and we determined the
components of the flow velocity vector as a function of distance
from the center of the sunspot, assuming an axial symmetry of both
the spot and the flow. We found that the flow velocity decreases
with decreasing height and that the maximum of the velocity shifts
towards the inner penumbral boundary. The flow related to some fibrils
deviates significantly from the average Evershed flow. The profile of
the magnitude of the flow velocity as a function of distance from the
spot center, indicates that the velocity attains its maximum value in
the downstream part of the flow channels (assumed to have the form of a
loop). This behavior can be understood in terms of a critical flow that
pass from subsonic to supersonic near the apex of the loop, attains
its higher velocity at the downstream part of the loop and finally
relaxes to subsonic through a tube shock. We computed the average flow
vector from segmented line-of-sight velocity maps, excluding bright
or dark fibrils alternatively. We found that the radial component of
the velocity does not show a significant difference, but the magnitude
of the vertical component of the velocity related to dark fibrils is
higher than that related to bright fibrils. Based on observations
performed on the NSO/SPO Richard B. Dunn Solar Telescope (DST).

---------------------------------------------------------
Title: The solar high-resolution imager - coronagraph LYOT mission
Authors: Vial, Jean-Claude; Song, Xueyan; Lemaire, Philippe; Gabriel,
Alan H.; Delaboudiniere, Jean-Pierre; Bocchialini, Karine; Koutchmy,
Serge L.; Lamy, Philippe L.; Mercier, Raymond; Ravet, Marie Francoise;
Auchere, Frederic
2003SPIE.4853..479V Altcode:
The LYOT (LYman Orbiting Telescope) solar mission is proposed to
be implemented on a micro-satellite of CNES (France) under phase A
study. It includes two main instruments, which image the solar disk
and the low corona up to 2.5 Ro in the H I Lyman-α line
at 121.6 nm. The spatial resolution is about 1” for the disk and
2.5” for corona. It also carries an EIT-type telescope in the He II
(30.4 nm) line. The coronagraph needs a super polished mirror at the
entrance pupil to minimize the light scattering. Gratings and optical
filters are used to select the Lyman-α wavelength. VUV cameras with
2048×2048 pixels record solar images up to every 10 seconds. The
satellite operates at a high telemetry rate (more then 100 kb/s,
after onboard data compression). The envisaged orbits are either
geostationary or heliosynchronous. Possible launch dates could be end
of 2006 - beginning of 2007.

---------------------------------------------------------
Title: Coronal linear threads: W-L radiation of supra-thermal streams
Authors: Koutchmy, S.; Nikoghossian, A. G.
2002A&A...395..983K Altcode:
The paper aims at revealing the role of the Compton effect when
considering the W-L scattering of the solar photospheric radiation by
coronal supra-thermal streams. We first document several examples
of well observed cases of linear W-L coronal threads extending
above flaring active regions which are good candidates to give the
signature known from the interpretation of radio type III bursts. The
height-dependent model problem of Compton scattering on the beam of
fast electrons gyrating around the lines of force of the magnetic
field is considered. The resulting change in frequency averaged
over the beam and the solid angle, within which the photospheric
radiation falls, is computed for both sunward and antisunward directed
streams. The dependence of the effect on the height above the solar
surface, the speed of electrons and the slope angle is discussed. For
illustration, we consider the case, in which the frequency distribution
of the incident radiation is Planckian. The effective value of the
cross-section of interaction is compared with that for the Thomson
scattering. In particular, we conclude that, depending on the angle
between the directions of the initial outburst and the magnetic
field, the streams moving away from the Sun may produce drifts in
frequency to the shortwave, as well as to the longwave domains of the
spectrum. The effect may become essential even for moderate energies of
fast electrons, and it should be measurable using precise photometric
color index determination, if only the fractional density of fast
electrons is not too small.

---------------------------------------------------------
Title: Center-limb and shape-factor variations of facular elements
Authors: Adjabshirizadeh, Ali; Koutchmy, Serge
2002ESASP.506..415A Altcode: 2002ESPM...10..415A; 2002svco.conf..415A
Digital processing is used to measure the contrast of solar faculae from
a set of high resolution selected images observed at the R.B. Dunn's
76 cm clear aperture vacuum telescope of NSO-Sacramento Peak
Observatory. Five ultra-narrow passbands from Red to Blue (Red, Hα,
Mgbl, Green, Blue) were given by the UBF. The range of heliocentric
distances covered by our measurements is 0.1 &lt; μ = cosθ &lt;
0.4 (θ ɛ 84°, 66°). About 104 facular "points" were
measured over nearly 100 selected images. By averaging and normalizing
the contrast of faculae and plotting them vs. heliocentric angle, we
found that the contrast increases monotonically towards the limb for
all wavelengths. The contrast increases as wavelength decreases. We
did not introduce any correction for the smearing in our measurements,
in order not to bias the results. In addition, we study the variations
of integrated brightnesses or fluxes in order to discuss the flux
contribution of faculae. Fluxes definitely show a peak value near μ =
0.25, and then a decrease towards the limb. The center limb effect of
the shape-factor of facular elements is finally analyzed; the ratio of
apparent sizes in the radial and in the tangential directions do not
show the foreshortening effect expected to be observed over cell-like
structures, suggesting that facular elements are structured by a small
scale highly concentrated magnetic field and not just by the gravity.

---------------------------------------------------------
Title: On Interpretation of the Radiation of Coronal Suprathermal
Streams. II
Authors: Nikoghossian, A. G.; Koutchmy, S.
2002Ap.....45..489N Altcode:
This is the second part of the series of two articles which consider
the effect of Compton scattering of the photospheric radiation on
fast electrons of the coronal suprathermal streams. As compared to
the previous part, a more realistic height-dependent model problem
is treated. The results of numerical calculations for the mean
frequency change and the proper cross-section for both the sunward
and antisunward directed beams of electrons are given as a function
of height and the slope angle. It is concluded that, depending on the
angle between directions of the initial outburst and magnetic field,
the scattering on the beams moving away the Sun may produce measurable
drifts in frequency to shortwave as well as to longwave domains of the
spectrum. At the same time, the sunward directed beams result only in
an increase in the photon energy.

---------------------------------------------------------
Title: About the prominence heating mechanisms during its eruptive
phase
Authors: Filippov, B.; Koutchmy, S.
2002SoPh..208..283F Altcode:
Recent EUV observations reveal that the `image' of the prominence
overlaying coronal emission sometimes suddenly changes from absorption
of EUV radiation to emission during the eruptive phase. This change
reveals fast heating of the plasma within the prominence. We propose
a kinetic mechanism of heating the fluid particles that transforms
magnetic energy of the pre-eruptive magnetic configuration stored in
the filament electric current into heat through collision processes of
counteracting flows. The shape of the flux that the filament is made
of should include upward concave segments to provide the counter flows
within the erupting prominence. A typical twisted flux rope easily meets
this requirement. Gas dynamic calculations are offered in addition to
permit a quantitative evaluation of the relevant parameters and their
time variations.

---------------------------------------------------------
Title: Coronal Linear Supra-thermal Streams
Authors: Koutchmy, S.; Nikoghossian, A.
2002sf2a.conf..143K Altcode:
Linear structures of the Solar Corona seen on eclipse images above
active regions after the flaring activity are good candidates for
being produced by primary supra-thermal streams of electrons. We
propose a method to compute the Compton scattering effect applied
to this case and compute the corresponding diagrams. This predicted
effect will be search for on eclipse data and possibly using the SoHO
Lasco coronagraph observations.

---------------------------------------------------------
Title: The global August 11, 1999 eclipse corona and solar cycle
variations
Authors: Adjabshirizadeh, Ali; Koutchmy, Serge
2002ESASP.477...65A Altcode: 2002scsw.conf...65A
Qualitative results from the last solar total eclipse (August 11th,
1999) are presented in order to extract some quantitative parameters
permitting to discuss the structure of the near-maximum corona and
insert the results among what is known of the changing with the solar
cycle of activity structure. The collaborative study of the solar
corona has been performed in Iran, using a radial gradient filter in
white light and other techniques. From the eclipse-processed pictures, a
structural drawing was analysed to give the distribution of streamlines
over the entire corona, in order to look at the deviations from the
local radial direction of identified coronal streamers. From the deduced
parameter and the known solar cycle variations of this instantaneous
"average deviation" of coronal streamers, as deduced from eclipse
observations of 4 preceding cycles, we correctly predicted the moment
of the following maximum of activity. We further discuss the method,
using the "average deviations" measured in 1996 - 2001 from the Lasco C2
coronagraph processed images (from NRL) of SoHO and found an excellent
agreement with the parameters deduced from the last total eclipses of
1998, 1999 and 2001. We believe that "average deviations" are a good
parameter to contribute in the understanding of the origin of solar
cycle variations of the solar wind and of the magnetic field.

---------------------------------------------------------
Title: The August 11th, 1999 total eclipse CME
Authors: Koutchmy, S.; Baudin, F.; Bocchialini, K.; Delaboudinière,
J. -P.; Adjabshirizadeh, A.
2002ESASP.477...55K Altcode: 2002scsw.conf...55K
We use spaceborne observations and ground-based eclipse observations
to analyse the spectacular W-limb CME which occurred several hours
after the totality in Iran. The underlying high arch system (possibly
a dome-like structure with cavities inside) which appeared on the
eclipse White-Light (W-L) images, is suggested to be a large scale
precursor of the CME, taking into account the related coronal cavities
(as measured from the broadening of the green Fe XIV line) and the
properties of the inserted prominence which erupted during the CME.

---------------------------------------------------------
Title: The Three-Dimensional Structure of the Solar Corona
Authors: Koutchmy, S. L.; Merzlyakov, V. L.; Molodenskii, M. M.
2001ARep...45..834K Altcode:
The surface where the radial component of the solar magnetic field
changes sign is computed for a minimum corona. It is shown that (1)
the projection of the folds of this surface onto the plane of the
sky is consistent with the helmet structures observed during the
eclipse of June 30, 1954; (2) there are type 1 and type 2 helmets,
according to the well-known classification of coronal structures; (3)
some elements of this sign-change surface of the radial field can be
classified as so-called envelopes. The results obtained suggest that
more complex coronal structures can be described in a similar way. An
MHD model of polar plumes is considered.

---------------------------------------------------------
Title: Interpretation of the Radiation of Coronal Suprathermal
Streams. I.
Authors: Nikoghossian, A. G.; Koutchmy, S.
2001Ap.....44..528N Altcode:
This is the first part of a series of two articles aimed at revealing
the role of the Compton effect in scattering of the solar photospheric
radiation by coronal suprathermal streams. The simplest situation of a
single beam of electrons gyrating around the strength lines of magnetic
field is considered. Attention is focused on the height-independent
problem, in which the role of the spatial angle of incident radiation is
ignored. Analytical expressions for the frequency change of interacting
photons and for the proper cross-section of the scattering process are
derived. The results of numerical calculations show that the effect
may by significant even for moderate energies of fast electrons and
will be observable only if the fractional density of fast electrons
is not too small.

---------------------------------------------------------
Title: Multi-wavelength study of Network Bright Points near the limb*
Authors: Georgakilas, A. A.; Christopoulou, E. B.; Koutchmy, S.
2001SoPh..202..241G Altcode:
We analyze the morphology of network bright points (NBPs), their
relation to fine dark mottles and their temporal variations,
using observations of a quiet region near the polar solar limb,
obtained during the solar minimum. For our analysis we used an
image-processing method for the selection and identification of
NBPs. Further we constructed 'maximum power frequency' maps computing
the power spectrum for each pixel of a field and selecting the frequency
of maximum spectral power as the most representative oscillating
frequency for this pixel. The morphological analysis of our data
indicates that the enhancement of NBPs is part of a complicated process
that is responsible for the formation of mottles. The analysis of the
lifetimes of NBPs indicates that although the general patterns of NBPs
remain constant for time intervals larger than an hour, the lifetime
of individual bright points is of the order of 16 min. Furthermore,
our results indicate an association of the lifetime of NBPs with that
of mottles. From the analysis of temporal variations we confirm that the
power of NBPs is smaller than the corresponding power for intra-network
points at both the 3-min and the 5-min oscillating modes and in both
the Mg b1−0.4 Å and the continuum. Our analysis revealed
enhanced power in the 7-min range, which is theoretically considered
a candidate frequency for transverse waves related to NBPs at the base
of the chromosphere (Kalkofen, 1997). However, we consider more likely
that this period is related to the evolution of individual NBPs.

---------------------------------------------------------
Title: Fine Structure of the Quiet Solar Chromosphere: Limb-Crossing
Features
Authors: Zachariadis, Th. G.; Dara, H. C.; Alissandrakis, C. E.;
Koutchmy, S.; Gontikakis, C.
2001SoPh..202...41Z Altcode:
In this article we study chromospheric structures (spicules) crossing
the solar limb in Hα images corrected for limb darkening. This
correction enabled us to view structures both on the disk and beyond the
limb in the same image. The observations were obtained at the Sacramento
Peak Observatory at Hα±0.75 Å. The processed images reveal both
bright and dark (relative to the local background) features crossing
the limb. We also observed bushes (rosettes) crossing the limb, as well
as structures indicating probably arch-shaped mottles beyond the limb.

---------------------------------------------------------
Title: Oscillations and running waves observed in
sunspots. III. Multilayer study
Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, S.
2001A&A...375..617C Altcode:
We continue our study of waves and oscillations observed in sunspots
using an improved method for enhancing the waves, giving the opportunity
to identify them and determine their properties in far Hα wings. We
found that the running penumbral waves are observable at least up to
the formation height of the Hα +/- 0.5 Å line, but not in the Hα +/-
0.75 Å or the Fe I+/-0.12 Å. We found a time lag between the waves
in the blue and the red wing of the Hα line corresponding to a phase
shift of 180o, that indicates a pure Doppler shift of the
line. There is a lag in the propagation of the waves seen at Hα center
and at Hα wings. Also there is a lag in the variation of the umbral
oscillations as they are observed from lower to higher atmospheric
layers. The correlation between umbral oscillations at various
atmospheric heights and running penumbral waves strongly indicates
that the latter are excited by photospheric umbral oscillations and
not the chromospheric ones. We found a new category of photospheric
waves that originate at approximately 0.7 of the distance between the
umbra and the penumbra boundary and propagate beyond the outer penumbra
boundary with a velocity of the order of 3-4 km s-1. Further,
we found 3 min penumbral oscillations apparent in the inner penumbra
at lower chromospheric layers (far Hα wings). Based on observations
performed on the NSO/SPO Richard B. Dunn Solar Telescope (DST)

---------------------------------------------------------
Title: Polar surges and macrospicules. II. Dynamics of an eruptive
event from off-limb observations
Authors: Georgakilas, A. A.; Koutchmy, S.; Christopoulou, E. B.
2001A&A...370..273G Altcode:
We continue our study of polar surges and macrospicules at the
period of solar minimum, analyzing high resolution multiwavelength
limb observations that provide a clearer picture of the dynamical
phenomena occurring well above the chromosphere of a polar cap. The
time sequence of an erupting and impulsive polar event is examined
from the low chromosphere to coronal heights, deriving both proper
motions and Doppler velocities. Our observations suggest that there is
a close association of polar surges with explosive events, supporting
the hypothesis that magnetic reconnection triggered by emerging flux
provides the accelerative mechanism for this polar region event.

---------------------------------------------------------
Title: Fine Structure of the Magnetic Chromosphere: Near-Limb Imaging,
Data Processing and Analysis of Spicules and Mottles
Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, S.
2001SoPh..199...61C Altcode:
The origin and the dynamical evolution of spicules and mottles continue
to be a highly interesting research subject. Using high-resolution
Hα observations obtained with the Dunn Solar Telescope of the
Sacramento Peak Observatory and an image processing technique for
the enhancement of near-limb solar images, we study the dynamics of
spicules and mottles as well as their relation. Our image-processing
technique is based on the correction for the limb darkening and the
use of a directionally sensitive operator, the `MadMax'. The temporal
evolution of characteristic cases of spicules, dark and bright mottles,
indicates an association between them and supports the suggestion that
the magnetic field and probably related forces play a fundamental
role in their generation and dynamics. We present characteristic
cases of fine bright mottles, observable in the Hα far wings, that
appear in close juxtaposition to dark mottles. The phenomenon appears
to be common, suggesting that the velocities derived from marginal
resolution spectroscopic observations could be underestimated. Typical
examples of individual mottles crossing the solar limb further
support the association between spicules and mottles. Finally we
show images of arch-shaped mottles above the limb and especially on
the disk, confirming the existence of chromospheric small loops. Our
image-processing method substantially enhances near-limb observations
and permits an insight into the studies of the very fine chromospheric
structures.

---------------------------------------------------------
Title: Brightness Variations of mg ib Bright Features
Authors: Dara, H. C.; Koutchmy, S.; Zachariadis, Th. G.; Alissandrakis,
C. E.
2001SoPh..198..313D Altcode:
We study the temporal intensity variations of Mgib bright features and
investigate the corresponding Hα velocity pattern. The network bright
features are well visible in the continuum, in images averaged over the
duration of the observations (130 min). We detected `flashing' bright
features, which appear and disappear within two to five minutes, while
the rest of the bright features undergo small variations of either their
shape and/or their intensity. A power spectrum analysis reveals a 10-min
oscillation for approximately half of the stable bright features. The
5-min oscillations are detected mainly at the network boundaries,
where stable bright features are located, while 3-min oscillations
coincide with few bright features, but are also quite intense inside
the network cells. The majority of bright features are associated
with Hα downflows. The downflow is very intense at the location of
`flashing' bright features.

---------------------------------------------------------
Title: Helical Magnetic Structure of White Light Polar Plumes
Authors: Zhukov, A. N.; Veselovsky, I. S.; Koutchmy, S.; Llebaria, A.
2001IAUS..203..434Z Altcode:
We describe the fine structure of white light polar plumes observed
by SOHO/LASCO C2coronagraph. The evolving helical structures of
different scales are clearly seen on the specifically processed images
(the processing reveals the faint contrast objects). The observed
structures trace the magnetic field lines, sothe electric currents
flow along the axis of the plumes. The MHD model of a plume takinginto
account field-aligned electric currents is developed. The model permits
to understand the existence of high-density plasma inside the plume
due to the balance between the Ampere force and transversal pressure
gradient. Consequences for the solar wind acceleration process and
for the structure of heliospheric current circuit are discussed.

---------------------------------------------------------
Title: Coronal Streamers
Authors: Koutchmy, S.
2000eaa..bookE2271K Altcode:
Streamers are the most outwardly extended structures of the solar
CORONA; they suggest that a permanent mass flow exists around and
further out, inside the furthest parts of streamers. The significance
of streamers in the solar corona should be found in the frame of our
knowledge of the slow solar wind and of the continuous dissipation of
the large-scale solar magnetic field in thin neutral sheet...

---------------------------------------------------------
Title: Oscillations and running waves observed in
sunspots. II. Photospheric waves
Authors: Georgakilas, A. A.; Christopoulou, E. B.; Koutchmy, S.
2000A&A...363..306G Altcode:
To continue our study of waves related to sunspots in the photosphere,
we analyzed CCD, high resolution sunspot observations obtained
in the Fe i 557.6 nm line. We produced “time slice images" which
reveal inward slow propagating waves in the photospheric penumbra and
outward propagating waves in the area around the sunspot. The phase
velocity of the waves is near 0.5 km s-1 in both cases and
their horizontal wavelength about 2500 km. The waves could be related
either to solar p-modes or to the subphotospheric layer large-scale
convection. Based on observations performed on the NSO/SPO Dunn's
Solar Telescope (DST).

---------------------------------------------------------
Title: On the origin of the prolate solar chromosphere
Authors: Filippov, Boris; Koutchmy, Serge
2000SoPh..196..311F Altcode:
A simple geometric model is proposed to explain the recently reported
effect of the prolateness of the solar chromosphere. We assume that a
specific dynamical part of the solar atmosphere above the 2 Mm level,
being a mixture of moving up and down jets of chromospheric matter
with the coronal plasma between them, is responsible for the solar
prolateness. Due to the dynamic nature of this layer, the magnetic
field is considered to play a very important role in the density
distribution with the height, guiding the mass flows along the field
lines. The difference of the magnetic field topology in the polar and
the equatorial regions leads to different heights of the chromospheric
limb. Calculations show a satisfactory coincidence with observations
when the mean separation between opposite polarity concentrations is
about 9 Mm. The possible observational signature of this network in
low photospheric and chromospheric layers is discussed.

---------------------------------------------------------
Title: Eclipse Science Results: Past and Present (Invited review)
Authors: Livingston, W.; Koutchmy, S.
2000ASPC..205....3L Altcode: 2000ltse.conf....3L
We have investigated X-ray ejecta above flare loops, which were observed
before soft X-ray peak time, using the Yohkoh soft X-ray observations
in 1996 when the background corona was very weak. We found 35 plasma
ejecta out of 84 flares and studied soft X-ray data to discover the
probability to observe the plasma ejecta. On the other hand, we searched
for prominence eruptions using Solar-Geophysical Data in the same flare
series and found 16 prominence eruptions out of 29 flares having soft
x-ray plasma ejecta. As a result, 76% of flares have plasma ejecta
observed in either Hα or soft X-ray wavelength. It follows from this
that there are many flare associated ejecta.

---------------------------------------------------------
Title: Oscillations and running waves observed in sunspots
Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, S.
2000A&A...354..305C Altcode:
In order to study umbral oscillations, running penumbral waves and
the relationship between them, we analyzed CCD, high resolution,
sunspot observations obtained at center and the wings of the Hα line
and the Fe I 5576 Ä line. The UBF filter was used in order to produce
high cadence sequences of filtergrams. Images were processed to remove
the sharp intensity gradient between the umbra and the penumbra. They
show the waves to start out around umbral oscillating elements and to
propagate outwards forming concentric cycles around the elements. The
waves appear to propagate beyond the outer edge of the photospheric
penumbra, in the superpenumbra, where they dilute. Comparing images
in 9 wavelengths along the Hα profile we found out that the waves
are definitely better observed near the Hα center and near the blue
wing -0.35 Ä. This indicates a possible vertical upward mass motion
in the oscillating penumbral structure and that the oscillation is not
symmetric about zero. We found different oscillating modes. Standing
umbral oscillations are dominant in the umbra and inner penumbra;
their frequency is around 6.5 mHz. Similar oscillations are observed
in the penumbra - superpenumbra boundary but with considerably lower
frequency (2 mHz). Oscillations are absent or have reduced magnitude
in the central part of the penumbra. Penumbral waves are running waves
propagating with a constant phase velocity around 13 km s-1;
their frequency is remaining constant over the whole penumbra, in the
band of 3 mHz. We produced “time slice images" which show, that there
is not a clear relationship between umbral oscillations and running
penumbral waves.

---------------------------------------------------------
Title: On Stereoimages of Some Structures in the Solar Atmosphere
Authors: Vedenov, A. A.; Koutvitsky, V. A.; Koutchmy, S.; Molodensky,
M. M.; Oraevsky, V. N.
2000ARep...44..112V Altcode:
Three-dimensional structures in the solar chromosphere and corona are
considered. It is demonstrated that two photoheliograms separated by
∼1 day can be used (using computer-graphics methods) to construct
a stereo image of the Sun. The algorithm for this is presented and
carried out for Hα images of the total disk. A bulge in
the equatorial region resulting from the differential rotation of
the Sun can be seen in the stereo image. Structures called Whitney
pleats in catastrophe theory are observed in the solar corona. Such
structures are encountered in prominences. The well-known helmets
(or streamers) are pleats of heliospheric plasma sheets. Isophotes
for such a sheet and the degree of polarization of the radiation in
the pleat are calculated and compared with observational data.

---------------------------------------------------------
Title: Commission 12: Solar Radiation and Structure (Radiation et
Structure Solaires)
Authors: Foukal, Peter; Solanki, Sami; Mariska, J.; Baliunas, S.;
Dravins, D.; Duvall, T.; Fang, C.; Gaizauskas, V.; Heinzel, P.;
Kononovich, E.; Koutchmy, S.; Melrose, D.; Stix, M.; Suematsu, Y.;
Deubner, F.
2000IAUTA..24...73F Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Coronal plasmoid dynamics. II. The nonstationary fine structure
Authors: Zhukov, A. N.; Veselovsky, I. S.; Koutchmy, S.; Delannée, C.
2000A&A...353..786Z Altcode:
We analyze the non-uniform motion of a white light coronal plasmoid
of 1.5 Mm in diameter, which has been followed at the prime focus of
the Canada-France-Hawaii Telescope (CFHT) during the July 11, 1991
total solar eclipse. Two possibilities are considered to explain the
acceleration of the plasmoid by the magnetic force: large amplitude
oscillations and the rotation of the plasmoid magnetic dipole about the
external inhomogeneous magnetic field vector. We then describe for the
first time the fine structure of the plasmoid, its splitting and its
interaction with the surrounding thread-like coronal structures. The
smallest-scale inhomogeneities (knots inside the plasmoid) have a
characteristic length of about 400 km. The observed complex behaviour
of these plasma objects leads us to conclude that existing models of
mass supply to the corona by expanding plasmoids and their input into
the process of the solar wind acceleration seem to be oversimplified,
mainly because the fine structure and the turbulent intermixing have
not been realistically taken into account. We also conclude on the
importance of dynamical processes at the smallest scales coronal
structures when the heating problem is considered.

---------------------------------------------------------
Title: Multiwavelength Observations of Ellerman Bombs
Authors: Georgakilas, A. A.; Christopoulou, E. B.; Koutchmy, S.
1999ESASP.448..279G Altcode: 1999mfsp.conf..279G; 1999ESPM....9..279G
No abstract at ADS

---------------------------------------------------------
Title: Fine Structure of the Solar Chromosphere: Dynamics of Spicules
and Fine Dark Mottles
Authors: Georgakilas, A. A.; Christopoulou, E. B.; Koutchmy, S.
1999ESASP.448..285G Altcode: 1999mfsp.conf..285G; 1999ESPM....9..285G
No abstract at ADS

---------------------------------------------------------
Title: New Results about Running Penumbral Waves
Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, S.
1999ESASP.448..245C Altcode: 1999mfsp.conf..245C; 1999ESPM....9..245C
No abstract at ADS

---------------------------------------------------------
Title: Chromospheric Mass Motions Associated with an Emerging
Flux Region
Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, S.
1999ESASP.448..593C Altcode: 1999ESPM....9..593C; 1999mfsp.conf..593C
No abstract at ADS

---------------------------------------------------------
Title: Eclipse of August 11, 1999: White-light Images and Simultaneous
EIT/SOHO Observations
Authors: Adjabshirizadeh, A.; Baudin, F.; Bocchialini, K.;
Delaboudinière, J. -P.; Grorod, P. -A.; Koutchmy, S.; Laal Aaly,
M.; Lamy, P.; Lochard, J.; Mouette, J.
1999ESASP.448.1283A Altcode: 1999ESPM....9.1283A; 1999mfsp.conf.1283A
No abstract at ADS

---------------------------------------------------------
Title: Dynamics and Nature of Macrospicules
Authors: Georgakilas, A. A.; Koutchmy, S.; Christopoulou, E. B.
1999ESASP.448..291G Altcode: 1999mfsp.conf..291G; 1999ESPM....9..291G
No abstract at ADS

---------------------------------------------------------
Title: L'éclipse du 11 aou^t 1999 et la couronne. Un premier bilan
scientifique.
Authors: Baudin, F.; Koutchmy, S.
1999LAstr.113..326B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Prolate Solar Chromosphere
Authors: Koutchmy, S.; di Folco, E.; Auchere, F.; Baudin, F.;
Delaboudinière, J. -P.; Koutchmy, O.; Noëns, J. -C.; Rondi, S.;
Jimemez, R.; Smartt, R. N.
1999ESASP.446..385K Altcode: 1999soho....8..385K
The solar prolateness above h=2Mm is now well established from
measurements performed during the years of solar minimum in HeII, Hα
and K3CaII lines. Low level coronal emissions usually penetrate deep
enough to completely mask this effect and show CH, quite similarly to
the behaviour of the HeI lines (D3; 1083nm) which does not show the
prolateness. We discuss the most recent observations for 1999 given
by a new facility developped at Pic du Midi Observatory (HACO II)
and we compare the results with EIT results in HeII. We also brielfly
discuss the possible interpretations of the prolateness effect. We
favor topological effects implying a large number of nano-flares
and ejecta during the interactions of small-scale low level network
magnetic fields with the more static large-scale magnetic field.

---------------------------------------------------------
Title: Helical Magnetic Structure Of EUV Polar Plumes
Authors: Veselovsky, I. S.; Zhukov, A. N.; Koutchmy, S.; Delannée,
C.; Delaboudinière, J. -P.
1999ESASP.446..675V Altcode: 1999soho....8..675V
The results of an analysis of joint CDS of SOHO and SXT of Yohkoh
observations of a decaying post-flare loop system are presented. The SXT
images were used to explain some peculiar structural features visible
in the examined CDS raster, resulting from the rapid evolution of the
observed system and from the way the CDS rasters are built. The SXT
data was also used to determine the time evolution of the temperature
and the emission measure of the hot part of the system during its
decay. The CDS data, with a very good temperature coverage, contains
a density sensitive line pair of Fe XIV which was used for electron
density analysis and a temperature sensitive line pair of Fe XVI and
Si XII which was used to study the temperature structure of the loop
system. From the integrated intensities of selected lines the emission
measures were calculated. From these measurements we estimated the
filling factor of the loop system in Fe XIV line.

---------------------------------------------------------
Title: The Global Activity of the Solar Corona
Authors: Llebaria, A.; Lamy, P.; Koutchmy, S.
1999ESASP.446..441L Altcode: 1999soho....8..441L
The question of the global activity of the solar corona, as a function
of time and distance from the center of the Sun, is considered by
analyzing long time-series of LASCO-C2 images. Polarized images
are first considered to perform the separation of the K and F
components. The F-corona images are used to construct a photometric
model of the F-corona wich reflects its annual variations resulting from
geometric effects. This time-varying model is then subtracted from all
corrected and calibrated images (unpolarized) to yield images of the
K-corona. Synoptic maps are created at different distances between 2.5
and 6 solar radii and the total white-light intensity is integrated to
estimate the total mass of the corona. Its variations in the range of
heliocentric distance and over a time span of 3 years will be presented
and discussed.

---------------------------------------------------------
Title: Simultaneous LASCO/1998-Eclipse Observations Of A Large-Scale
Polar Event
Authors: Zhukov, A.; Koutchmy, S.; Lamy, Ph.; Delaboudinière,
J. -P.; Delannée, C.; Bocchialini, K.; Guisard, S.; Filippov, B.;
Veselovsky, I.
1999ESASP.446..731Z Altcode: 1999soho....8..731Z
A relatively faint but large scale polar region event was observed
in Aug. 1996 by Boulade et al. 1998 (SoHO SP 404, 217); we first
reconsider this event which has been related to a high latitude
filament disappearance. We continue the study of this class of events by
analyzing the large scale restructuring which occurred above the N-Pole
region at the time of the last Feb. 26, 1998 total solar eclipse. Well
calibrated WL-eclipse images are used to provide the absolute values
of electron densities of the quasi-radial structure appearing at
the feet of the event. This structure can also be considered as a
type of abnormally broad and curved polar plume, a type of activity
already reported in the literature. Unfortunately, the examination
of sequences of EIT images taken at that time seems to indicate that
the roots of the structure are on the back side of the Sun. However
the most impressive effects are seen in the high polar region, at
several radii, based on the analysis of processed Lasco-C2 difference
images. Large proper motions are deduced over density structures. Both
these events confirm that polar regions are indeed showing a new class
of CME activity (possibly related to the Hewish's CMEs), which is seen
inside coronal holes. A whole set of interesting questions is then
appearing to understand the occurrence of a polar CME propagating in
the heart of a large unipolar magnetic region of the corona.

---------------------------------------------------------
Title: Propagating Magneto-Acoustic Waves in the Network
Authors: Baudin, F.; Bocchialini, K.; Koutchmy, S.
1999ASPC..184..232B Altcode:
The analysis of spectroscopic data taken in the chromospheric network
is interpreted as evidence for propagating waves. These waves are
seen from the photospheric level propagating upward to the highest
levels of the chromosphere at velocities around 40 km/s, suggesting a
magneto-acoustic nature. We note the lack of an adequate one-dimensional
model of the solar chromosphere to interpret these data.

---------------------------------------------------------
Title: Running Penumbral Waves in Sunspots
Authors: Christopoulou, E. B.; Georgakilas, A. A.; Koutchmy, Serge
1999ASPC..184..103C Altcode:
In order to study running penumbral waves, we analyzed high resolution
sunspot observations obtained at the center and the wings of the
Hα line. The sharp intensity gradient between the umbra and the
penumbra has been removed by using an image processing technique. The
processed images show the waves to start out from the umbral oscillating
elements and to propagate outwards forming concentric circles around the
elements. The propagation velocity is between 6 to 18 km s1;
and the average period is about 190 sec.

---------------------------------------------------------
Title: Coordinated observations between SOHO/SUMER and ground during
the 1998 total eclipse: Non-thermal line broadenings and electron
densities in a polar coronal hole
Authors: Patsourakos, S.; Vial, J. -C.; Gabryl, J. -R.; Koutchmy,
S.; Schühle, U.
1999AIPC..471..285P Altcode: 1999sowi.conf..285P
Alfvén waves represent one of the most prominent ways of heating the
solar corona and accelerating the solar wind. One of their signatures
is to broaden the spectral lines in excess of their thermal width. Here
we aim to combine observations of non-thermal broadenings measured
by SUMER in OVI (1037.6 Å) line and electronic densities derived
from white-light observations during the 1998 total eclipse. After
checking the validity of the frequently-used assumption of equal ion
and electron temperatures, we compute the variation of the non-thermal
velocity as a function of height in an interplume region within the
south polar coronal hole.

---------------------------------------------------------
Title: Erratum: "Fine structure of the solar chromosphere: arch-shaped
mottles" [Sol. Phys., Vol. 184, No. 1, p. 77 - 86 (Jan 1999)].
Authors: Zachariadis, T. G.; Georgakilas, A. A.; Koutchmy, S.; Dara,
H. C.; Alissandrakis, C. E.
1999SoPh..187..227Z Altcode:
No abstract at ADS

---------------------------------------------------------
Title: L'imagerie haute résolution. Pourquoi et comment?
Authors: Koutchmy, S.
1999LAstr.113..116K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Eclipse 99: l'imagerie haute résolution: pourquoi et comment?
Authors: Koutchmy, S.
1999C&T...115...82K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Steady-state configuration of the heliospheric sheet
Authors: Koutchmy, S. L.; Molodensky, M. M.; Matsuura, O. T.;
Picazzio, E.
1999AstL...25..258K Altcode:
An analysis of the coronal structure for several eclipses, including
the eclipse of November 3, 1994, shows that coronal streamers and
helmets can be described as folds and pleats produced when the B_r =
0 plane is projected onto the plane of the sky (Vial and Molodensky
1993; Molodensky et al. 1996). We consider equilibrium conditions for
plasma in the heliospheric sheet from the corona base out to distances
of several R_solar. We construct an analytic model that represents the
equilibrium configuration of plasma near the equatorial plane of the
equivalent dipole. This model is characterized by two parameters: the
sheet thickness 1/k (radians) and M/qR_solar. We show the following:
(1) the current in the sheet is opposite in sign to the current that
produces the initial dipole moment of the Sun, and (2) the parameter
that determines the sheet thickness is k = 20. The temperature,
the density, and the magnetic field match the real values of the
corresponding parameters in the corona.

---------------------------------------------------------
Title: Eclipse 99 -- High Resolution Imaging: Why and how?
Authors: Koutchmy, S.
1999CoSka..28..173K Altcode:
A very large white-light (W-L) coronal flux is made available during
total eclipses. High speed analysis of very fine-scale structures
of the magnetically dominated solar atmosphere is then possible,
including the deeply seeded sources of the solar mass loss. Additional
observations of both the disk and of the more outer corona should be
simultaneously collected from space, using the SOHO and the Yohkoh
missions to complement the data. The most optimum eclipse studies
should concentrate on the intermediate corona where acceleration
processes are taking place. MHD waves, including magneto-acoustic
propagating waves and standing loop-resonance waves are everywhere
present with rather short periods. W-L fine imaging at high-speed and
high signal-noise ratio is needed to avoide the overlapping problem
and measure their magnitude. Ubiquitous plasmoid-like objects are
also produced in this region near the temperature maximum and they
need a special attention. They are the rather privileged site where
both the radiative cooling and the magnetic dissipation mechanisms
are occuring. Eclipses are good opportunities to look at the dynamics
of coronal ejecta. At larger scale, sharp edges of streamers and
plumes can be used to deduce a 3-D view of the coronal neutral sheets,
provided pictures taken at several hours interval are made available
along the path of the totality. Both the quasi-rigid rotation and the
more subtil outward motions of coronal material are then evidenced,
giving a good tool to study the origine of the slow wind.

---------------------------------------------------------
Title: The plane of polarization of the solar corona during eclipse
observations
Authors: Koutchmy, S.; Matsuura, O.; Molodensky, M. M.; Picazzio,
E.; Starkova, L. I.
1999ARep...43..198K Altcode:
Analyses of the orientation of the plane of polarization for the solar
corona are presented, based on polarization isophotes of the solar
eclipses of June 30, 1973 (Africa), November 3, 1994 (Brazil), and
March 9, 1997 (Eastern Siberia). Deviations of the polarization plane
from the radial direction, indeed, exist at distances from the solar
limb greater than 0.5 R_solar. These deviations cannot be explained by
the aberration of scattered photons on moving coronal electrons or by
F-corona emission. It is proposed that the deviations are produced by
sky polarization (the auroral ring), i.e., by Rayleigh scattering in the
Earth's atmosphere during the eclipse. A model of the total emission
of the corona taking into account the sky background is constructed,
and the positions of singular points of the polarization tensor with
topological index -1/2 are indicated.

---------------------------------------------------------
Title: Polar surges and macrospicules: simultaneous Hα and He BT
II 304 Angstroms observations
Authors: Georgakilas, A. A.; Koutchmy, S.; Alissandrakis, C. E.
1999A&A...341..610G Altcode:
We compare simultaneous sequences of Hα and He ii 304 Angstroms images
near the solar limb. We propose to distinguish polar surges and giant
spicules (macrospicules), among the He ii structures observed beyond
the solar limb. Polar surges have a complex structure when observed
in Hα and an eruptive nature, reminiscent of normal surges in small
scale. Giant spicules are simple spikes, very narrow compared to
surges. They don't go as high as polar surges and apparently have
shorter lifetimes. We found that most polar surges and giant spicules
observed in He ii are associated with Hα spikes; however there were
cases without any corresponding Hα structure. Furthermore we observed
Hα spikes that did not have He ii counterparts. We analyze an example
of a polar surge that appeared in He ii well before its appearance in
Hα and remained visible for a longer time. Most polar surges that we
observed showed a similar behavior.

---------------------------------------------------------
Title: Mg bright points and the corresponding velocity pattern.
Authors: Dara, H. C.; Zachariadis, T.; Alissandrakis, C.; Koutchmy, S.
1999joso.proc..135D Altcode:
The authors study the temporal intensity variations of the Mg b1
bright points, in an effort to detect oscillations and investigate
the corresponding Hα velocity pattern. Apart from the "flashing
bright points", bright points which appear and disappear within two to
three minutes, the rest of the bright points undergo small intensity
variations. Power spectrum analysis revealed a 10-min oscillation
for half of the stable bright points. The 5-min oscillations are
detected mainly at sites where there are no bright points, while 3-min
oscillations coincide with some of the bright points. The majority of
the bright points are associated with Hα downflows. The downflow is
very intense at the "flashing bright points".

---------------------------------------------------------
Title: Outflow Velocities at the Base of a Polar Coronal Hole During
the 1998 Total Eclipse
Authors: Patsourakos, S.; Vial, J. -C.; Gabryl, J. -R.; Koutchmy,
S.; Schühle, U.
1999SSRv...87..291P Altcode:
Polar coronal holes represent the most convincing site from which the
high-speed solar wind originates. Here we report high-accuracy Doppler
shifts measured in the O VI (1037.6 Å) line obtained by SUMER on SOHO
inside an interplume region within the south polar coronal hole. We
infer limits on the outflow velocity and draw hints about the flow
geometry.

---------------------------------------------------------
Title: Large-Scale Polar Coronal Magnetic Field Model and the Expected
August 11, 1999 Eclipse Corona
Authors: Veselovsky, I. S.; Zhukov, A. N.; Panassenko, O. A.;
Koutchmy, S.
1999RoAJ....9S..29V Altcode:
We compare available SOHO/LASCO C2 images with the model calculations
of the large-scale coronal magnetic field near the magnetic poles of the
Sun. The model field consists of the ones of the dipole and of the thin
current sheet in the plane perpendicular to the dipole. The positions
of the dipole and the current sheet (representing the heliospheric
current sheet) are obtained via comparison of the SOHO/LASCO, SOHO/EIT
observations and coronal magnetic field calculations (Wilcox Solar
Observatory). The values of the solar dipole vector components are
taken from the same calculations of the coronal magnetic field. The
strength of the heliospheric current sheet is obtained via analyses
of the interplanetary magnetic field preliminary data from the
ACE spacecraft. This model is better applicable during the solar
cycle minimum. However, the obtained model polar magnetic field is
in agreement with the observations near the solar maximum, when the
polar plumes could be visible over the magnetic (and not heliographic)
poles of the Sun if the magnetic dipole is perpendicular to the line
of sight. The configuration of the solar corona during the August 11,
1999 total solar eclipse expected from our analysis does not contain
polar plumes and will be close to the maximal-shape corona dominated
by coronal rays and streamers.

---------------------------------------------------------
Title: Total eclipses : science, observations, myths, and legends
Authors: Guillermier, Pierre; Koutchmy, Serge
1999teso.conf.....G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Fine structure of the Solar Chromosphere: Arch-Shaped Mottles
Authors: Zachariadis, Th. G.; Georgakilas, A. A.; Koutchmy, S.;
Alissandrakis, C. E.; Dara, H. C.
1999SoPh..184...77Z Altcode:
We analyze a time series of high resolution observations near the solar
limb, obtained in Hα and the Mg b1 line. We identified arch-shaped dark
mottles, which are thin, faint Hα structures observable under very
good seeing conditions, best seen in Hα +0.75 Å. Their mean length
is about 15”, their mean height about 6” and indicative lifetimes
is of the order of 5 min. They show negative (away from the observer)
line-of-sight velocities. A possible interpretation is that material
flows from the apex towards the feet of the arches.

---------------------------------------------------------
Title: SOPHIE: a solar EUV multilayer reflecting coronagraph
Authors: Hassler, Donald M.; Slater, David C.; Smartt, Raymond N.;
Koutchmy, Serge L.
1998SPIE.3443...61H Altcode:
SOPHIE (Solar Photometric Helium Imaging Experiment) is a design for
a new space-borne EUV multi-layer reflecting coronagraph to obtain
full coronal field-of-view (solar disk and 1.1 to 3.0 solar radii
above the limb) observations in He II 304 angstrom, and to measure the
coronal helium abundance as a function of structure and time in the
corona. Knowledge of the coronal helium abundance is fundamental to
understanding the dynamics of the solar wind acceleration region, yet
its value is not well known. SOPHIE will open up a new observational
domain by providing full field-of-view coronagraph observations of
helium, as opposed to electrons observed with traditional white light
coronagraphs. Moreover, it has been recognized in the last several
years that time variable phenomena is important and relevant to every
aspect of the transition region and corona.

---------------------------------------------------------
Title: High Resolution Analysis of the Eclipse Solar Corona
Authors: Koutchmy, S.
1998jena.conf...13K Altcode:
A very large W-L coronal flux is made available during total
eclipses. High speed analysis of very fine-scale structure of the
magnetically dominated solar atmosphere is made possible, including
the deeply seeded sources of the solar mass loss. Additional
observations of both the disk and of the more outer corona should
be simultaneusly collected from space, using the SOHO and the Yohkoh
missions to complements the data. The most optimum eclipse studies
should concentrate on the intermediate corona where acceleration
processes are taking place. MHD waves, including magneto-acoustic
propagating waves and standing loop-resonance waves are everywhere
present with rather short periods. W-L fine imaging at high signal-to
noise ratio is needed to avoid the overlapping problem and measure
their magnitude. Ubiquituos plasmoid like objects are also produced
in this region near the temperature maximum and they need a special
attention. They are rather privileged site where both the radiation
cooling and the magnetic dissipation mechanisms are occurring. Eclipses
are good opportunities to look at the dynamics of coronal ejections. At larger scale, sharp edges of streamers and plumes can be used
to deduce a 3-D view of the corona neutral sheets, provided pictures
taken at several hours interval are made available along the path of
the totality. Both the quasi-rigid rotation and the more subtle outward
motions of coronal material are then evidenced, giving a good tool to
study the origin of the slow wind.

---------------------------------------------------------
Title: The prolate solar chromosphere
Authors: Auchere, F.; Boulade, S.; Koutchmy, S.; Smartt, R. N.;
Delaboudiniere, J. P.; Georgakilas, A.; Gurman, J. B.; Artzner, G. E.
1998A&A...336L..57A Altcode:
We present a comparative analysis of the chromospheric solar
limb prolateness, using strictly simultaneous H_alpha ground-based
observations and Heriptsize{II} space-based observations. The typical
prolateness is found to be Delta D/D=5.5*E(-3) in Heriptsize{II}
and 1.2*E(-3) in H_alpha . The first measurements in the 30.4 nm
Heriptsize{II} line over a period of two years, as well as coronal
data, are discussed to explore further the origin of the prolateness
and its possible consequences.

---------------------------------------------------------
Title: Advances in ground-based and space-based reflecting coronagraph
designs
Authors: Smartt, Raymond N.; Koutchmy, Serge L.
1998SPIE.3352..614S Altcode:
A program to develop ground-based emission-line solar coronagraphs
based on super-polished primary objective mirrors has been underway at
the National Solar Observatory/Sacramento Peak over the last several
years. The fundamental design requirements for effective coronagraph
performance are discussed. The instrument currently under development
has a 60-cm diameter objective with a 700-cm primary focal length. This
design has been refined with an emphasis on achieving an extremely
low level of instrumental stray light, suitable for both visible
and IR operation and for carrying out high-precision polarimetry. It
is seen as a possible prototype for a new generation of much larger
aperture, low-scattered-light solar telescopes. Special applications
include measurements of the signatures of waves in coronal loops,
transient events such as coronal loop interactions, the spatial
variation of magnetic fields in prominences allowing computation of
electric currents, and the determination of the magnitude of coronal
magnetic fields. For applications in space, a white-light reflecting
coronagraph has been developed under the USAF program, SWATH (Space
Weather and Terrestrial Hazards). This novel catadiopric design has a
10-cm diameter superpolished primary objective mirror, and a unique
external occulter. It has a significantly higher throughput and
resolution as compared with conventional space-borne lens-objective
coronagraphs. Two basic modifications of this design are proposed
that result in an in-line symmetric configuration, with a decrease in
mass, while improving the scattered-light performance. Some special
applications are described.

---------------------------------------------------------
Title: Chromospheric heating by electric currents induced by
fluctuating magnetic elements
Authors: Lorrain, Paul; Koutchmy, Serge
1998SoPh..178...39L Altcode: 1998SoPh..178..477L
We refer to two papers by Goodman (1995, 1996) on the heating of
the chromosphere by large-scale electric currents, and to our paper
(Lorrain and Koutchmy, 1993) on magnetic elements. Goodman assumes
that the dynamo that runs a magnetic element stops operating at t =
0. From then on, the magnetic field decays exponentially, and the
induced currents heat the chromosphere. The time constants calculated
by Goodman disagree with the observed values, possibly because he
disregards the driving dynamo. Also, he assumes static conditions,
but his magnetic force density appears suddenly when the dynamo stops,
and it is about equal to the gravitational force density. The magnetic
force acts downward and fluctuations in the current flowing through
the magnetic element should induce vertical oscillations at the
photosphere. This point should be investigated further.

---------------------------------------------------------
Title: Cor-I: a coronal white-light imager for a solar probe
Authors: Vial, J. -C.; Koutchmy, S.; Habbal, S. R.
1998AdSpR..21..291V Altcode:
Solar and heliospheric observations acquired over several decades,
have shown that the corona is a highly structured medium. There is
no doubt that these structures reflect the response of the coronal
plasma - confined by the highly inhomogeneous magnetic field - to
different forms of energy input. While in-situ plasma measurements
have provided the characteristic properties of both fast and slow
solar winds, they have fallen short in connecting them to the source
regions of the wind. A near-Sun flyby mission offers an unprecedented
opportunity to explore the solar wind at distances much closer to
the Sun than ever achieved before. However, it is essential that
in-situ measurements be coordinated with simultaneous imaging of
the structures encountered in the corona. We present the concept and
design of a white-light imager called Cor-I, as a key instrument for a
near-Sun flyby mission which makes it possible to distinguish spatial
structures from temporal changes in the plasma parameters. With the
inference of the electron density from the Thomson scattered emission,
white-light measurements are also a very powerful tool for quantitative
studies of the acceleration region of the solar wind. In addition, the
proposed instrument carries the potential for discovery of transient
events and waves in these parts of the acceleration region of fast and
slow solar winds that are inaccessible to in-situ plasma instruments.

---------------------------------------------------------
Title: A Model of Plasma Sheets in Equilibrium
Authors: Koutchmy, S.; Molodensky, M.; Vibert, D.
1998ASPC..150..127K Altcode: 1998IAUCo.167..127K; 1998npsp.conf..127K
No abstract at ADS

---------------------------------------------------------
Title: Corona of the polar regions
Authors: Starkova, L.; Molodensky, M.; Kouvitsky, Vi.; Koutchmy, S.
1998ESASP.421..317S Altcode: 1998sjcp.conf..317S
No abstract at ADS

---------------------------------------------------------
Title: Solar plume formation in the solar corona
Authors: Veselovsky, I. S.; Panassenko, O. A.; Koutchmy, S.
1998ESASP.421..345V Altcode: 1998sjcp.conf..345V
No abstract at ADS

---------------------------------------------------------
Title: The polar extension of the solar chromosphere
Authors: Auchère, F.; Delaboudinière, J. P.; Koutchmy, S.;
Boulade, S.
1998ESASP.421..245A Altcode: 1998sjcp.conf..245A
No abstract at ADS

---------------------------------------------------------
Title: About polar ejection events and surges
Authors: Loucif, M. L.; Koutchmy, S.; Stellmacher, G.; Georgakilas,
A.; Bocchialini, K.; Delaboudinière, J. -P.
1998ESASP.421..299L Altcode: 1998sjcp.conf..299L
No abstract at ADS

---------------------------------------------------------
Title: Wave Activity and Prominence Eruption
Authors: Baudin, F.; Bocchialini, K.; Delannee, C.; Koutchmy, S.;
Stellmacher, G.; Shibata, K.; Veselovsky, I. S.; Panasenko, O. A.;
Zhukov, A. N.
1998ASPC..150..314B Altcode: 1998IAUCo.167..314B; 1998npsp.conf..314B
No abstract at ADS

---------------------------------------------------------
Title: Coronal plasmoid dynamics. I. Dissipative MHD approach
Authors: Delannee, C.; Koutchmy, S.; Veselovsky, I. S.; Zhukov, A. N.
1998A&A...329.1111D Altcode:
Energy and momentum balance equations of the dissipative MHD approach
are applied to the coronal plasmoid phenomenon observed with the
Canada-France-Hawaii Telescope during the July 11, 1991 total solar
eclipse. The situation is marginal for the applicability of the MHD
description,which has been used for orders of magnitude estimates of the
governing physical parameters. Their analysis confirms the suggestion
about the possibility for a relatively cold but rapidly moving plasma
body to heat the corona through dissipative viscous effects. It also
shows that magnetic stresses, gas pressure gradients and viscous drags
by the fast plasma flows from the chromosphere are viable candidates
to lift the plasmoid against the gravity force.

---------------------------------------------------------
Title: Properties of Hα spicules from disk and limb high-resolution
observations
Authors: Dara, H. C.; Koutchmy, S.; Suematsu, Y.
1998ESASP.421..255D Altcode: 1998sjcp.conf..255D
No abstract at ADS

---------------------------------------------------------
Title: SXR Coronal Polar Jets and Recurrent Flashes
Authors: Koutchmy, S.; Hara, H.; Shibata, K.; Suematsu, Y.; Reardon, K.
1998ASSL..229...87K Altcode: 1998opaf.conf...87K
No abstract at ADS

---------------------------------------------------------
Title: Foreword
Authors: Koutchmy, S.; Martens, P.; Shibata, K.
1998ESASP.421...14K Altcode: 1998sjcp.conf...14K
No abstract at ADS

---------------------------------------------------------
Title: Time domain analysis of polar plumes observed with LASCO-C2
and EIT
Authors: Llebaria, A.; Lamy, P.; Deforest, Ce.; Koutchmy, S.
1998ESASP.421...87L Altcode: 1998sjcp.conf...87L
No abstract at ADS

---------------------------------------------------------
Title: Spicules and Macrospicules: Simultaneous Hα and He II (304
Å) Observations
Authors: Georgakilas, A. A.; Dara, H.; Zachariadis, Th.; Alissandrakis,
C. E.; Koutchmy, S.; Delannée, C.; Delaboudinière, J. -P.; Hochedez,
J. -F.
1998ASPC..155..376G Altcode: 1998sasp.conf..376G
No abstract at ADS

---------------------------------------------------------
Title: Coronal Plasmoid Dynamics
Authors: Delannee, C.; Koutchmy, S.; Zhukov, A.; Veselovsky, I.
1998ASPC..150..388D Altcode: 1998npsp.conf..388D; 1998IAUCo.167..388D
No abstract at ADS

---------------------------------------------------------
Title: White-light polar plumes from solar eclipses
Authors: Koutchmy, S.; Bocchialini, K.
1998ESASP.421...51K Altcode: 1998sjcp.conf...51K
No abstract at ADS

---------------------------------------------------------
Title: European Plans for the Solar/Heliospheric Stereo Mission
Authors: Bothmer, V.; Bougeret, J. -L.; Cargill, P.; Davila, J.;
Delaboudiniere, J. -P.; Harrison, R.; Koutchmy, S.; Liewer, P.;
Maltby, P.; Rust, D.; Schwenn, R.
1998ESASP.417..145B Altcode: 1998cesh.conf..145B
No abstract at ADS

---------------------------------------------------------
Title: Coronal jet turbulent activity to explain distorted emission
line
Authors: Loucif, M. L.; Ben Jaffel, L.; Koutchmy, S.; Vial, J. -C.
1998ESASP.421..303L Altcode: 1998sjcp.conf..303L
No abstract at ADS

---------------------------------------------------------
Title: Polar jets and plasmoids:Results from JOP 57
Authors: Delannee, C.; Koutchmy, S.; Delaboudiniere, J. -P.; Hochedez,
J. -F.; Vial, J. -C.; Dara, H.; Georgakilas, A.
1998ESASP.421..129D Altcode: 1998sjcp.conf..129D
No abstract at ADS

---------------------------------------------------------
Title: Kinematics of Hα spicules from near-limb observations.
Authors: Zachariadis, T. G.; Georgakilas, A. A.; Dara, H. C.;
Alissandrakis, C. E.; Koutchmy, S.
1998joso.proc..126Z Altcode:
The authors have studied the behavior of dark mottles near the solar
limb. After the corrections for flat field and limb darkening the
authors can identify spicules crossing the solar limb. Most of the
mottles initially show an ascending velocity which gradually turns
to descending. Moreover, the authors observe a group of dark mottles
which have the shape of arches. One of the footpoints of the arch is
in a chromospheric network cell, while the other in a nearby rosette.

---------------------------------------------------------
Title: Flashing Mgb1 bright points.
Authors: Dara, H. C.; Georgakilas, A.; Zachariadis, T.; Alissandrakis,
C.; Koutchmy, S.
1998joso.proc..124D Altcode:
High resolution observations, obtained at the Sacramento Peak
Observatory near the solar limb, are analysed for the study of
the evolution of Mgb1 (5183.22 Å) bright points, as well as their
association to bright features in the continuum (5256.40 Å) and Hα
wings (±0.75 Å). The authors have detected stable bright points from
the beginning to the end of the time series which hardly move and
whose shape undergoes small changes, bright points whose brightness
increases and decreases periodically, and bright points which suddenly
appear and disappear within one or two minutes.

---------------------------------------------------------
Title: La mission SoHO vers un nouveau Soleil?
Authors: Baudin, F.; Koutchmy, S.
1997LAstr.111..286B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The heliospheric layer and the coronal structure on November
3, 1994
Authors: Koutchmy, S.; Molodenskii, M. M.; Starkova, L. I.; Kutvitskii,
V. A.; Ershov, A. V.; Ivanov, A. A.; Petrov, B. B.; Sidorov, C. C.
1997AstL...23..818K Altcode: 1997PAZh...23..939K
No abstract at ADS

---------------------------------------------------------
Title: Granulation and magnetism in the solar atmosphere.
Authors: Baudin, F.; Molowny-Horas, R.; Koutchmy, S.
1997A&A...326..842B Altcode:
The properties of the photosphere in magnetic and non magnetic
regions, at two levels in the solar atmosphere, have been studied,
using two virtually simultaneous time sequences of 109 mn duration
of CCD images taken at the Vacuum Tower Telescope of the Sacramento
Peak Observatory. The selected wavelengths correspond to the true
continuum and to the wing of the MgIb_1_ line, where brightenings
are taken as proxies of magnetic elements. Averaged intensities,
intensity fluctuations and horizontal motions in different regions
and levels of the photosphere have been compared. We obtained various
results concerning: the intensities inside and outside an active region
showing different behaviours; the granulation keeping a kind of remnant
structure at the continuum level; the mapping of proper motions of the
granules imaged in the continuum outlining clearly the super-granular
cells in the deepest layers of the photosphere; the “freezing”
influence of the magnetic field on these motions in active regions;
and the temporal variation of the correlation between images at the
two heights indicating that intensity variations at the higher level
precede those of the lower one. These results are briefly discussed
and compared with previous ones and with published model calculations.

---------------------------------------------------------
Title: Fine Structure of the solar atmosphere from near-limb
observations in three wavelengths
Authors: Georgakilas, A. A.; Dara, H.; Zachariadis, Th.; Alissandrakis,
C. E.; Koutchmy, S.
1997SoPh..172..133G Altcode: 1997ESPM....8..133G
We analyze a time series of high-resolution observations near the
limb, in the continuum, in the Mg b1 line (-0.4 Å off
line center), and in the wings of Hα (+0.75 Å). The observations
were obtained with a CCD camera at the Vacuum Tower telescope of
the Sacramento Peak Observatory. We study the association of facular
points, as they appear at different heights of the solar atmosphere
(continuum, b1 - 0.4 Å, Hα + 0.75 Å) with the feet of
fine dark mottles.

---------------------------------------------------------
Title: SXR Coronal Flashes.
Authors: Koutchmy, S.; Hara, H.; Suematsu, Y.; Reardon, K.
1997A&A...320L..33K Altcode:
We provide evidence for the existence of a new type of soft X-ray
(SXR) brightening event that we call coronal flashes. The phenomenon
was observed on deep time series taken with the SXT of Yohkoh in the
north polar coronal hole, near the sunspot minimum. Events last as
short as 1.5 mn and the corresponding SXR flux span the range of
energies, from single pixel brightenings corresponding to fluxes
of about 10^24^erg but barely surpassing the level of the noise,
to higher and more smeared multiple px brightenings still orders
of magnitude smaller than the known small SXR bright points and/or
transient brightenings. The typical occurrence rate of flashes is
1-event/arcmin^2^/5mn with a 1/2mn integration time. At least part of
the coronal flashes are recurrent and some of them could be associated
with a SXR jet; it is not clear what is their optical counterpart.

---------------------------------------------------------
Title: Eclipse WL polar plumes: what is the connection with the
disk activity?
Authors: Koutchmy, Serge; Bocchialini, Karine
1997AIPC..385..137K Altcode: 1997recs.conf..137K
We discuss both the origin and the role that eclipse WL-polar plumes
could have in the context of the coronal hole physics: densities,
temperatures and flows. Some new results coming from the campaigns of
the 1994 and 95 eclipses are reported and YOHKOH data are also taken
into account.

---------------------------------------------------------
Title: Distribution on halfwidths for the green coronal line
(5303 Å).
Authors: Alexeeva, I. V.; Kim, I. S.; Matsuura, O. T.; Picazzio, E.;
Koutchmy, S.
1997ASIC..494....7A Altcode: 1997topr.conf....7A
Distribution on halfwidths for Fe XIV (5303 Å) coronal line is
analyzed. The Fabry-Perot interferogram obtained during the total
solar eclipse of November 3, 1994 is used. The profiles not distorted
by the white light corona contributions as well as by ghost images
were selected. A multimodality with probability of 87% is found in the
histogram. Average values of halfwidths differ for different coronal
structures (0.91 Å for SW-helmet, 0.85 Å for NW and 0.81 Å for SE
coronal regions). An evident increase of the halfwidths with distance
is revealed for SW-helmet structure.

---------------------------------------------------------
Title: Polar Jets and Plasmoids: Preliminary Results from JOP 57
Authors: Delannée, C.; Koutchmy, S.; Delaboudiniè, J. -P.; Hochedez,
J. -F.; Vial, J. -C.; Dara, H.; Georgakilas, A.
1997ESASP.404..327D Altcode: 1997cswn.conf..327D
No abstract at ADS

---------------------------------------------------------
Title: Characterisation of Polar Plumes from LASCO-C2 Images in
Early 1996
Authors: Lamy, P.; Liebaria, A.; Koutchmy, S.; Reynet, P.; Molodensky,
M.; Howard, R.; Schwenn, R.; Simnett, G.
1997ESASP.404..487L Altcode: 1997cswn.conf..487L
No abstract at ADS

---------------------------------------------------------
Title: Coronal physics inferred from the analysis of fine structures.
Authors: Koutchmy, S.
1997ASIC..494...39K Altcode: 1997topr.conf...39K
Solar total eclipses are rare occasions offering the opportunity to make
a snapshot of the solar corona. The availability of a large radiative
flux makes sophisticated methods usefull to analyse all parts of the
highly structured white-light corona. Coronal absolute intensities
and line emissions, including their polarization, are also studied to
analyse density and temperature inhomogeneities, velocities and magnetic
fields. Detailed density distribution is directly extracted for fine
coronal structures. During the July 11, 1991 eclipse, the large 3.6 m
aperture CFH optical telescope was used to analyse time sequences over
small coronal fields and to image the finest structures never seen;
results from this experiment are presented with emphasis on small-scale
dynamical plasma processes including wave-phenomena. Finally, the
author gives an overview of what is known on coronal structures from
eclipse observations: temperatures, densities, velocities, occurrence
and structure of streamers, coronal holes, threads, etc.

---------------------------------------------------------
Title: Analysis of a High Latitude Slow CME with Travelling Ejecta
Authors: Boulade, S.; Delanné, C.; Koutchmy, S.; Lamy, P.; Llebaria,
A.; Howard, R.; Schwenn, R.; Simnett, G.
1997ESASP.404..217B Altcode: 1997cswn.conf..217B
No abstract at ADS

---------------------------------------------------------
Title: Mais où est passé le nouveau cycle d'activité solaire?
Authors: Koutchmy, S.
1997LAstr.111....4K Altcode:
Depuis plus d'un an les astrophysiciens solaires du monde entier
analysent les magnétogrammes du soleil pour détecter les signes
annonciateurs du nouveau cycle d'activité du Soleil, cycle qui portera
le numéro 23.

---------------------------------------------------------
Title: Degree polarization distribution in the solar corona of 03
November 1994.
Authors: Belenko, I. A.; Bougaenko, O. I.; Kim, I. S.; Koutchmy, S.;
Matsuura, O. T.; Picazzio, E.
1997ASIC..494...15B Altcode: 1997topr.conf...15B
Preliminary data reduction of the color index polarization
wave experiment carried out in Brazil (Chapeco town) is
described. Distributions of polarization degree (polarization images)
in the range 1.1 - 1.6 Rsun are obtained by an algorithm
developed on the basis of the Stokes vector presentation and IDL
software. The polarization image of the "quasi-white-light" corona
(summary of the blue and red spectral region emissions) is analyzed. On
the average, no fit is found with the van de Hulst model for the inner
corona at heliographic latitudes of ±45°. The polarization degree
reaches a plateau at 1.2 - 1.35 Rsun.

---------------------------------------------------------
Title: High frequency magneto-acoustic waves in the chromosphere
Authors: Bocchialini, Karine; Koutchmy, Serge
1997AIPC..385..153B Altcode: 1997recs.conf..153B
From a time series taken over the disk center network and cell
elements in different chromospheric and photospheric lines, we discuss
the possible detection of wave-trains corresponding to frequencies
higher than the 7 mHz frequency of the familiar chromospheric 3 mn
oscillations. Their analysis would greatly benefit from observations
taken with an improved spatial resolution, free of seeing effects
which limit the precision in ground-based measurements.

---------------------------------------------------------
Title: The three-dimensional structure of the corona on November
3, 1994
Authors: Molodenskii, M. M.; Starkova, L. I.; Koutchmy, S.; Ershov,
A. V.
1996ARep...40..848M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The polarization and 3-D structure of the corona on 11.3.94
Authors: Koutchmy, S.; Molodenskii, M. M.; Starkova, L. I.; Kutvitskii,
V. A.; Ershov, A. V.
1996R&QE...39..921K Altcode:
We present the results of observations of the white-light corona in
polarized light (Criciuma, Brazil) in 1994. The space location of
the surface Br=0 is calculated using the synoptic map
of filaments during the solar eclipse. A good agreement was found
between the corona ray structure and the surface folds and pleats,
which result from its projection onto the sky plane. The measured
polarization degree is compared with calculations by the Van de Hulst
model. A conclusion is made concerning the adequacy between the proposed
model and the observation data.

---------------------------------------------------------
Title: MHD Shock Interactions in Coronal Structures
Authors: Grib, S. A.; Koutchmy, S.; Sazonova, V. N.
1996SoPh..169..151G Altcode:
We consider the magnetohydrodynamic (MHD) interactions of solar coronal
fast shock waves of flare and/or nonflare origin with the boundaries
of coronal streamers and coronal holes. Boundaries are treated as MHD
tangential discontinuities (TD). Different parameters of the observed
corona are used in the investigation. The general case of the oblique
interaction is studied.

---------------------------------------------------------
Title: Propagating magneto-acoustic waves in the solar chromosphere.
Authors: Baudin, F.; Bocchialini, K.; Koutchmy, S.
1996A&A...314L...9B Altcode:
We report on spectroscopic one dimensional observations showing for
the first time upward propagating 5mn period waves, which emerge from
the deep chromospheric network. Wavetrains are well measured at the
height where the He I line (at A=1083nm) is formed by the coronal
back radiation. We also present results from a time series of narrow
filtergrams of a quiet region at the disk center. The two dimensional
mapping of the power of waves observed in the chrormosphere shows the
familiar cell-like distribution corresponding to the network magnetic
field pattern. In addition, Fourier components with significantly
longer periods than 5mn were detected in the chromospheric network. We
suggest that the waves propagating in the open corona are reminescent
of photospheric oscillations transmitted by the magnetic field of the
chromospheric network.

---------------------------------------------------------
Title: White-Light Coronal Dark Threads and Density Fine Structure
Authors: November, Laurence J.; Koutchmy, Serge
1996ApJ...466..512N Altcode:
High spatial resolution white-light coronal observations from the
eclipse of 1991 July 11 taken with the 3.6 m Canada-France-Hawaii
Telescope on Mauna Kea are the best ever achieved because of the
unique opportunity of observing the totally eclipsed Sun with a large
aperture telescope. Photometric calibration of the photographic data is
verified by the average radial intensity variation, which agrees with
the classical function. Dividing out the average radial variation, we
identify relatively dark and bright fine "threads" with enhanced spatial
power in the range of 1-5 Mm. Spatial filtering using unsharp masking
or "mad-max" algorithms clearly shows relatively dark and bright radial
threads in loops as fine as the resolution limit of about 1 Mm. The main
feature is an arcade of concentric dark and bright threads that extend
above a small prominence just above the limb. A small coronal cavity
near the prominence contains numerous fine dark threads. The relative
electron-density depletion and enhancement required to explain the
observed thread contrast, assuming that they are isolated cylindrically
symmetric structures, is found to be ΔNe/Ne
∼ ± 100%, indicating that the dark threads are fully evacuated. An
excess of approximately 1 G field strength in stationary non-force-free
magnetic fields can produce the observed thread contrast. Evacuated
threads representing non-force-free magnetic fields introduce special
constraints on the coronal thermodynamics.

---------------------------------------------------------
Title: Two Dynamical Models for Solar Spicules
Authors: Lorrain, Paul; Koutchmy, Serge
1996SoPh..165..115L Altcode:
Solar spicules are luminous jets that erupt up to 10 000 km from the
surface of the Sun and have diameters, all along their length, of
only about 150-200 km. We first review some recent observations made
at the Hα wavelength. According to our models, a solar spicule is a
self-channelled proton beam emitted by a magnetic element and surrounded
by a cold sheath. The beam originates in a self-excited dynamo that
exploits a v × B field and that could be situated either below or above
the element, where v is the local plasma velocity and B is the local
magnetic flux density. In falling back, the sheath provides a return
current of protons that cancels the outgoing current. We discuss the
channelling of charged-particle beams of very large cross-section and
propose velocity channelling, which is apparently a new concept. We
assume a steady state and a hydrogen plasma.

---------------------------------------------------------
Title: L'ère SoHO a commencé.
Authors: Baudin, F.; Koutchmy, S.
1996JAF....53...10B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A coronal optical imager for a solar probe
Authors: Lamy, P.; Koutchmy, S.
1996AdSpR..17c..95L Altcode: 1996AdSpR..17...95L
A Coronal Optical Imager (COI) can make a significant contribution
to a solar probe, for instance, by detecting the faintest plasma and
magnetic structures, by analyzing the He/H ratio and the cool plasma
component and by observing possible sources of dust near the Sun. We
describe an instrument which combines the capability of EUV, UV and
visible imaging as well as visible polarimetry, and propose two versions
respectively adapted to a spinning and a 3-axis stabilized probes.

---------------------------------------------------------
Title: 3-D Structure of Heliospheric Current Sheet Deduced from
Eclipse Observations
Authors: Molodensky, Michael M.; Starkova, Lidia I.; Koutchmy, Serge
L.; Ershov, Andre V.
1996ASPC...95..385M Altcode: 1996sdit.conf..385M
No abstract at ADS

---------------------------------------------------------
Title: A coronal plasmoid crossing a magnetic structure.
Authors: Delannee, C.; Koutchmy, S.
1996CRASB.322...79D Altcode:
The authors observed, during the solar eclipse in 1991, a coronal
plasmoid. They analyzed the trajectory, the dynamic and radiative flux
variation of the plasmoid. The motion is upward and decelerated. The
flux presents a strong decrease. The plasmoid appears to go across a
structure, which is supposed to follow the local magnetic field. It
travels across the magnetic field line; this is not in agreement with
the theory of the "melon seed" acceleration and additional forces are
needed to explain the motion.

---------------------------------------------------------
Title: On the three-dimensional structure of the solar corona
Authors: Koutchmy, S.; Ershov, A. V.; Molodenskii, M. M.
1996ARep...40..109K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: 1995: une éclipse en Indochine.
Authors: Koutchmy, S.
1995LAstr.109..340K Altcode:
Solar eclipse 1995 October 24 in Indochina.

---------------------------------------------------------
Title: Chromospheric Oscillations from Simultaneous Sequences of
HEL 1083 and Call K 393.4 Spectroscopic Measurements
Authors: Bocchialini, K.; Koutchmy, S.
1995ESASP.376b.499B Altcode: 1995help.confP.499B; 1995soho....2..499B
No abstract at ADS

---------------------------------------------------------
Title: The Space-Time Structure of the Upper Solar Atmosphere
Authors: Koutchmy, S.; Veselovsky, I. S.
1995ESASP.376b.475K Altcode: 1995soho....2..475K; 1995help.confP.475K
No abstract at ADS

---------------------------------------------------------
Title: Nonlinear MHD interactions in some solar coronal structures
Authors: Grib, S. A.; Koutchmy, S.; Sazonova, V. N.
1995sowi.conf...60G Altcode:
The magnetohydrodynamic (MHD) interactions of solar coronal fast shock
waves of flare and/or nonflare origin with the boundaries of such
structures like the streamer and the coronal hole are considered. These
boundaries are treated as MHD tangential discontinuities (TD). Different
parameters of the observed corona are used. The general case of oblique
interaction is studied. It is shown that a fast shock wave is usually
refracted as a fast shock wave inside the coronal streamer. But for
a special case of the velocity shear across a TD a slow shock wave
may be generated. On the contrary the shock wave is refracted inside
the coronal hole, indeed as a slow shock wave. The significance of
different effects due to the interaction of fast and slow shock waves
with the coronal magnetic field is noticed, especially at the time
of coronal mass ejection (CME). Thus slow shock waves may help to
'open' the coronal magnetic field, and fast shock waves - to 'close'
it. It is also shown, that an oblique fast MHD coronal shock wave may
trigger an instability at the boundary of a streamer considered as
a TD. It might have a relation with the observed abrupt process of
disappearance of the streamer's boundary in the solar corona.

---------------------------------------------------------
Title: L'éclipse totale de Soleil du 3 novembre 1994 sur les Andes
chiliennes.
Authors: Koutchmy, S.; Zimmermann, J. -P.
1995LAstr.109..110K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Special Session - Waves on the Extended Transition-region
and Loops
Authors: Koutchmy, S.
1995ESASP.376a.233K Altcode: 1995heli.conf..233K
No abstract at ADS

---------------------------------------------------------
Title: Equilibrium and stability of axially symmetrical plasma
configurations in the Sun's atmosphere.
Authors: Koutchmy, S. L.; Koutchmy, O. K.; Kutvitskij, V. A.;
Molodenskij, M. M.; Solovev, L. S.
1995BRASP..59.1570K Altcode:
On the basis of a unified approach the authors consider the conditions
of the MHD equilibrium and stability of a number of axially symmetrical
plasma configurations responsible for typical formations in the Sun's
atmosphere, such as coronal helmets and loops, and also a new object,
i.e., the coronal plasmoid observed 11 July 1991 during the solar
eclipse.

---------------------------------------------------------
Title: Near-Infrared Coronagraphic Detection of Space Debris
Authors: Neidig, D. F.; Smartt, R. N.; Kim, I. S.; Koutchmy, S.
1995itsa.conf..253N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: White-Light Coronal Fine Structure
Authors: November, L. J.; Koutchmy, S.
1995itsa.conf...37N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Advanced Coronagraphy
Authors: Koutchmy, S.
1995itsa.conf....1K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Mirror Coronagraphic Device and Its Application
Authors: Kim, I. S.; Bougaenko, O. I.; Brouevitch, V. V.; Koutchmy,
S.; Neidig, D. F.; Smartt, R. N.; Evseev, O. A.
1995itsa.conf..239K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the 3-D Structure of the November 3, 1994 Eclipse Corona
Authors: Koutchmy, S.; Molodensky, M.; Starkova, L.; Ershov, A.;
Matsuura, O.
1995pist.conf...60K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Reflecting Coronagraphs: Prospects
Authors: Smartt, R. N.; Koutchmy, S.
1995itsa.conf..163S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Detection of a Dual "Disparition Brusque" at Pic-Du-Midi
Authors: Niot, J. M.; Noëns, J. C.; Romeuf, D.; Koutchmy, S.
1995itsa.conf..247N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Wave Properties of the Chromosphere in He I 1083 nm and CA II K
Authors: Bocchialini, K.; Baudin, F.; Koutchmy, S.
1995itsa.conf..423B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Pic du Midi observations of dual `disparition brusque'
Authors: Koutchmy, S.; Noëns, J. C.
1994ESASP.373...91K Altcode: 1994soho....3...91K
No abstract at ADS

---------------------------------------------------------
Title: About small plasmoids propagating in the solar corona
Authors: Koutchmy, S.; Bouchard, O.; Grib, S.; November, L.; Vial,
J. -C.; Gouttebrone, P.; Koutvitsky, V.; Molodensky, M.; Solov'iev,
L.; Veselovsky, I.
1994ESASP.373..139K Altcode: 1994soho....3..139K
No abstract at ADS

---------------------------------------------------------
Title: White-Light Coronal Fine Structure
Authors: November, L. J.; Koutchmy, S.
1994AAS...185.9204N Altcode: 1994BAAS...26.1472N
No abstract at ADS

---------------------------------------------------------
Title: Fast coronal transient (CME) with twisted legs
Authors: Airapetian, V. S.; Koutchmy, S.
1994ESASP.373..195A Altcode: 1994soho....3..195A
No abstract at ADS

---------------------------------------------------------
Title: On the three-dimensional structure of coronal rays
Authors: Koutchmy, S.; Molodenskii, M. M.; Vial, J. -C.
1994ARep...38..822K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Magnetic configuration of coronal streamers and threads
Authors: Koutchmy, S.; Koutvitsky, V. A.; Molodensky, M. M.; Solov'iev,
L. S.; Koutchmy, O.
1994SSRv...70..283K Altcode:
We give a short account of the most prominent structures of the
intermediate corona. Then we propose an axially symmetrical model for
coronal streamers, according to which charged particles move along
magnetic surfaces whose sources are electrical currents situated in
the vicinity of the photosphere. The simplest current configuration
is a pair of coaxial, coplanar, circular, and oppositely directed
currents parallel to the photosphere. Magnetic surfaces for this current
distribution exhibit a helmet-shaped separatrix and a saddle point. The
temperature profile along the streamer can be predicted qualitatively
if one takes into account the conservation of an adiabatic invariant
in the drift theory of the charged particle motion.

---------------------------------------------------------
Title: The Chromospheric network dynamics as derived from the analysis
of CA II K and He I 1083 NM lines
Authors: Bocchialini, S.; Vial, J. -C.; Koutchmy, S.
1994SSRv...70...57B Altcode:
We present results of line profile analysis of observations
simultaneously performed around the Ca II K and He I (1083 nm) lines,
using the Horizontal Spectrograph of the Vacuum Tower Telescope of
NSO/SP. From the spectral analysis of a 83 min long sequence of CCD
spectra, we derive some dynamical properties of the main components
of the quiet chromosphere: i) the magnetic network, ii) the cell
interior. We present a whole set of amplitude spectra near 5 and 3
min periods for the two lines; K3 and He I velocity spectra
extending up to 100 mHz are also considered, for the first time.

---------------------------------------------------------
Title: On the Visible Shape of the Cold Plasma Jets in the Solar
Chromosphere
Authors: Veselovsky, I. S.; Triskova, L.; Koutchmy, S.
1994SoPh..153..237V Altcode:
Lines of equal optical thickness are calculated for cold plasma jets
propagating in the simplest magnetic configuration. The paraxial
approximation is used in the case of jets directed along the axis of a
magnetic dipole. The results explain the apparently convergent as well
as divergent shapes of the jets in a divergent magnetic configuration.

---------------------------------------------------------
Title: Moon-based UV reflecting coronagraph
Authors: Vial, J. C.; Koutchmy, S.; Smartt, R. N.
1994AdSpR..14f..43V Altcode: 1994AdSpR..14...43V
UV observations of the solar disc, and above the limb, have evidenced
a wide range of possible diagnostics, especially in the Lα line. On
the disc, Lα traces the magnetic (sometimes unexpected) structuring of
the top of the atmosphere; out from the limb, it allows measurement of
radial velocities up to a few solar radii where most optical techniques
fail. Other diagnostics include the kinematics of ejections (e.g. CMEs,
but also small-scale rapidly evolving plasmoïds). We propose a
dual-channel reflecting coronagraph combining relatively-high angular
resolution (0.2-0.4”) with large spatial (2.5 solar radii from Sun
center) and temporal coverage. The advantages offered by a Moon-based
instrument are discussed.

---------------------------------------------------------
Title: Magnetic configurations of ray structures of the solar corona
Authors: Koutchmy, S.; Kutvitskii, V. A.; Molodenskii, M. M.; Solov'ev,
L. S.
1994ARep...38..417K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Coronal physics from eclipse observations
Authors: Koutchmy, S.
1994AdSpR..14d..29K Altcode: 1994AdSpR..14...29K
Solar total eclipses are rare occasions offering the opportunity to
make a snapshot of the solar corona. Thanks to the availability of
a large radiative flux in the optical region, sophisticated methods
can be used from the ground to analyse all parts of the highly
structured white-light corona. Coronal absolute intensities and line
emissions, including their polarization, are also studied to analyse
density and temperature inhomogeneities, velocities and magnetic
fields. Detailed density distribution is directly extracted from fine
coronal structures. During the July 11, 1991 eclipse, the large 3.6m
aperture CFH optical telescope was used to analyse time sequences over
small coronal fields and to image the finest structures; results from
this experiment are presented with emphasis on small-scale dynamical
plasma processes with possible inclusion of wave-phenomena. Finally,
to prepare the SOHO mission on coronal physics, we give an overview of
what is known on coronal structures from eclipse observations of the
past solar cycles: temperatures, densities, velocities, occurence and
structure of streamers, coronal holes, threads, overall variability. associated with the Pierre et Marie Curie University of Paris VI,
France

---------------------------------------------------------
Title: Dynamical Properties of the Chromosphere In and Out of the
Solar Magnetic Network
Authors: Bocchialini, Karine; Vial, Jean-Claude; Koutchmy, Serge
1994ApJ...423L..67B Altcode:
We present the results of a comparative analysis of an 83 minute
time sequence of spectra taken around the Ca II and He I 1083 lines,
near the center of the solar disk and away from active regions. We
discuss the behavior of the Fourier spectra at low frequency: 3
minute oscillations are well observed out of the network, and 5 minute
oscillation waves are prominent in the network. The 5 s sampling time
also permits the observation of the high-frequency part of the Fourier
spectra of intensity and velocity fluctuations at different heights. At
high frequencies, K2V-K2R and 1083 (velocity)
results differ when magnetic and non-magnetic regions are compared.

---------------------------------------------------------
Title: Very High Resolution Analysis of the Dynamics of a Coronal
Plasmoid
Authors: Bouchard, O.; Koutchmy, S.; November, L.; Vial, J. -C.;
Zirker, J. B.
1994scs..conf..593B Altcode: 1994IAUCo.144..593B
The authors present the results of the analysis of a movie taken over a
small field of view in the intermediate corona at a spatial resolution
of 0.5", a temporal resolution of 1 s and a spectral passband of 7
nm. These CCD observations were made at the prime focus of the 3.6 m
aperture CFHT telescope during the 1991 total solar eclipse.

---------------------------------------------------------
Title: Near-IR Solar Coronal Observations with New-Technology
Reflecting Coronagraplis
Authors: Smartt, R. N.; Koutchmy, S.; Noens, J. -C.
1994IAUS..154..603S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the Optical Polarization of the White-Light Coronal
Structures
Authors: Filippov, B. P.; Molodensky, M. M.; Koutchmy, S.
1994scs..conf..601F Altcode: 1994IAUCo.144..601F
A special experiment was designed to measure the orientation of the
polarization plane in the solar corona during the total eclipse of
July 11, 1991. Rotating polaroids with the axes directed at +45° and
at -45° of the radial direction in all directions were used. The
polarization plane was found to be tangential to the solar limb
everywhere with an accuracy within 1°.

---------------------------------------------------------
Title: The IR Contrast of Magnetic Elements Obtained from High
Spatial Resolution Observations at 1.6 MU M
Authors: Darvann, T. A.; Koutchmy, S.
1994IAUS..154..483D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On Sunspot and Facular Contrast Variations Near 2 MU M and
4 MU M
Authors: Kotov, V. A.; Koutchmy, S.
1994IAUS..154..265K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A Method to Obtain Stereo-Diagrams of the Solar Disc
Authors: Molodensky, M. M.; Starkova, L.; Koutchmy, S.
1994scs..conf..605M Altcode: 1994IAUCo.144..605M
In order to obtain a 3D picture of the Solar disc planoconvex spherical
and elliptical lenses were made by the authors using organic glass. The
comparison between the effects produced by the lenses and the results
of the calculation have shown that the elliptical lenses give the
best results.

---------------------------------------------------------
Title: Wave Properties in the Upper Chromosphere and at the Base of
the Corona
Authors: Bocchialini, K.; Vial, J. -C.; Koutchmy, S.
1994scs..conf..123B Altcode: 1994IAUCo.144..123B
From a 83 min long sequence of observations of Ca II K and He I (1083
nm) line profiles, some dynamical properties of the main components
of the quiet upper chromosphere are derived: for both the magnetic
network and the internetwork, amplitude and phase spectra of the
Doppler velocities are presented.

---------------------------------------------------------
Title: Analysis of Chromospheric Proxies of Coronal Bright Points
Authors: Bocchialini, K.; Vial, J. -C.; Koutchmy, S.; Zirker, J. B.
1994ASPC...68..389B Altcode: 1994sare.conf..389B
No abstract at ADS

---------------------------------------------------------
Title: On the 3D Solar Corona Structure
Authors: Koutchmy, S.; Molodensky, M. M.; Vial, J. -C.
1994scs..conf..585K Altcode: 1994IAUCo.144..585K
The authors consider the 3D structure of the solar corona using
eclipse observations. They use a pseudostereoscopic effect of the
rigidly rotating corona to determine the true position of the main
coronal structures: broad threads, rays and streamers. An example of
stereo-view deduced from a simple analysis of results coming from the
1991 eclipse is given. The authors conclude that large helmet streamers
are composed by the pleats of the heliosphere current sheet projected
on the plane of the sky.

---------------------------------------------------------
Title: The Infrared Granulation - Observations
Authors: Koutchmy, S.
1994IAUS..154..239K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: CFHT eclipse observation of the very fine-scale solar corona
Authors: Koutchmy, S.; Belmahdi, M.; Coulter, R. L.; Demoulin, P.;
Gaizauskas, V.; MacQueen, R. M.; Monnet, G.; Mouette, J.; Noens,
J. C.; November, L. J.
1994A&A...281..249K Altcode:
At the July 11, 1991 solar total eclipse, a modern large optical
telescope, Canada-France-Hawaii telescope (CFHT), was used to
probe the solar corona. The best possible pictures were obtained
with the CFHT, using fast imaging techniques and post-facto image
selection and processing. Several cameras were run during totality
to acquire sub-arcsec spatial resolution white-light images, with
both narrow-band and broad-band filters. The setup and the observing
procedure are described. Preliminary results, together with an
evaluation of the merits of the experiment, are given, as well as a
sample of images. Fine-scale coronal features were observed for the
first time in a time series, confirming the importance of plasmoid-like
activity in the inner corona. The observation of the smallest coronal
feature ever reported is analyzed, giving a typical cross-section of
0.4 +/- 0.1 arcsec. On a larger scale, dark loops around a foreground
prominence are resolved for the first time, suggesting that sheet-like
voids exist above a filament channel.

---------------------------------------------------------
Title: IR Observations of the K and F Corona During the 1991 Eclipse
Authors: Kuhn, J. R.; Lin, H.; Lamy, P.; Koutchmy, S.; Smartt, R. N.
1994IAUS..154..185K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Magnetic structures of the intermediate corona
Authors: Koutchmy, S.; Molodensky, M.
1994LNP...432..167K Altcode: 1994LNPM...11..167K
The fine structures of the corona are analyzed using SXR and W-L
eclipse pictures. The measurement of the finest features observed at
the CFHT on July 11, 1991 is discussed. We call the attention to the
3-D aspect of the magnetic structure which can be apprehended and
analysed assuming the plasma is concentrated in thin curved sheets
observed on eclipse W-L pictures. More geometrical parameters can
be deduced from the stereo-view based on the hypothesis of a rigid
rotation. A preliminary 2.5-D model calculation is put forward to
explain the active region coronal rays. It is based on the assumption
of ad hoc chromospheric current distribution and analytic calculations.

---------------------------------------------------------
Title: Magnetic Structures of the Intermediate Corona
Authors: Koutchmy, S.; Molodensky, M. M.; Koutvitsky, V.; Solov'ev,
L. S.
1994scs..conf...55K Altcode: 1994IAUCo.144...55K
The fine structures of the corona are analyzed using SXR and WL eclipse
pictures. The measurement of the finest features observed at the CFHT
on July 11, 1991 is discussed. A preliminary 2.5D model calculation
is put forward to explain the active region coronal rays.

---------------------------------------------------------
Title: on the Three-Dimensional Structure of Coronal Rays
Authors: Koutchmy, S.; Molodenskii, M. M.; Vial, J. C.
1994AZh....71..925K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Magnetic Field of a Bipolar Sunspot Region in the
Photosphere and the Chromosphere
Authors: Dara, H. C.; Koutchmy, S.; Alissandrakis, C. E.
1994emsp.conf...61D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Analysis of the Chromospheric Proxies of Coronal Bright Points
- Preliminary Results
Authors: Bocchialini, K.; Koutchmy, S.; Vial, J. -C.; Zirker, J. B.
1994emsp.conf..173B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Chromospheric Faculae as Filaments Feet?
Authors: Koutchmy, S.; Stellmacher, G.
1994emsp.conf...91K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Solar eclipses.
Authors: Koutchmy, S.
1994oga..book...81K Altcode:
Contents: 1. Introduction. 2.Circumstances of
eclipses. 3. Observation of the event. 4. Inner Coronal photography and
photometry. 5. Photographing the K, or plasma, corona. 6. Photography of
the outer corona. 7. Spectroscopic study of the corona. 8. Conclusions.

---------------------------------------------------------
Title: Toward High-Spatial Resolution IR Solar Observations
Authors: Koutchmy, S.; Restaino, S.
1993rtpf.conf..171K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Finest White-Light Coronal Features
Authors: Koutchmy, S.; Bouchard, O.; Mouette, J.; Koutchmy, O.
1993rtpf.conf..147K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Finest White-Light Coronal Features
Authors: Koutchmy, Serge; Bouchard, Olivier; Mouette, Jean; Koutchmy,
Olga
1993SoPh..148..169K Altcode:
An attempt to detect the finest white-light coronal features
observed with a large optical telescope was made at the July 11,
1991 Solar Total Eclipse. A few selected results taken from the
video-CCD high speed observations obtained at the prime focus of the
Canada-France-Hawaï-Telescope (CFHT) with a red coronal interference
filter are presented. The smallest (sub-arsec) detected and/or resolved
coronal features are shown. The methods that were used to extract
them from the noisy and seeing-limited images taken from video frames
are described.

---------------------------------------------------------
Title: Photospheric and chromospheric magnetic field structure of
a bipolar sunspot region
Authors: Dara, H. C.; Koutchmy, S.; Alissandrakis, C. E.
1993A&A...277..648D Altcode:
We present high resolution magnetograms of a large split spot and an
opposite polarity pore in the 6102.7 Å Ca I photospheric line and in
Hα and we discuss their fine structure. We found important differences
between the photospheric and chromospheric magnetic field. Although
the large spot was apparently unipolar at the photospheric level, we
detected an opposite polarity region at the chromospheric level. We
also found that there was hardly any trace of the pore magnetic field
in the Hα magnetogram. These results cannot be interpreted in terms
of constant-α magnetic fields. Finally we confirm the occurrence
of filamentary magnetic structures in Hα at the location of the
superpenumbra of the large spot.

---------------------------------------------------------
Title: Measuring the polarization of the solar corona
Authors: Koutchmy, S.; Molodenskii, M. M.; Nikol'Skii, G. M.; Filippov,
B. P.
1993ARep...37..286K Altcode: 1993SvA....37..286K
No abstract at ADS

---------------------------------------------------------
Title: Photospheric electric currents in solar magnetic elements
Authors: Lorrain, P.; Koutchmy, S.
1993A&A...269..518L Altcode:
In order to explain recent high-resolution magnetogram and filtergram
observations, we propose a self-excited dynamo model for the magnetic
elements, or network patches, that occur in the high photosphere
of the sun at the periphery of supergranules. We assume that an
element is a magnetic flux tube that stands more or less vertically
and that results from the presence of azimuthal electric currents,
and we describe a mechanism that could generate these currents. As a
first approximation, we assume that the electric current density is
uniform. This model accounts for the existence of magnetic elements,
for their stability, for the existence of neighboring fields of opposite
polarity, and for their mutual attraction and repulsion. The power
dissipation associated with the azimuthal currents accounts for only a
small part of the observed radiation in the low photosphere, so that
other explanations for the brilliance will have to be considered. We
also propose a more realistic but more elaborate model in which the
azimuthal electric current distribution is not uniform.

---------------------------------------------------------
Title: Toward High Spatial Resolution Infrared Solar Observations
Authors: Koutchmy, Serge; Restaino, Sergio R.
1992SoPh..142..359K Altcode:
To achieve high spatial resolution capability for IR solar observations,
we suggest the use of a special mask placed before the entrance
aperture of large conventional optical telescopes. Such a mask would
match well the resolution of a non-redundant array and would provide
safe operation of a large telescope used for solar observations. The
proposed solution has the additional advantage of relatively low cost
because already-existing optical telescopes are used.

---------------------------------------------------------
Title: Three-dimensional image of the solar corona from white-light
observations of the 1991 eclipse
Authors: Koutchmy, Serge; Molodenskii, Mikhail M.
1992Natur.360..717K Altcode:
THE structure of the solar corona is believed to be governed by the
solar magnetic field induced by currents at the surface of the Sun
and perhaps within the corona itself1. Inhomogeneities
in the corona are well known from radially compensated
eclipse images2 in white light or coronal emission
lines3. We have used two whitelight images taken
about three hours apart by the Multi-station International Coronal
Experiment4 during the July 1991 total eclipse in an attempt
to deduce directly the three-dimensional structure of the corona. We
observed prominent coronal structures, including broad threads, rays
and streamers, and used them to calibrate a model based on solid-body
rotation and bulk coronal outflow. The errors in the reconstruction
method are small enough to give us confidence that quasi-rigid rotation
is a reasonable approximation over these timescales. We illustrate
the deduced coronal structure by means of a stereogram.

---------------------------------------------------------
Title: Coronal photometry and analysis of the eclipse corona of July
22, 1990
Authors: Koutchmy, S.; Altrock, R. C.; Darvann, T. A.; Dzubenko,
N. I.; Henry, T. W.; Kim, I.; Koutchmy, O.; Martinez, P.; Nitschelm,
C.; Rubo, G. A.
1992A&AS...96..169K Altcode:
Results are presented of aircraft-based observations and ground
observations from multiple stations, made during the July 1990
eclipse. The main results of the analysis of the large-scale features of
the inner corona concern the measurement of the flattening index of the
near-maximum-activity corona; the occurrence of a large coronal hole;
and the importance of the line emissions recorded on the broadband
white-light pictures, due to the presence of numerous large or faint
prominences all around the limb.

---------------------------------------------------------
Title: Photoelectric analysis of the solar granulation in IR
Authors: Koutchmy, Serge
1992STIN...9318334K Altcode:
Results of both image analysis and statistical analysis of 1D
scans the IR granulation observed in the opacity minimum region
are briefly presented. The same technique was applied at 600 nm
and results partially presented by Koutchmy and Lebecq, 1986,
Astron. Astrophys. 169, 323. All observations were collected at
the prime focus of the Sac Peak VTT using high signal-to-noise ratio
measurements with a specially-designed pinhole PbS spectro-photometer;
imaging has been made using both 2D scanning of the telescope and
processed video-scans of an IR-vidicon. Images of the IR granulation
and of sunspot umbral dots and penumbral filaments are present for
the first time.

---------------------------------------------------------
Title: Streamer eclipse observations.
Authors: Koutchmy, Serge
1992ESASP.348...73K Altcode: 1992cscl.work...73K
During the 1991 eclipse, the large 3.6 m aperture CFH optical telescope
was used to analyse time sequences over small coronal fields and to
reach the finest structure; results from this experiment are presented
including the analysis of the faintest detected feature and small-scale
dynamical plasma processes. To prepare the SOHO mission on coronal
physics, an overview of what is known on coronal structures from eclipse
observations of the past solar cycles is given. The non-potential nature
of the coronal magnetic field is well illustrated by the large deviation
of streamers from the radial direction as well as by the systematic
occurence of tangential discontinuities at edges of streamers.

---------------------------------------------------------
Title: No Evidence of a Circumsolar Dust Ring from Infrared
Observations of the 1991 Solar Eclipse
Authors: Lamy, P.; Kuhn, J. R.; Lin, H.; Koutchmy, S.; Smartt, R. N.
1992Sci...257.1377L Altcode:
During the past 25 years there have been many attempts to detect a
possible dust ring around the sun, with contradictory results. Before
the 1991 eclipse, infrared eclipse experiments used single-element
detectors to scan the corona along the ecliptic for excess surface
brightness peaks. The availability of relatively large-format infrared
array detectors now provides a considerable observational advantage:
two-dimensional mapping of the brightness and polarization of the corona
with high photometric precision. The 1991 eclipse path included the
high-altitude Mauna Kea Observatory, a further advantage to measure the
corona out to large angular distances from the sun. Results are reported
from an experiment conducted on Mauna Kea with a HgCdTe-array detector
sensitive to wavelengths between 1 and 2.5 micrometers, using broad-band
J, H, and K filters. Although the sky conditions were not ideal, the H-
and K-band surface brightnesses clearly show the inhomogeneous structure
in the K-corona and the elliptical flattening of the F-corona, but no
evidence of a circumsolar, local dust component out to 15 solar radii.

---------------------------------------------------------
Title: Coronal Streamers
Authors: Koutchmy, Serge; Livshits, Moissei
1992SSRv...61..393K Altcode:
The general significance of streamers of the solar corona is discussed
in the frame of our knowledge of the solar wind phenomenon and the
large-scale solar magnetic structure. Thermodynamical and geometric
parameters of streamers observed and measured at total solar eclipses
are reviewed. Both the low part (in the form of a helmet with a cusp)
and the external part (in the form of a stalk extended at many solar
radii) are considered. The modelling of streamers starts with the
analysis of effects produced by the solar wind flow on a magnetic
structure. Facts and arguments are presented in favor of a model
with a current sheet and reconnection processes going on along the
axis of the streamer, especially in the non-collisional part of the
radially extended streamer. Further development of the Pneuman and
Kopp (1971) model is discussed, including difficulties occurring
in the interpretation of a stationary solution. An empirical model
satisfying observations is presented. Future researchs on streamers
were discussed with emphasis on observations to be done with the
space-borne coronagraphs on the SOHO spacecraft.

---------------------------------------------------------
Title: Structural changes in the solar corona during the July
1991 eclipse
Authors: Zirker, J. B.; Koutchmy, S.; Nitschelm, C.; Stellmacher, G.;
Zimmermann, J. P.; Martinez, P.; Kim, I.; Dzyubenko, N.; Kurochka,
L.; Makarov, V.
1992A&A...258L...1Z Altcode:
Preliminary results of the analysis of radially filtered pictures
obtained at several hours interval during the July 11, 1991 total
solar eclipse are given. Instrumental parameters and method are
outlined. Structural changes are discussed.

---------------------------------------------------------
Title: Evidence of plasmoid ejection in the corona from 1991 eclipse
observations with the Canada-France-Hawaii telescope
Authors: Vial, J. -C.; Koutchmy, S.; Monnet, G.; Sovka, J.; Clark,
C.; Salmon, D.; Purves, N.; Sydserff, P.; Coulder, R.; November, L.
1992ESASP.344...87V Altcode: 1992spai.rept...87V
Observations of the solar corona with a large telescope at high
altitude was fully exploited with the 3.60 m CFHT (Canada France
Hawaii Telescope) in Hawaii, during the 11 Jul. 1991 eclipse,
are reported. Different instruments set up for the eclipse and
preliminary results are given. The moving feature in the corona is
focused upon. Physical conditions in this plasmoid and its origins
are discussed. One of the four cameras installed in the primary focus
was a video charge coupled device camera with a red filter at 637
nm selecting the red line. The power of the telescope allowed for a
good signal in a pixel as small as 0.12 arcsec and a very good time
resolution. The spectral resolution as measured at the Moon limb
was better than one arcsec. During the three minute long sequence,
6000 video images were obtained. Among the fine structures recorded,
a plasmoid about 1500 km wide was seen to ascend and dilute in the
corona. Possible emission mechanisms are discussed. It was found that
both low and relatively high temperature plasmas can be confined in this
ejected plasmoid. Such a small scale phenomenon could be important for
the heating of the corona and should be observed in UV emission lines
in a wide range of temperatures. The high spatial resolution achieved
by Solar Interferometric Mission for Ultrahigh Resolution Imaging and
Spectroscopy (SIMURIS) allows to study the shape, stability and the
diagnostics of such plasmoids in the corona.

---------------------------------------------------------
Title: Development of Reflecting Coronagraphs
Authors: Smartt, R. N.; Koutchmy, S.
1992ASPC...26..660S Altcode: 1992csss....7..660S
No abstract at ADS

---------------------------------------------------------
Title: The solar corona of July 11, 1991. Observations in Brazil
(MICE).
Authors: Dzyubenko, N. I.; Kurochka, L. N.; Rubo, G. A.; Kim,
I. S.; Artamonov, B. P.; Boczko, R.; Matsuura, O. T.; Koutchmy, S.;
Zimmermann, J. P.; Zirker, J. B.
1992ATsir1552...21D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Eclipse Totale de Soleil du 11 Juillet 1991
Authors: Koutchmy, S.
1992BCFHT..26....2K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Observations of the solar corona on July 22, 1990. The
structure and the identification.
Authors: Dzyubenko, N. I.; Ivanchuk, V. I.; Rubo, G. A.; Koutchmy, S.
1991BSolD..11...98D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Observations of total solar eclipses in the stratosphere.
Authors: Koutchmy, S.
1991ZemVs...5...33K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Multicolor Continuum Analysis of the Solar Granulation in
Quiet and Active Regions
Authors: Keller, C. U.; Koutchmy, S.
1991ApJ...379..751K Altcode:
A set of narrow-band filtergrams of the solar photosphere recorded in
three widely separated true continuum windows and in Mg I b1 with a
spatial resolution of about 0.5 arcsec is analyzed. The influence of
small-scale magnetic fields on the granulation is studied by comparing
various statistical parameters in selected active and quiet regions,
and the temperature stratification of faculae at the level of continuum
formation is investigated. In active regions there exist more points
with enhanced continuum intensity as compared with quiet regions, and
there is more power at small spatial scales in active regions, whereas
more power exists at large scales in quiet regions. Quiet regions
near and far away from a large sunspot do not show any significant
difference. It is concluded that changes in the granular pattern near
sunspots are caused by the small-scale magnetic fields often found near
sunspots. Faculae, identified by their brightness in the Mg I b1 wing,
show an enhanced continuum intensity and a reduced ratio between the
blue and the red continuum, which is consistent with current flux
tube models.

---------------------------------------------------------
Title: Study of small scale magnetic flux and the corresponding
velocity pattern
Authors: Alissandrakis, C. E.; Dara, H. C.; Koutchmy, S.
1991A&A...249..533A Altcode:
Two-dimensional maps of the longitudinal magnetic field and the
line of sight velocity of two small-scale magnetic regions in
the quiet sun, using a one-hour time sequence of filtergrams in
the magnetically sensitive lambda 6103 A CaI line (with circular
polarization measurements) obtained with the Sacramento Peak Vacuum
Tower Telescope and the universal filter, are calculated. After the
elimination of the effect of the 5-minute photospheric oscillations,
downflows smaller than 300 m/s are found in both magnetic regions. The
magnetic field intensity and the velocity are weakly correlated:
high values of the magnetic field tend to occur in regions of small
negative velocities. The magnetic field intensity increased during
the observations, while some magnetic peaks moved with respect to
others. The difference of the magnetic field intensity measured in
the blue and the red wing indicates a line asymmetry; this asymmetry
was found to be independent of the line of sight velocity.

---------------------------------------------------------
Title: Eclipse Plans for NSO/SP
Authors: Zirker, J. B.; Koutchmy, S.; Coulter, R. L.; November, L. J.;
Smartt, R. N.
1991BAAS...23.1063Z Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Small scale magnetic field mapping with high temporal
resolution.
Authors: Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S.
1991sopo.work..257D Altcode:
Two dimensional maps of the longitudinal magnetic field can be readily
calculated for small-scale magnetic regions. Here the authors use
an one-hour time sequence of high spatial resolution (0.75 arc sec)
filtergrams, obtained at the Sacramento Peak Vacuum Tower Telescope with
the universal filter (UBF) in the wings of the magnetically sensitive
λ 6103 Ca I line. The time difference between two magnetic maps is
32 sec. The measurements of the magnetic field in the blue wing are
about 40% higher than in the red wing.

---------------------------------------------------------
Title: High spatial resolution V-Stokes polarimetry to measure the
Zeeman effect in flux tubes and prominence filament threads.
Authors: Koutchmy, S.; Zirker, J. B.; Darvann, T.; Koutchmy, O.;
Stauffer, F.; Mann, R.; Coulter, R.; Hegwer, S.
1991sopo.work..263K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Coronal activity.
Authors: Koutchmy, Serge; Zirker, Jack B.; Steinolfson, Richard S.;
Zhugzhda, Iosif D.
1991sia..book.1044K Altcode:
This chapter considers the rather extended, very inhomogeneous and
dynamical part of the solar atmosphere called the corona. Coronal
structures are first described from the point of view of quasi-static
structure in order to consider their thermodynamical gross properties,
including heating and magnetic fields. The solar-cycle-related
variations of coronal structures are reviewed as well. Solar prominences
are a well-observed ingredient of the corona; they form its cool
component. Their properties, including magnetic field, thermal and
velocity field structures are reviewed before considering the problem of
their formation. Coronal mass ejections are the most dramatic phenomena
occurring in a short time in the corona and are almost inevitably
phenomena occurring in a short time in the corona and are almost
inevitably related to a prominence ejection. Their observations are
described with reference to several related solar phenomena in order
to understand the driving mechanism. Models of coronal mass ejections
are described based on numerical simulations including consideration
of waves. Finally, the very important and still open question of the
waves in the solar corona is briefly discussed from a theoretical
point of view, emphasizing the possible role of hydromagnetic waves.

---------------------------------------------------------
Title: Properties of Impulsive Events in a Polar Coronal Hole (With
6 Figures)
Authors: Koutchmy, S.; Loucif, M. L.
1991mcch.conf..152K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Future Observations of the F-Corona with the LASCO Coronagraph
Space Experiment
Authors: Lamy, P. L.; Llebaria, A.; Maucherat, A.; Koutchmy, S.;
Giovane, F.
1991ASSL..173..191L Altcode: 1991IAUCo.126..191L; 1991oeid.conf..191L
No abstract at ADS

---------------------------------------------------------
Title: High spatial resolution observations of magnetic flux elements.
Authors: Koutchmy, S.
1991sopo.work..237K Altcode:
The author shortly reviews works done at the VTT of SPO during
the last 15 years, on both high spatial resolution spectroscopy
using polarization analysis and magnetography with a polarization
modulator inside the UBF. Respective merits and noticeable results
are discussed. The author stresses the importance of using high-speed
measurements to track the magnetic signal and avoid losses due to image
motion; the efficiency in improving the resolution using the 2-D Wiener
filtering is also demonstrated. Subarcsec resolution magnetic maps are
discussed, to show not only the dominant-polarity magnetic-elements,
but also the mixed minor-polarity and the weak field outside.

---------------------------------------------------------
Title: Prominence Fine Structure - Part Two - Diagnostics
Authors: Zirker, J. B.; Koutchmy, S.
1991SoPh..131..107Z Altcode:
A random-clustering model of prominence fine-structure has been applied
to observations of prominence Hα spectra. The model yields an estimate
of the number of unresolved elements that form an individual resolved
feature, and sets limits on their velocity and Hα profile dispersions.

---------------------------------------------------------
Title: L'Observatoire Solaire de Sacramento Peak
Authors: Koutchmy, S.
1990LAstr.104..395K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Observation de la couronne dans la stratosphére.
Authors: Koutchmy, Serge
1990LAstr.104..385K Altcode:
Reasons for conducting solar-eclipse observations from the stratosphere
are discussed. Stratospheric observations of the total solar eclipse
of July 22, 1990 from a specially equipped Falcon 20 are described. A
visualization of the corona of the 1990 eclipse is presented.

---------------------------------------------------------
Title: UV solar reflecting coronagraph
Authors: Smartt, R. N.; Koutchmy, S.; Vial, J. C.
1990AIPC..207..578S Altcode: 1990am...proc..578S
A dual-channel reflecting coronagraph is proposed that would provide
observations of Lα corona and chromosphere, upper transition-region
phenomena in CIV, and also helioseismology observations in the continuum
around 166 nm. Each channel would use a 104×104-UV-sensitive CCD
array. The combined velocity and magnetic field data would link
events in the chromosphere, the transition region and the corona to
an elongation of about 2.5 R0. These data would be used to study both
the global-scale and also the fine-scale properties of the corona in
terms of the physical processes that deposit energy and momentum in the
corona. Specific question to be investigated would be the origin and
morphology of CME's and other coronal transients, sources of coronal
heating, and the source(s) and dynamics of the coronal wind in the
inner coronal region.

---------------------------------------------------------
Title: Erratum: Velocity Pattern of Small Scale Magnetic Fields
Authors: Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S.
1990SoPh..128..431D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Real-time image processing and data handling for ground-based
and spaceborne coronal observations
Authors: Koutchmy, S.; Colley, S.; Smartt, R.; Nitschelm, C.;
Zimmermann, J. P.
1990SPIE.1235..849K Altcode:
Ground-based observations of the solar corona, as well as deep
night-time observations close to bright objects, are degraded by
highly variable aureole effects produced by the earth's atmosphere,
even when the stationary background pattern of both atmospheric and
instrumental origin is removed using detectors and special processing
techniques. First observations using an objective mirror advanced
coronagraph reveal that small particles (both continental and maritime
aerosols) imaged on the focal plane as they cross the field of view
can dominate the background unter clear-sky conditions, producting a
considerable noise background that it is not easily removed. Suggestions
are made to reduce to noise of this "dynamical aureole". The authors
also discuss the possibility of optically detecting orbital space
debris of small size, using either an externally-occulted space-borne
mirror coronagraph or a large-aperture ground-based mirror coronagraph,
and the corresponding detection system requirements.

---------------------------------------------------------
Title: New technology mirror coronagraph with extended applications
Authors: Smartt, Raymond N.; Koutchmy, Serge L.; Colley, Stephen A.;
Caron, R.; Schwenn, Rainer; Restaino, Sergio R.
1990SPIE.1236..206S Altcode:
General design considerations of objective-mirror coronagraphs are
presented. A 1-m-focal-length prototype reflecting coronagraph based on
a 5.5-cm aperture spherical superpolished silicon mirror objective is
described. The design is simple off-axis reflection from the objective
to a conventional coronagraph optical system (occulting disk, field
lens, Lyot stop, and imaging system). This instrument has produced the
first images of the emission corona using a ground-based reflecting
coronagraph. A second prototype instrument based on a 15-cm aperture
superpolished fused-silica mirror is also described.

---------------------------------------------------------
Title: The magnetic-field polarity of quiescent prominences
Authors: Kim, I. S.; Klepikov, V. Y.; Koutchmy, S.; Stepanov, A. I.;
Stellmacher, G.
1990PAZh...16..545K Altcode:
A statistical analysis of magnetographic data on quiescent solar
prominences is presented. The existence of two different magnetic
field systems in quiescent prominences is suggested. The first system
is oriented opposite to the underlying photospheric field; the angle
between the long axis of the filament and the field direction is
equal to 15 deg and B-parallel equals 15-18 G. The polarities of the
second system and of the underlying photospheric field are the same,
B-parallel = 5-7 G.

---------------------------------------------------------
Title: Magnetic Field Polarity of Quiescent Prominences
Authors: Kim, I. S.; Klepikov, V. Y.; Koutchmy, S.; Stepanov, A. I.;
Stellmacher, G.
1990SvAL...16..234K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Prominence Fine Structure
Authors: Zirker, J. B.; Koutchmy, S.
1990SoPh..127..109Z Altcode:
The vertical fine structure in a quiescent prominence was modelled as an
assembly of very narrow, optically thin threads. Random clusterings of
the threads can account for the observed contrast and Hα line profiles
of the fine structures. In this picture, each structure consists of
a cluster of 7-20 elementary threads.

---------------------------------------------------------
Title: Velocity pattern of small scale magnetic fields
Authors: Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S.
1990SoPh..126..403D Altcode:
High resolution observations of horizontal proper motions, as well
as vertical Doppler velocities measured over two selected regions
of small scale magnetic elements show a coherent behaviour. In a
region with two opposite polarities, approching with a velocity of
0.4 km s-1, the material in between moves downwards with
a velocity of 0.10 to 0.45 km s-1; while in a region with
two peaks of the same polarity, moving apart with a velocity of 0.3 km
s-1, the material in between moves predominantly upwards,
with a velocity of up to 0.3 km s-1.

---------------------------------------------------------
Title: Video Magnetograms with Sub-Arcsecond Resolution
Authors: Koutchmy, S.; Stauffer, F.; Zirker, J.; Keil, S.; Mann, R.;
Coulter, R.; Hegwer, S.
1990BAAS...22..880K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Coming: 24 hour surveillance of the sun.
Authors: Koutchmy, S.; Vial, J. -C.
1990Rech...21...10K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Analysis of the Solar Granulation in the Opacity Minimum Region
Authors: Koutchmy, S.
1990IAUS..138...81K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Small Scale Motions Over Concentrated Magnetic Field Regions
of the Quiet Sun
Authors: Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S.
1990IAUS..138..153D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Estimation of the line of sight amplitude of the magnetic
field on threads of an active region prominence
Authors: Koutchmy, S.; Zirker, J. B.
1990LNP...363..242K Altcode: 1990IAUCo.117..242K; 1990doqp.coll..242K
No abstract at ADS

---------------------------------------------------------
Title: On the Spatial Distribution of Prominence Threads
Authors: Zirker, J. B.; Koutchmy, S.
1990LNP...363..237Z Altcode: 1990doqp.coll..237Z; 1990IAUCo.117..237Z
No abstract at ADS

---------------------------------------------------------
Title: A movie of small-scale Doppler velocities in a quiescent
prominence
Authors: Koutchmy, Serge; Zirker, Jack; Gilliam, Lou B.; Coulter,
Roy; Hegwer, Stephen; Mann, Richard; Stauffer, Fritz
1990LNP...363..240K Altcode: 1990doqp.coll..240K; 1990IAUCo.117..240K
A movie made of selected H off-band images of a typical Quiescent
Prominences has been produced with the optical printer of NSO-S.P. High
speed pictures were obtained with the UBF of the VTT on June 21, 1987
during 30 min of very good seeing, at a 20 sec cycling rate. Blue and
red wings images are made at plus and minus .040 nm from line center,
with a .022 nm passband. Original Pictures were enlarged to give an
effective field of view of 100 × 80 arcsec2. Negative to positive
superposition allows the mapping of strongly Doppler-shifted features
(± 20 km sec-1) on a grey scale. The prominence threads are mostly
discrete, allowing accurate measurement of proper motions. Typical
transverse velocities of proper motions of small knots moving
vertically downward are about 10 km sec-1 The movie also demonstrates
the turbulent behaviour of the prominence plasma. Large-scale motions
at lower transverse velocities are also clearly present.

---------------------------------------------------------
Title: High Resolution Analysis of Quiescent Prominences at National
Solar Observatory / Sacramento Peak Observatory
Authors: Darvann, Tron A.; Koutchmy, Serge; Stauffer, Fritz; Zirker,
Jack B.
1990LNP...363..239D Altcode: 1990doqp.coll..239D; 1990IAUCo.117..239D
We present preliminary results of several experiments carried out at
the National Solar Observatory / Sacramento Peak (NSO/SP) Vacuum Tower
Telescope (VTT) with the aim to resolve velocities and magnetic fields
of the fine scale structures of filaments and prominences.

---------------------------------------------------------
Title: Le Soleil 24 Heures Sur 24
Authors: Koutchmy, S.; Vial, J.
1990Rech..217...10K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: High Resolution Observations of Motions and Structure of
Prominence Threads
Authors: Zirker, J. B.; Koutchmy, S.
1990LNP...363..244Z Altcode: 1990doqp.coll..244Z; 1990IAUCo.117..244Z
H profiles and filtergrams were obtained of quiescent prominences at
the National Solar Observatory, Sunspot, NM, with spatial resolution
better than 1.6 arcseconds. The H profiles of individual threads are
often Gaussian, but may show marked asymmetries, particularly near
the prominence edges. Filtergrams, taken at ± 0.7 Å (± 30 km/sec)
in H (with a 0.18 Å passband) show high speed knots and threads
at the prominence edges, that persist with no perceptible change
for at least 10 minutes. This result implies plasma motions (along
essentially horizontal magnetic fields) over distances as large as
18000 km, i.e. much larger than typical thicknesses (5000 km) of H
filaments. These motions may be associated with thread formation or
decay, but continuous observations of this prominence over 6 hours
show that the large-scale form of the prominence remained unchanged.

---------------------------------------------------------
Title: An Automated Procedure for Measurement of Prominence Transverse
Velocities
Authors: Darvann, Tron Andre; Koutchmy, Serge; Zirker, Jack B.
1990LNP...363..267D Altcode: 1990doqp.coll..267D; 1990IAUCo.117..267D
A computer algorithm for measurment of transverse velocities (proper
motion) in prominences has been developed. We present the method and
examples of computed proper motion maps. The method is a modified
version of the local cross correlation technique previously applied to
granulation images (November 1986, Title et al 1987, November and Simon
1988, November 1988, Darvann 1988, Brandt et al 1988). Prominence images
show much steeper intensity gradients and a wider range of spatial
scales of fine structure than granulation images. Due to this we find
it necessary to replace the prominence images by an image showing the
intensity gradients (derivative of the intensity image). Furthermore,
in our algorithm we compute absolute differences instead of correlation
coefficients in order to reduce the influence of large scale intensity
gradients across a local window (Karud 1988). We have tested the method
on datasets obtained at the Vacuum Tower Telescope of NSO/SP. The
accuracy of the algorithm is seen to be ±0.3 pixels which, in our
data, corresponds to about 1/10 arcsec. Seeing effects are effectively
reduced by averaging N cross correlation functions formed from images
sampled t apart. We find that t = 120s gives the highest accuracy in
the proper motion measurement when applied to our data consisting
of quiescent prominences. The correlation coefficient between two
interlaced, independent proper motion maps is as high as 0.92 when
N=50. The size of the smallest structure for which a proper motion
velocity can be measured is limited by the size of the smallest local
window that can successfully be applied in the measurement. It needs
to be large enough to contain some high contrast structures, typically
4×4 arcsec in our data. Our algorithm is self-adaptive to the data in
the sense that the window size is changed automatically depending on
the presence of local high contrast structures. We conclude that the
method successfully produces prominence proper motion maps in addition
to being able to correlation track prominence images. Furthermore the
algorithm will be useful for destretching of prominence images before
producing Doppler-grams or carrying out oscillation studies at high
spatial resolution.

---------------------------------------------------------
Title: Comet P/Halley at a heliocentric preperihelion distance of
2.6 AU - Jet activity and properties of the dust coma
Authors: Lamy, P. L.; Malburet, P.; Llebaria, A.; Koutchmy, S.
1989A&A...222..316L Altcode:
This paper presents an in-depth analysis of a high-resolution
photograph of comet P/Halley obtained on September 12, 1985 when it
was a heliocentric distance of 2.6 AU preperihelion. The coma has a
diameter of 138,000 km and exhibits structures which are interpreted
as three jets, one best seen in the outer part of the coma extending
to 29000 km and the two others, in the inner part extending to about
7000 km. The integrated magnitude and radial profiles of the coma are
given showing that the comet does not follow the simple steady-state,
radial outflow model. By combining the photometric result with nearly
simultaneous ultraviolet and infrared observations, it is found that
the strong reddening in the ultraviolet gradually levels off in the
visible as the color becomes neutral at 2 microns and blue beyond 3
microns. A geometric albedo at zero phase angle of 0.04 is obtained,
as well as a dust production rate of 30 to 120 kgs.

---------------------------------------------------------
Title: High resolution photographic Stokes polarimetry of small
scale magnetic flux (poster)
Authors: Keller, C. U.; Koutchmy, S.
1989hsrs.conf..443K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Optimum filter and frame integration application to granulation
pictures
Authors: Koutchmy, O.; Koutchmy, S.
1989hsrs.conf..217K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: High resolution observations of the solar corona: why and how?
Authors: Koutchmy, S.; Smartt, R. N.
1989hsrs.conf..560K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Magnetic fields of solar prominences: strength and latitude
distribution.
Authors: Kim, I. S.; Klepikov, V. Yu.; Koutchmy, S.; Stepanov, A. I.;
Stellmacher, G.
1989BSolD..11...98K Altcode:
According to the data obtained by a Nikolsky-type magnetograph
during 1979 - 1986 there are two maxima in histograms
"occurrence-B∥": O - 21 G and 27 - 36 G. The probability of
the minimum between these maxima is equal to 82%. The first maximum may
be divided into three distributions with peaks at 8, 15 and 20 G. The
second maximum refers to active latitude prominences. The major part
of the data (80%) belongs to the pre-minimum and minimum epochs. For
this period the average latitude of prominence formation is less than
20°. The authors believe that the peak at 15 G characterizes the
critical field strength of prominence formation.

---------------------------------------------------------
Title: Ground-Based Mirror Coronograph: First Results
Authors: Smartt, R. N.; Koutchmy, S.; Schwenn, R.
1989BAAS...21..848S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: New Observations and Analysis of the Helium D3 Shell above
the Limb
Authors: Avrett, E. H.; Koutchmy, S.
1989BAAS...21..828A Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Image processing of coronal pictures
Authors: Smartt, Raymond N.; Koutchmy, Olga; Koutchmy, Serge;
Nitschelm, Christian; Sykora, Julius
1989STIN...8924252S Altcode:
Coronal images contain many complex, superposed, faint, optically-thin
structures: rays, loops, curved streamers, etc. The spatial resolution
is often limited by the signal/noise ratio in the recording medium while
the dynamic range in intensity is severely dominated by the radial
gradient. The results obtained with a new simple image processing
algorithm are applied to several typical eclipse and coronographic
pictures. This 2D filter (second order difference operator in
k-direction) shows superior quality by improving the signal/noise ratio,
reducing the dynamic range and enhancing faint coronal structures. A
comparison with results obtained with more commonly used 2D filters is
also presented. The algorithm used here are briefly described, together
with discussions of enhanced coronal images of coronal physics interest.

---------------------------------------------------------
Title: On the Spatial Distribution of Prominence Threads
Authors: Zirker, J. B.; Koutchmy, S.
1989HvaOB..13...41Z Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Photoelectric Analysis of the Solar Granulation in the Infrared
Authors: Koutchmy, S.
1989ASIC..263..347K Altcode: 1989ssg..conf..347K
No abstract at ADS

---------------------------------------------------------
Title: Granulation In and Out of Magnetic Regions
Authors: Koutchmy, S.
1989ASIC..263..253K Altcode: 1989ssg..conf..253K
No abstract at ADS

---------------------------------------------------------
Title: An Automated Procedure for Measurement of Prominence Transverse
Velocities
Authors: Darvann, T. A.; Koutchmy, S.; Zirker, J. B.
1989HvaOB..13..243D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Prominence fine structure.
Authors: Zirker, J. B.; Koutchmy, S.
1989BAAS...21.1027Z Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Solar cycle variations of coronal structures
Authors: Loucif, M. L.; Koutchmy, S.
1989A&AS...77...45L Altcode:
Using eclipse pictures of the solar corona, properly scaled
drawings have been prepared to constitute a short atlas of coronal
structures. These drawings have been used to extract 2 parameters
which are further considered with respect to the sunspot number and the
sunspot cycle: the extension of polar regions free of coronal streamers
and the average radial deviation of large streamers. The flattening
index deduced from the photometric analysis of a larger number of
eclipse pictures is also considered. The out-of-phase behavior of
several coronal parameters is confirmed. The results are discussed in
the light of the analysis of the green-line activity as observed during
30 years at the Pic du Midi Observatory. The N-S asymmetric behavior
of the activity in different solar hemispheres and the occurrence of
a powerful secondary maximum of coronal activity are discussed.

---------------------------------------------------------
Title: On variation of prominence heights with the solar cycle.
Authors: Kim, I. S.; Klepikov, V. Yu.; Koutchmy, S.; Stepanov, A. I.;
Stellmacher, G.
1988BSolD...5...77K Altcode:
The behaviour of prominence heights with the solar cycle is
studied. Prominence pictures taken by the Nikolsky magnetograph in
1979 - 1986 are used. A dependence of the average height with time
is analysed. The minimum height took place in the fall of 1984, 2
years before the solar activity minimum. Histograms of "prominence
occurrence versus height" were constructed for different phases of
the solar cycle. It is pointed out that the behaviour of the average
prominence height depends on the variation of the distribution of
prominence heights with the solar cycle. The minimum height is due to
a relative increase of the number of prominences which is less than
25 arcsec. The occurrence of these prominences has a peak before the
minimum of solar activity. Such prominences are predominantly located
at the latitudes 0 - 20°.

---------------------------------------------------------
Title: Optical Detection of Space Debris Using a Large Achromatic
Coronograph
Authors: Koutchmy, S.; Nitschelm, C.
1988Ap&SS.143...45K Altcode:
The space debris detectin will become greater and greater in the near
future with the space debris enhancing. We introduce a theoretical
approach of this problem assuming the using of a new generation large
coronograph. We get some interesting — and alarming — results
about the great probability to be able to observe space debris with
this new ground-based large coronograph.

---------------------------------------------------------
Title: Spectroscopic Coronal Observations Using A High-Sensitivity
Camera
Authors: Smartt, R. N.; Colley, S. A.; Gilliam, L. B.; Koutchmy, S.;
Zirker, J. B.
1988BAAS...20..704S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Space-borne coronagraphy
Authors: Koutchmy, Serge
1988SSRv...47...95K Altcode:
We consider the main aspects of a rather delicate discipline,
space-borne coronagraphy, which is essentially performed with
white-light, externally-occulted coronagraphs. Methods of observation
and recent results are presented in a scientific section; a short
account of historical rocket-borne and balloon-borne experiments is
also given. The review concentrates on both the NRL-type coronagraphs
and the HAO-type coronagraphs, stressing the essential features and
merits of numerous experiments which were flown. A small section is
devoted to other designs. A large number of figures, including many
drawings, are used to illustrate the growing complexity of experiments.

---------------------------------------------------------
Title: On the distribution of prominence heights.
Authors: Kim, I. S.; Klepikov, V. Yu.; Koutchmy, S.; Stepanov, A. I.;
Stellmacher, G.
1988BSolD1988...75K Altcode:
The distribution of prominence heights is studied. Prominence
pictures obtained in 1979 - 1986 by the Nikolsky magnetograph are
used. Discreteness in the distribution of heights is found. There are
two peaks: the first narrow peak at 20 - 25 arc sec and the second
one at 35 - 45 arc sec. One finds that the prominences with heights
less than 25 arc sec locate mainly at the latitude interval 0 &lt;
φ ≤ 20°. During the preminimum and minimum of solar activity the
average latitude of the filaments (prominences) formation is 18 -
21°. The most likely height interval for prominence formation is at
20 - 25 arc sec (which is the critical height).

---------------------------------------------------------
Title: Solar cycle variations of coronal neutral lines and polar
regions activity.
Authors: Makarov, V. I.; Makarova, V. V.; Koutchmy, S.; Sivaraman,
K. R.
1988sscd.conf..362M Altcode:
Observations of the corona, of prominences, of polar faculae and of
large scale magnetic fields show solar activity over all latitudes, in
contrast with sunspot activity, which is limited to mid-latitudes. The
global behaviour of the solar activity is considered here thanks to
the analysis of chromospheric synoptic maps which include the location
of Hα and Ca II K prominences. The process of "migration" of neutral
lines during the cycle (supposed to represent the large scale coronal
magnetic field) is shown.

---------------------------------------------------------
Title: Image processing of coronal pictures.
Authors: Koutchmy, Olga; Koutchmy, Serge; Nitschelm, Christian;
Sykora, Julius; Smartt, Raymond N.
1988sscd.conf..256K Altcode:
The authors present the results obtained with a new simple image
processing algorithm applied to several typical eclipse and
coronographic pictures. This 2D filter (second order difference
operator in k-direction) shows superior quality by improving the
signal/noise ratio, reducing the dynamic range and enhancing faint
coronal structures. A comparison with results obtained with more
commonly used 2D filters is also presented. The authors describe
briefly the algorithm used, together with discussions of enhanced
coronal images of coronal physics interest.

---------------------------------------------------------
Title: Small scale coronal structures.
Authors: Koutchmy, Serge L.
1988sscd.conf..208K Altcode:
The author reviews a few problems connected with the observation
and the analysis of fine scale coronal density structures. The inner
corona and middle corona are considered. The relations existing between
the coronal magnetic fields and the coronal dynamics at small scale,
including impulsive events are emphasized.

---------------------------------------------------------
Title: A Study of Disconnection Velocities in the Plasma Tail
of P/halley
Authors: Caron, R.; Koutchmy, S.; Sarrazin, M.
1988scaa.conf..158C Altcode: 1988IAUCo..98..158C
No abstract at ADS

---------------------------------------------------------
Title: Etude de la dynamique du nuage zodiacal par la mesure du
décalage Doppler.
Authors: Lamy, P.; Koutchmy, S.; Bücher, A.; Robley, R.
1988jopl.conf..227L Altcode:
At the Pic-du-Midi Observatory, the authors have started a program
to observe the spectrum of the zodiacal light in the region of
the b absorption lines of Mg I. They use a 1 m spectrograph with a
holographic grating followed by a focal reducer to obtain a 19 Å/mm
dispersion over the micro-channel plate camera. Calibrated spectra
obtained with an exposure time of 10 minutes systematically show earth
atmospheric emission lines attributed to both N I and OH. The temporal
variability of these emissions prevents an accurate determination of
the line profiles.

---------------------------------------------------------
Title: Observations et propriétés des poussières de la comète
de Halley.
Authors: Lamy, P.; Perrin, J. M.; Koutchmy, S.; Grün, E.; Llebaria,
A.; Malburet, P.
1988jopl.conf..211L Altcode:
The authors present the results of various observations and analysis
of the dust grains of comet Halley.

---------------------------------------------------------
Title: High Spatial Resolution Coronal Physics: The Need for Larger
Coronagraphs
Authors: Smartt, R. N.; Koutchmy, S.; Zirker, J. P.
1987BAAS...19Q1122S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Des observations à grand champ et en couleur.
Authors: Caron, R.; Koutchmy, S.; Sarrazin, M.
1987LAstr.101..255C Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Night sky optical spectrum from a high altitude observatory.
Authors: Louistisserand, S.; Bucher, A.; Koutchmy, S.; Lamy, P.
1987A&AS...68..539L Altcode:
Night sky spectrum between 380 and 660 nm with effective spectral
resolution of 0.2 nm is presented for evaluation of effects
produced by the different sources of light including lights of urban
origin. Numerous emission lines superposed on a continuum spectrum
are identified.

---------------------------------------------------------
Title: Small-scale motions over concentrated magnetic regions of
the quiet Sun
Authors: Dara, H. C.; Alissandrakis, C. E.; Koutchmy, S.
1987SoPh..109...19D Altcode:
We have used a 5.5 min time-sequence of spectra in the Fe I lines
λ5576 (magnetically insensitive), λ6301.5 and λ6302.5 (magnetically
sensitive) to study the association of concentrated magnetic regions
and velocity in the quiet Sun. After the elimination of photospheric
oscillations we found downflows of 100-300 m s −1,
displaced by about 2″ from the peaks of the magnetic field; this
velocity is comparable to downflow velocity associated with the
granulation and of the same order or smaller than the oscillation
amplitude. Quasi-periodic time variations of the vertical component
of the magnetic field up to ± 40% were also found with a period near
250 s, close to the values found for the velocity field. Finally we
report a possible association of intensity maxima at the line center
with peaks of the oscillation amplitude.

---------------------------------------------------------
Title: L'observation des filigrées.
Authors: Koutchmy, S.
1987JAF....29...14K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Some Statistical Properties of the Magnetic Field in
Prominences
Authors: Kim, I.; Koutchmy, S.; Stellmacher, G.; Stepanow, A. I.
1987rfsm.conf..289K Altcode:
Magnetic field observations based on the Zeeman effect, measuring the
longitudinal component B∥ of the field with an entrance
hole of 6.4 arcsec diameter, were obtained for a great number of
prominences during 1979 to 1985.

---------------------------------------------------------
Title: Improved measurements of scattered light level behind
occulting systems.
Authors: Koutchmy, S.; Belmahdi, M.
1987JOpt...18..265K Altcode: 1987JOp....18..265K
No abstract at ADS

---------------------------------------------------------
Title: Micrométéorites et débris orbitaux.
Authors: Koutchmy, S.
1987LAstr.101..426K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Properties of a Concentrated Magnetic Field Region
Authors: Koutchmy, S.; Stellmacher, G.
1987rfsm.conf..103K Altcode:
Further results concerning the fine structure of concentrated magnetic
field regions or network elements, observed near disk center well
outside of active regions, are presented.

---------------------------------------------------------
Title: Ground-Based Large-Scale Monochromatic Images of Comet Halley
during the Giotto Flyby
Authors: Koutchmy, S.; Lamy, P.; Loucif, M.; Malburet, P.
1986ESASP.250c..79K Altcode: 1986ehc3.conf...79K
A wide-field camera (f = 135 mm) equipped with an image-tube was set up
at the geophysical observatory of Tamanrasset during the first half of
March. Monochromatic images were obtained in CN (390 nm), CO+
(426.3 nm) and in the continuum (582 nm), in March 14.19, a few hours
after the Giotto flyby.

---------------------------------------------------------
Title: The Disconnection Events of January 10 and April 8 1986 IN
the Plasma Tail of Comet Halley
Authors: Caron, R.; Guerin, P.; Koutchmy, S.; Sarrazin, M.; Zimmermann,
J. P.
1986ESASP.250c.143C Altcode:
A sequence of 6 white-light pictures covering 10 hrs of the Jan. 10,
1986 Halley's comet plasma tail disconnection was analyzed in order to
deduce the variation of the relative velocity of the ion tail revealing
a sudden acceleration. A second sequence of 8 CO(+) pictures covering
2.5 hr of the April 8, 1986 large disconnection event was obtained and
the velocity field was studied. An attempt to trace the origin of this
event on early sequence of white light pictures is discussed, as well
as the occurrence of sudden accelerations. The images confirm sudden
increases or decreases of the velocity, but it is difficult to say
whether these changes can be wholly attributed to sudden acceleration.

---------------------------------------------------------
Title: Early resolved structures in the coma of Comet Halley
Authors: Dossin, F.; Guerin, P.; Koutchmy, S.; Lamy, P.; Malburet, P.
1986ESASP.250b.173D Altcode: 1986ehc2.conf..173D
Three high-resolution photographs of comet Halley were obtained on
September 12, 1985 with the Schmidt telescope operated by CNRS and
Liège University at the Observatoire de Haute-Provence on hypered
Kodak 2415 film and exposure times of 1 hour. The best image (FWHM
of 2 arcsec) has been analyzed in order to deduce the 2-dimensional
distribution of light presumably scattered by the dust. Two jet-like
structures are present in the near nuclear region, one extending outward
up to 15 arcsec. The total absolute magnitude has also been determined.

---------------------------------------------------------
Title: Étude de la structure de la couronne solaire grâce aux
éclipses totales.
Authors: Koutchmy, Serge
1986LAstr.100..499K Altcode:
The methods used and results of worldwide photometric imaging of
the solar corona during total eclipses are summarized. Combining
the observations from different sites enlarges the temporal window
of the observations from minutes at a single site to several hours
of data. Attention is given to techniques applied to estimate the
contributions from light reflected by the coronal plasma and by dust
in the interplanetary medium. Sample coronographic images illustrate
methods employed to study coronal structures, mainly by tuning the
instruments to H-alpha wavelengths. Magnetographic data are also
discussed which are used to map the magnetic field around the sun and
thereby gain information on the solar dynamo.

---------------------------------------------------------
Title: L'observation des contacts d'une éclipse et son intérêt.
Authors: Koutchmy, Serge; Sarrazin, Michel
1986LAstr.100..525K Altcode:
Analytical techniques for predicting the occurrence of a total eclipse
at a particular location are summarized. Emphasis is placed on the use
of two opposing sites on the limb of the moon as the loci for predicting
the location and total area of a solar eclipse. The calculations
are carried out using astronomical ephemerides and, in the case of
observations from an aircraft, consider the magnetic declination of the
earth and the flight path of the aircraft. Sample data are presented
for measurements of the eclipse area predicted and measured during the
flight of an instrumented aircraft. The alterations in the location
of the lunar limb due to the coronal light of the sun are noted.

---------------------------------------------------------
Title: The solar granulation. II - Photographic and photoelectric
analysis of photospheric intensity fluctuations at the
meso-granulation scale
Authors: Koutchmy, S.; Lebecq, C.
1986A&A...169..323K Altcode:
A statistical analysis of the intensity fluctuations of the solar
photosphere, recorded photoelectrically, shows the influence of both
seeing effects and especially the 5 min oscillations when intensity
fluctuations at scales larger than the scale of the granulation are
considered. A one-dimensional photo-electric set of records was
time-averaged in order to show the existence of quasi-stationary
cells in the range 5arcsec - 50arcsec, with amplitude modulations of
up to ±30K. The photographic processing of a 23-min time sequence of
excellent granulation pictures also showed the existence of cells of
quasi-stationary intensity modulations. The amplitudes and stationary
nature are larger for larger sizes, but the existence of cells at the
meso-granulation scale is fully confirmed.

---------------------------------------------------------
Title: Dynamical properties of a pre-perihelion comet
tail. I. December 6, 1985 observations of P/Halley 82i.
Authors: Guerin, P.; Koutchmy, S.; Vial, J. C.
1986A&A...167..395G Altcode:
Wide field pictures of comet P/Halley 1982i obtained every hour on
December 6, 1985, have been analyzed in order to study the dynamics
of low intensity plasma structures in the tail. The deduced radial
velocities increase from 50 to 80 km s-1 over distances
of 2 to 6×106km. The measured apparent aberration angle
is interpreted as a result of a large polarward solar wind velocity
component.

---------------------------------------------------------
Title: The 1981 total solar eclipse. III - Photometric study of the
prominence remnant in the reversing south polar field
Authors: Stellmacher, G.; Koutchmy, S.; Lebecq, C.
1986A&A...162..307S Altcode:
High resolution white light colour pictures obtained during the
1981 total solar eclipse were used for a photometric analysis of
the S-pole region. A small helmet-like streamer was visible over
the S-polar limb overlying a faint polar prominence from the polar
crown belt of filament channels that reached 87° latitude at the
eclipse date. Typical electron densities deduced are ne
≅ 2×109cm-3 for the activated top of the
prominence and ne ≅ 6×108cm-3
for the associated coronal structures. Upward velocities up to 160 km
s-1 are obtained for the eruptive prominence parts. The
authors found that dynamic processes are controlled by magnetic
forces for fields B ≥ 3.5 Gauss, and that the coronal structures
are apparently connected with the faintest and most dynamic parts of
the prominence.

---------------------------------------------------------
Title: A kinematic analysis of the disconnection of the plasma tail
of cometP/Halley, January 10, 1986.
Authors: Guerin, P.; Koutchmy, S.
1986CRASB.303..147G Altcode: 1986CRASM.303..147G
Photographic images of Halley's Comet tail were analyzed to determine
if disconnections of the tail from the comet were due to the crossing
of the Comet from one solar magnetic sector to another. The six
photographs, taken over a 16 hr period on Jan. 10, 1986, provided detail
sufficient for about 1.2753 arcmin accuracy in the Comet ephemerides
and the tracks of nodosities at the nucleus and their antisunward
movement and separation from the cometary tail. The images depict
the simultaneous acceleration of an entire separated tail section
region followed by a deceleration of the same section, suggesting that
the tail crossed a pre-existing region of interplanetary space. The
deceleration to a velocity comparable to the remaining tail took a
period of 9 hr. Insufficient data were available for explaining the
appearance and behavior of a bar that appeared at the sunward end of
the separated nodosity and seemed associated with an influx of solar
wind matter as the IMF changed polarity.

---------------------------------------------------------
Title: Periodic Comet Halley (1982i)
Authors: Ney, E. P.; Knutson, A. G.; Wootten, Alyn; Loren, R.;
Koutchmy, S.; Lamy, P.
1986IAUC.4161....1N Altcode:
E. P. Ney and A. G. Knutson, University of Minnesota, report the
following infrared magnitudes measured with a 26" diaphragm at the
O'Brien Observatory: 1985 Dec. 12.08 UT, K = 6.8, L = 6.1, [8.6 micron]
= -0.5, N = -1.8, [12.5 micron] = -1.9, [18 micron] = -3.3; Dec. 14.00,
[8.6 micron] = 0.9, N = -0.8, [12.5 micron] = 0.0, [18 micron] = = -2.8;
Dec. 25.05, J = 6.8, K = 7.1, L = 5.2, M = 3.1, [8.6 micron] = -0.5,
N = -1.6, [12.5 micron] = -1.6, [18 micron] = -3.0; 1986 Jan. 1.0, N =
-1.4, [12.5 micron] = -0.9; Jan. 7.9, H = 6.0, K = 6.1, L = 3.9, M =
1.2, [8.6 micron] = -1.5, N = -2.8, [12.5 micron] = -2.6, [18 micron]
= -4.0. The silicate feature at 10 micron is ~ 0.5 mag above the
continuum. A. Wooten, National Radio Astronomy Observatory, reports:
"R. Loren, University of Texas, obtained spectra of P/Halley in the
region of the P(2,1) line of protonated water (H3O+) at 307.19241 GHz
on Jan. 6 with the 4.9-m telescope of the Millimeter Wave Observatory
at Fort Davis. No emission was detected, rms(TR*) = 0.85 placing a
preliminary upper limit of 5 x 10**-27 s**-1 for the H3O+ production
rate. Receiver tuning was verified through observation of CHEOH at
307.16594 GHz in OMC-1." S. Koutchmy, Institut d'Astrophysique, Paris;
and P. Lamy, Laboratoire d'Astronomie Spatiale, Marseilles, telex that
100 image-tube spectra (180 A/mm resolution, range 350-700 nm) were
obtained with the Haute Provence Observatory's 0.8-m telescope during
1985 Dec. 10-15. CN emission was detected, extending up to 2 deg away
from the sun, but no ions were noted until Dec. 12. From Dec. 13.8 UT
onward the N2+ (0,0) line at 391.4 nm was seen in the vicinity of the
coma and extending in the antisolar direction up to 2 deg. Observations
with the Marly spectrograph (range 326-526 nm, dispersion 80 A/mm,
slit width 50 micron, slit length projection 3'7, IIa-O hypered plates)
on the 1.20-m f/6 telescope during 1985 Dec. 2.76-2.98 and 3.72-3.97
UT revealed CN, C2 and C3 (all well observed); N2+ (0,0) extending
over 16"; CO+ (3,0) lines at 400.18 and 402.4 nm extending over 37"
and 14", respectively; CO2+ (0,1) at 367.4 nm was suspected; numerous
Fraunhofer absorption lines (including H and K and several Fe lines)
were also noted. Photographs (hypered IIIa-J and 2415 emulsions) of
the plasma tail with the 0.62-m f/3.5 and 0.30-m f/2 Schmidt telescopes
during Dec. 3- 15 revealed an inner part (extending &lt; 1 deg from the
head) whose orientation oscillated about the antisolar direction with a
maximum deviation of + 5P and a characteristic time of one to two days.

---------------------------------------------------------
Title: Les éclipses totales solaires.
Authors: Koutchmy, S.
1986LAstr.100..497K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Relations Between Large Scale Coronal Structure, Chromospheric
Filaments and the Solar Cycle
Authors: Koutchmy, S.; Loucif, M.; Koutchmy, O.
1986stp..conf...67K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Periodic Comet Halley (1982i)
Authors: Jewitt, D.; Meech, K.; Ricker, G.; Lamy, P.; Koutchmy, S.;
Vial, J. C.
1985IAUC.4148....1J Altcode:
D. Jewitt, K. Meech, and G. Ricker, Massachusetts Institute of
Technology, communicate: "Observations from McGraw-Hill Observatory
on Kitt Peak over 4 nights show variable structures in the inner
coma of P/Halley. Images were taken through broad and narrowband
interference filters using the MIT 'MASCOT' CCD camera on the 1.3-m
telescope. Jet-like structures were observed in position angles 358
and 313 on Nov. 29 UT. The jets extended 10 000 km in the plane of
the sky and had widths comparable to the atmospheric seeing. The
jets were visible in both broad and narrowband continuum filters and
are probably dust features. The jets showed no variation in position
angle or brightness in an observing interval of &gt; 3 hr but were
absent on the preceding and following nights." Meech and Jewitt also
report: "Observations of P/Halley with the Kitt Peak 0.61-/0.91-m
Schmidt telescope (with baked IIIa-J plates and exposure times
30-60 min) show that extensive tail development has occurred within
the past month. Observations on Nov. 6-9 showed only a transient,
faint anti-solar tail (length 20' on Nov. 6.20) which faded in &lt;
1 day. Observations on Dec. 4-8 show a persistent plasma tail (length
&gt; 2.5 deg) displaying a classical streamer morphology. We are able
to follow knots, kinks, and streamers in the tail for up to 6 hr. The
measured speeds of 3 tail knots are 190, 216, and 240"/hr (39, 45, and
50 +/- 5 km/s along the tail, km/s), considerably less than the solar
wind speed but similar to the speeds measured in the tails of other
comets. No evidence for acceleration of the features is seen. Two
episodes of ray formation have been seen in 25 hr of observation;
the rays form in ~ 1 hr and evolve over several hr, but fade in &lt;
18 hr. The tail as a whole shows gross brightness changes from night
to night. No dust tail is seen." P. Lamy, Laboratoire d'Astronomie
Spatiale, Marseille, and S. Koutchmy, Institut d'Astrophysique, Paris,
telex: "Four consecutive 1-hr-exposure IIIa-J hypered plates obtained
between Dec. 6.79-6.96 UT by Koutchmy and J. C. Vial with the 0.62-m
f/3 Schmidt telescope of Haute Provence Observatory show a disturbed,
narrow, plasma tail of length &gt; 2 deg. The tail's inner part
deviates southward from the anti-solar direction by 4.8 +/- 0.7 deg;
the outer part widens and nears the anti-solar direction. The point
of bifurcation seems to move radially outward with time."

---------------------------------------------------------
Title: Measurement of magnetic fields in solar prominences
Authors: Nikolskij, G. M.; Kim, I. S.; Koutchmy, S.; Stepanov, A. I.
1985AZh....62.1147N Altcode:
Measurements of magnetic fields in solar prominences on the basis of
the Zeeman effect are described. The circular polarization along the
entire line profile is recorded. The spectral scanning is done with a
Fabry-Perot interferometer and the modulation is done with a lithium
niobate crystal. The influence of the instrumental characteristics
on the measurements is discussed. A histogram of the frequency of
appearance of longitudinal fields with a spatial resolution of 6-8
arcsec for prominences of 1979-1982 has clear maxima at 8 and 20 G. The
peak at 20 G corresponds to prominences of active latitudes (less than
+ or - 35 deg) for which the angle beta between the long axis of the
filament and the line of sight was close to 25 deg. From a comparison
with the results measurement of the total field vector (data of Athay
et al.) for prominences of the same epoch (1979-1981) the following
conclusion is drawn about the field orientation: For prominences of
active latitudes B parallel about = B; i.e., the angle between the
long axis of a filament and the line of sight is close to the angle
between the long axis of the filament and the magnetic field vector.

---------------------------------------------------------
Title: Measurement of Magnetic Fields in Solar Prominences
Authors: Nikolskii, G. M.; Kim, I. S.; Koutchmy, S.; Stepanov, A. I.;
Stellmacher, G.
1985SvA....29..669N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The 1981 total solar eclipse corona. II. Global absolute
photometric analysis.
Authors: Lebecq, C.; Koutchmy, S.; Stellmacher, G.
1985A&A...152..157L Altcode:
Detailed results of the absolute photometry of the solar corona
during the July 31, 1981 total eclipse are presented together with
a morphological analysis. The basic calibration method uses the
detailed photometry of images of stars present on the same coronal
picture. Both sky intensity and coronal aureola variations over the
field are carefully evaluated. The recent axi-symmetric non-spherical
model of the F-corona is introduced and the relevant K-corona intensity
variations are derived. The determinations of the Ludendorf index of
flattening and the integrated total brightness of the K-corona alone
are made and discussed in relation to the phase of the sunspot cycle
of activity.

---------------------------------------------------------
Title: Periodic Comet Halley (1982i)
Authors: Koutchmy, S.; Lecacheux, J.; Dossin, F.
1985IAUC.4112....2K Altcode:
S. Koutchmy and J. Lecacheux, Institut d'Astrophysique, Paris, and
Meudon Observatory, report good-resolution, 1-hr exposures on Kodak
2415 hypered film obtained on Sept. 12-14 by F. Dossin and Koutchmy
with the 0.62-m f/3 Schmidt telescope of Haute-Provence Observatory; the
P/Halley images show a resolved central region with an average FWHM of
5"7 (5"4 north-south, 6"6 east-west) with an overall coma extension from
the nucleus of 58" (65" westward). The inner coma near the nucleus was
V-shaped with arms 3"5 long at p.a. 30 and 300. An additional faint,
jet-like feature at p.a. 30, extending radially up to 15" from the
nucleus, is apparent on the picture (free of faint star trails) obtained
on Sept. 12.094 UT; magnitudes measured by flux integration in circles
of 10" and 120" diameter were V = 15.0 +/- 0.2 and 13.8, respectively.

---------------------------------------------------------
Title: Solar constant variabilities.
Authors: de Charentenay, C.; Koutchmy, S.
1985CRASB.301..151D Altcode: 1985CRASM.301..151D
The solar-constant variations which were measured from Feb. 16-Nov. 7,
1980 by means of the NASA ACRIM experiment on board the SMM satellite
are analyzed. It is shown that if the radiative deficit produced
by the passage of sunspots on the solar disk and the radiative flux
excess produced by the passage of faculae at the edge of the solar
disk are introduced on a weekly basis, the measured variations can
be reproduced. Meudon Observatory synoptic maps are used to measure
the faculae surfaces. An empirical model which specifies the relation
between the activity cycle and the long-term solar-constant variations
is presented. A relative decrease of the solar constant at the time
of the sunspot activity minimum is predicted.

---------------------------------------------------------
Title: On a possible relation of the law of planetary distances to
the 160-minute pulsation of the sun.
Authors: Kotov, V. A.; Koutchmy, S.
1985IzKry..72..199K Altcode:
The discovery of the global solar pulsation with the period of
P0 = 160m enables to introduce characteristic
wavelength L = c×P0 = 19.24 A.U. for the solar system,
where c is the speed of light. A corresponding analysis of planetary
distances reveals the existence of a statistically significant
quasi-commensurability between L and 2πai for inner planets
and between 2ai and L for outer ones (ai being
the major semi-axis of a planetary orbit). It is suggested that this
L-commensurability can offer new approach to an explanation of the
well-known Titius-Bode law for planetary distances. The physical
mechanism enforcing the L-commensurability in the solar system is
presumably related with 160m-gravitational waves from some
external source of unknown nature.

---------------------------------------------------------
Title: The F-Corona and the Circum-Solar Dust Evidences and Properties
(ir)
Authors: Koutchmy, S.; Lamy, P. L.
1985ASSL..119...63K Altcode: 1985IAUCo..85...63K; 1985piid.proc...63K
This review deals with the main properties of the F-corona. Analysis
of its morphology and photometry allows to derive a new axisymmetric,
non-spherical model. Polarization, color and infra-red properties are
further considered. The authors suggest the existence of a variable
"local" component superimposed on a quasi-stationary "far" component.

---------------------------------------------------------
Title: Color photographic photometry of the inner zodiacal light
observed from the Salyut 7 orbital station
Authors: Koutchmy, S.; Nesmianovich, I. A.; Dzhanibekov, V. A.;
Nikolskii, G. M.
1985AbaOB..60..207K Altcode:
Photometric data of the inner zodiacal light obtained during the
Soviet-French mission aboard Salyut 7 are analyzed. Isophote curves
for zodiacal brightness are examined; it is observed that the plane
of maximum zodiacal light brightness is close to the orbital plane of
Venus. The law governing the brightness intensity is given, and the
relation between brightness intensity and elongation is studied.

---------------------------------------------------------
Title: A colorimetric and photometric analysis of the inner zodiacal
light observed from the orbiting laboratory "Salyut-7".
Authors: Dzhanibekov, V. A.; Koutchmy, S.; Nesmyanovich, I. A.;
Nikol'Skij, G. M.
1985AbaOB..60..207D Altcode:
The authors present the results of a photographic photometry
of the best colour picture of the inner zodiacal light, obtained
during the joint Soviet-French mission aboard the Salyut-7 orbiting
laboratory. Isophote-map indicates that the plane of maximum zodiacal
light brightness is very near the orbital plane of the planet
Venus. Intensity in the plane of maximum brightness can be matched
using the law BZL ≡ E-2.04 at the elongations
23° ≤ ɛ ≤ 35°, the colorimetric index being bound to be nearly
solar. The influence of submicron-sized particles seems to be excluded.

---------------------------------------------------------
Title: The 160-min period in the solar system: solar pulsation and
the spin rates of planets and asteroids
Authors: Kotov, V. A.; Koutchmy, S.
1985BCrAO..70...37K Altcode: 1985BuCri..70...37K; 1987BCrAO..70...37K
No abstract at ADS

---------------------------------------------------------
Title: Magnetic and Velocity Field Analysis of a Quiet Region near
the Center of the Sun
Authors: Dara-Papamargariti, H.; Koutchmy, S.
1985LNP...233..231D Altcode: 1985hrsp.proc..231D
A selected region of the quiet sun near the center of the disc was
analyzed in order to deduce parameters concerning regions of highly
concentrated magnetic field, including network elements. The present
analysis covers a sequence of spectra corresponding to a total time
laps of 6 min over the same region. Spectra of both magnetically
sensitive and insensitive lines were measured in detail in order to
deduce the velocity distribution around magnetic flux tubes. Large
amplitude five minute oscillatory components were removed using an
averaging over time procedure. Preliminary results are discussed as
well as factors which could affect their interpretation.

---------------------------------------------------------
Title: A possible relation between planetary distances and the
160-minute solar pulsation.
Authors: Kotov, V. A.; Koutchmy, S.
1985BCrAO..72..171K Altcode: 1985BuCri..72..171K; 1987BCrAO..72..171K
No abstract at ADS

---------------------------------------------------------
Title: Doppler Shifts Measurements of the Zodiacal Light at the PIC
Midi Observatory
Authors: Robley, R.; Buecher, A.; Koutchmy, S.; Lamy, Ph.
1985ASSL..119...85R Altcode: 1985IAUCo..85...85R; 1985piid.proc...85R
The authors have started a program to observe the spectrum of the
zodiacal light in the region of the b absorption lines of Mg I. They
use a 1 meter spectrograph with a holographic grating followed by a
focal reducer to obtain a 19 Å/mm dispersion over the micro-channel
plate camera. Calibrated spectra obtained with an exposure time of 10
minutes systematically show earth atmospheric emission lines attributed
to both N I and OH. The temporal variability of these emissions
prevents an accurate determination of the line profiles. The authors
best processed measurements of Doppler shifts obtained during five
nights do not allow to discriminate between circular and hyperbolic
orbits of the interplanetary dust.

---------------------------------------------------------
Title: Facular and Duration of the Solar Cycle
Authors: Makarov, V. I.; Makarova, V. V.; Koutchmy, S.
1985BSolD...8...53M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A magnetograph with scanning along the whole profile of a
spectral line.
Authors: Nikol'Skij, G. M.; Kim, I. S.; Klepikov, V. Yu.; den, O. E.;
Stepanov, A. I.; Koutchmy, S.
1985AbaOB..60..177N Altcode:
A magnetograph with scanning along the whole profile of the line is
described. This instrument was built for measuring magnetic fields
in prominences and in the corona. The study of the Zeeman effect is
carried out in different emission lines.

---------------------------------------------------------
Title: Global solar oscillations observed from relative near-IR
photosphericbrightness fluctuations.
Authors: Kotov, V. A.; Koutchmy, S.; Kononovich, Eh. V.; Ryzhikova,
N. N.; Tsap, T. T.
1985BCrAO..73...24K Altcode: 1987BCrAO..73...24K
No abstract at ADS

---------------------------------------------------------
Title: Polar faculae and duration of the solar cycle.
Authors: Makarov, V. I.; Makarova, V. V.; Koutchmy, S.
1985BSolD1985...53M Altcode:
An analysis of a 20-year series of daily observations of polar faculae
has been made. It is shown that for the cycle with a one-fold polarity
reversal the solar activity in the polar zone correlates rather well
with the sunspot activity in 2.5 cycles, i.e. in 27 - 28 years. In the
cycles with a three-fold polarity reversal the shift takes place in
about 6 years. A conclusion is made that the global process of solar
activity at all the latitudes lasts for about 17 - 18 years.

---------------------------------------------------------
Title: A Coronascanner for a Sun Oriented Space Mission
Authors: Koutchmy, S.; Lamy, P. L.
1985ASSL..119..141K Altcode: 1985IAUCo..85..141K; 1985piid.proc..141K
No abstract at ADS

---------------------------------------------------------
Title: Photometric calibrations of an MCP space qualified
photographic-camera
Authors: Koutchmy, S.; Verlhac, A.
1985A&A...142..355K Altcode:
The authors describe the methods developed to guarantee quantitative
calibrations of a high sensitivity micro-channel plate photo-camera
designed to obtain large scale night sky pictures of astronomical
and geophysical interest in the optical and near infrared spectral
range. In-flight calibrations were obtained with a sensitometer
and absolute calibrations were performed in laboratory with a
quasi-monochromatic black body source. Results obtained for calibrating
the camera are given with emphasis on the comparison of measurements
deduced in ground based and orbital condition.

---------------------------------------------------------
Title: Photographic Observations of the Inner Zodiacal Light Aboard
Saliout 7
Authors: Nikolskii, G.; Koutchmy, S.; Lamy, P. L.; Nesmianovich, I. A.
1985ASSL..119....7N Altcode: 1985IAUCo..85....7N; 1985piid.proc....7N
Color photographs of the inner zodiacal light were obtained aboard
Salyut 7 with Kodak Ekta 400. Absolute calibrations were performed
in-flight with attenuated sunlight. The photometric analysis was carried
out in three colors and corrections were introduced for the O I emission
of the F layers. The brightness of the zodiacal light along the ecliptic
is found in good agreement with published data while its color is found
slightly redder than the sun. Its out-of-ecliptic variation coincides
neither with the fan nor the ellipsoidal model; the photometric axis
is found near the projection of the orbital plane of Venus.

---------------------------------------------------------
Title: Astrophysical and geophysical observations with piramig/salyut
7 experiment
Authors: Levasseur-Regourd, A. C.; Courtes, G.; Herse, M.; Koutchmy,
S.; Lamy, P.; Muliarchik, T. M.; Rocca-Volmerange, B.; Savchenko,
S. A.; Secher, B.; Tovmassian, H. M.; Beresovoy, A. N.; Chretien,
J. L.; Ivanchenkov, A. S.; Djanibekov, V. A.; Lebedev, V. V.; Popov,
L. I.; Savitskaya, S. E.; Serebrov, A. A.
1985AdSpR...5c..27L Altcode: 1985AdSpR...5...27L
The facility offered by the Salyut 7 vehicle has allowed
teams of scientists of 3 CNRS french laboratories to develop
an instrument optimized for several disciplines in astrophysics
and geophysics. P.I.R.A.M.I.G. (Photography Infra-Red Atmosphere,
Interplanetary Medium, Galaxies) is a wide field (10° and 40°) camera
devoted to high sensitivity photographic photometry. The spectral
range is limited to the visible and near-infrared (400-850 nm), the
main advantage being to observe above the absorving and emitting layers
of the atmosphere.

---------------------------------------------------------
Title: Global oscillations of the sun according to observations of
(relative) fluctuations of photospheric brightness in the near
infrared
Authors: Koutchmy, S.; Kononovich, E. V.; Ryzhikova, N. N.; Kotov,
V. A.; Tsap, T. T.
1985IzKry..73...26K Altcode:
The instrument designed for monitoring of relative center-to-limb
brightness fluctuations of the photosphere in near IR spectral range (λ
= 1.65 μm) is described. Analysis of 67 days of observations carried
out in 1981 - 1982 shows clearly the presence of 160-min variations of
the differential, center-to-limb intensity with an average amplitude
of about 3×10-5 in units of the {average solar} brightness
near 1.65 μm or 0.2K in terms of the temperature of the photosphere.

---------------------------------------------------------
Title: G. M. Nikolsky, 1929 - 1982.
Authors: Koutchmy, S.
1985ASSL..119D..23K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Empirical model of the solar corona using solar-cycle related
parameters.
Authors: Koutchmy, S.; Loucif, M.
1984ESASP.220..265K Altcode: 1984ESPM....4..265K
Using a set of eclipse pictures, the distribution of stream lines over
the outer corona was analyzed.

---------------------------------------------------------
Title: Comparative magnetographic observations in different prominence
lines
Authors: Nikolsky, G. M.; Kim, I. S.; Koutchmy, S.; Stellmacher, G.
1984A&A...140..112N Altcode: 1984A&A...140..112K
Analysis of the longitudinal field strength in prominences obtained
by measurements of Zeeman polarization in HeD3, Hα, and Hβ is
presented. The measurements were performed with the spectrally scanning
magnetograph installed at the 53 cm coronograph of the Kislovodsk high
altitude station. The observations allow to correlate the values of
the equivalent widths and those of the half widths with magnetographic
data. No systematic dependence of field strengths on line widths is
found. High field strengths persist for large Doppler shifts and low
emissions. In the histogram showing the distribution of observed field
strengths two peaks near B∥ ≅ 8 Gauss and B∥
≅ 20 Gauss appear. The second peak corresponds to prominences
mainly related to active regions for latitudes &lt;±35°. A similar
distribution is obtained from a set of data deduced from observation
of the Hanle effect and corresponding to the same epoch.

---------------------------------------------------------
Title: Éclipse totale du soleil sur un territoire français
d'Outre-mer, La Nouvelle-Calédonie, le 23 novembre 1984.
Authors: Nitschelm, Ch.; Koutchmy, S.
1984LAstr..98..393N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Photometric analysis of the June 11, 1983 solar corona
Authors: Koutchmy, S.; Nitschelm, C.
1984A&A...138..161K Altcode:
The solar corona was observed using different photo-cameras during the
solar total eclipse on June 11, 1983 under good sky conditions. Pictures
were used to perform a detailed morphological analysis of K-corona
structures and an isophotometric analysis. Accurate values of the
flattening index over 8 earth-radii are deduced.

---------------------------------------------------------
Title: Photographic colour photometry of the inner zodiacal light.
Authors: Nikol'Skij, G. M.; Koutchmy, S.; Nesmyanovich, I. A.
1984ATsir1310....3N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A Magnetograph Scanning Along the Whole Profile of the Line
Authors: Nikolsky, G. M.; Kim, I. S.; Koutchmy, S.; Klepikov, V. Y.;
Den, O. E.; Stepanov, A. I.
1984BSolD...9...88N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Widefield Coronograph for Observations of Coronal
Transient Phenomena
Authors: Nikolsky, G. M.; Koutchmy, S.; Fatianov, M. P.
1984BSolD...7...53N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A magnetograph scanning along the whole profile of a line.
Authors: Nikol'Skij, G. M.; Kim, N. S.; Koutchmy, S.; Klepikov,
V. Yu.; den, O. E.; Stepanov, A. I.
1984BSolD1984...88N Altcode:
A magnetograph recording the Zeeman-effect along the whole profile of a
line with modulator of a LiNbO crystal and a Fabry-Perot interferometer
is described.

---------------------------------------------------------
Title: Wide-field coronograph for observations of coronal transient
phenomena.
Authors: Nikol'Skij, G. M.; Koutchmy, S.; Fat'yanov, M. P.
1984BSolD1984...53N Altcode:
A small Lyot coronograph is described. The results of the trial
observations are discussed.

---------------------------------------------------------
Title: Periodic Comet Crommelin (1983n)
Authors: Koutchmy, S.; Laques, P.; Lecacheux, J.
1983IAUC.3876....2K Altcode:
The following three precise positions, obtained using a micro-channel
device on the 2-m reflector at Pic du Midi, have been selected from 21
made on the same night by S. Koutchmy, P. Laques and J. Lecacheux. The
positions are geocentric. 1983 UT R.A. (1950.0) Decl. Sept. 4.94350 20
07 26.92 +22 13 55.5 4.96399 20 07 25.44 +22 13 46.8 4.97875 20 07 24.52
+22 13 40.3 P/Crommelin has been selected by the International Halley
Watch for a dry run to test out the procedures planned for observations
of P/Halley. This test will mainly be during the week 1984 Mar. 25-31,
at which time P/Crommelin will probably not be fainter than mag 17.5
(although it may not be all that much brighter).

---------------------------------------------------------
Title: Photospheric faculae-III-intensity, and magnetic field mapping
of a typical element of the photospheric network
Authors: Dara-Papamargaritis, H.; Koutchmy, S.
1983A&A...125..280D Altcode:
The authors studied a typical quiet sun magnetic network
element. Without introducing any correction, high spatial resolution
spectra (=0arcsec.75) of two iron lines, simultaneous Ca II K
and white-light slit-jaw pictures as well as spectroheliograms in
H&amp;alpha; and Mgb1 - 0.4 Å of a typical
quiet region of the solar photosphere were analyzed in order: 1. to
map the intensity, the velocity field and the magnetic field of a
typical element of this region; 2. to study the underlying solar
granulation, which seems to have a lower contrast; 3. to get from
H&amp;alpha; filtergrams the fibril structure around the
rosette. Finally the authors give an estimate of the magnetic flux of
a large region of the quiet sun.

---------------------------------------------------------
Title: Photometric analysis of sunspot umbral dots. III
Spectrophotometry and preliminary model of a 2-component umbra
Authors: Adjabshirzadeh, A.; Koutchmy, S.
1983A&A...122....1A Altcode:
An empirical two-component model of the solar sunspot core based on the
results of a two-dimensional photometrical analysis of quasi-statistical
nature is presented. Spectrophotometrical line profile measurements of
a highly selected observation are also used. The core of a sunspot
is considered to be composed of a more or less homogeneous dark
and cold background occupying 95 percent of the area of the core,
with many tiny, very bright umbral dots embedded inside. The average
radiative flux corresponding to the dots amounts to 37 pecent of the
total flux of the core at 6000 A. With a calculated distribution of
temperature and pressure of the proposed hydrostatic two-component
model, it is demonstrated that the essential results given by the
most recent homogeneous models can be easily retrieved when the hot
and cold components of the present model are adequately mixed.

---------------------------------------------------------
Title: Exploration du ciel nocturne par photographie à partir de
la station orbitale Saliout.
Authors: Belmahdi, M.; Koutchmy, S.
1983LAstr..97..263B Altcode:
The photography equipment and procedures, and examples of ionospheric
and sky surveys performed from the Salyut space station during the visit
by the French astronaut Chretien are described. Space-based viewing is
unencumbered by skyglow from cities, the appearance of false sources
near the terminator line, and interferences from the ionospheric F
region. Standard astronomical and photographic equipment were used,
including cross-hair sights, filters, objectives, and cassette loaded
films. Once an object was sighted and the cameras pointed the entire
station was placed into an inertial navigation mode to provide up to 40
sec stability for photography. Samples from studies of the ionospheric
D region, the zodiacal cloud, and terrestrial limb are provided.

---------------------------------------------------------
Title: Short period coronal oscillations - Observation and
interpretation
Authors: Koutchmy, S.; Zhugzhda, Ia. D.; Locans, V.
1983A&A...120..185K Altcode:
The result of an experiment devoted to the search of short period
coronal waves using the green coronal line 5303 Å of Fe XIV are
analyzed. After the subtraction of sky aureola fluctuations, 2
time series of measurements performed at a 40arcsec height over a
faint facular area and small changing chromospheric features show
power spectra with evidence of Doppler velocity oscillations with
periods near 300 s, 80 s, and especially 43 s. However, no prominent
intensity fluctuations appeared. The observed waves are considered
as good candidates for being resonant Alfvén oscillations viewed at
a low level through several legs of coronal arches, with a typical
distance between feet being equal to the autocorrelation distance of
the network and with foot-points inserted in the photosphere. A model
of such an arch is subsequently computed and seems to fit quite well
the observed periods and velocity amplitudes. In addition the energy
flux balance is evaluated and the role of such waves in the heating
mechanism of coronal arches is discussed.

---------------------------------------------------------
Title: Les éclipses totales et l'environnement solaire.
Authors: Koutchmy, S.
1983LAstr..97..177K Altcode:
The solar corona, which becomes highly visible during an eclipse,
was first characterized as belonging to the sun in 1868, and the
ionized state of the plasma was recognized in 1941. Coronal jets,
i.e., particle streaming, were recognized in the 20th century. Modern
era measurements include spectroscopic and radioastronomical data,
gathered during the transit of the moon across the solar disk, with
'slices' taken of different sections of the solar image. Spectroscopy
and monochromatic photometry have disclosed the limb structures of
the chromosphere and coronal bursts. The ability to photograph the
coronal features in totality during an eclipse is emphasized, as is
photography of the stellar field around the sun. Comparisons are then
made with photographs taken six months later. Additionaly, total field
photography allows for examinations of the solar magnetic field lines
and the plasma flow, which is the origin of the solar wind.

---------------------------------------------------------
Title: The electron density of faint prominences observed during
the solar eclipse of July 31, 1981
Authors: Koutchmy, S.; Lebecq, C.; Stellmacher, G.
1983A&A...119..261K Altcode:
Prominences visible on the narrow band filtergrams of the
eclipsed Sun, July 3t, 1981, are analysed. The ratio of the Hβ
line intensity to the continuum intensity at λ=6073 Å is used to
derive the electron density ne as a function of electron
temperature Te. The prominences present on that day were
of low brightness: Eβ,max ≃ 0.2 104 [erg
cm-2 s-1 sterad-1]. An electron density
ne = 5.7 109 [cm-3] at Te
= 10,000° is obtained, being typical for prominence edges.

---------------------------------------------------------
Title: Observation of global 160-min infrared (differential) intensity
variation of the Sun
Authors: Kotov, V. A.; Koutchmy, S.; Koutchmy, O.
1983SoPh...82...21K Altcode: 1983IAUCo..66...21K
The method developed and the instrument designed for detecting
variations of the solar limb darkening at the atmospheric transparency
window of the solar opacity minimum region of λ 1.65 μ are
described. This differential technique proved to be successful in
rejecting undesirable low frequency noises due to the atmosphere
and to the instrument. Analysis of observations made in 1977, 1978,
and 1981 indicates the persistance of global fluctuations of the IR
differential, center-to-limb intensity at the wellknown 160 min period
with an average amplitude of about ± 2 × 10-4 in units
of the `average Sun' intensity near 1.65 μm.

---------------------------------------------------------
Title: Relative distribution of colour of the solar corona on June
30, 1973.
Authors: Nikol'Skij, G. M.; Koutchmy, S.; Nesmyanovich, I. A.
1983BSolD1983...67N Altcode:
A more precise photometric analysis of a colour picture obtained
during the June 30, 1973 total solar eclipse showed that the F-corona
is slightly redder than the K-corona.

---------------------------------------------------------
Title: Relative Distribution of Color of the 1973JUN30 Solar Corona
Authors: Nikolsky, G. M.; Koutchmy, S.; Nesmyanovich, I. A.
1983BSolD...4...67N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Measurement of magnetic fields in solar prominences.
Authors: Nikol'Skij, G. M.; Kim, I. S.; Koutchmy, S.; Stepanov, A. I.
1983ppsf.conf...52N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Night Sky from Salyut
Authors: Koutchmy, S.; Nikolskii, G. M.
1983S&T....65...23K Altcode:
The equipment and astronomical observations on the Salyuts 6 and 7
space stations are described. Noting that only one and a half hours
of night sky viewing are available during each orbit, observations
become either well-planned or innovative, with the presence of a
crew in space an asset to taking advantage of opportunities as they
arise. Human movement on board the stations is restricted while viewing
is being performed. The station can be inertially stabilized for up
to 40 sec. The results of photography of the F layer are presented,
together with twilight photography and a reproduction of the inner
zodiacal cloud. Other sessions have recorded the internal structure
of noctiluminescent clouds, the 6300 A emissions of the F layer,
and auroral structures.

---------------------------------------------------------
Title: Eclipse Totale de Soleil du 11 Juin 1983 Propositions
D'observations Astrophysiques pour L'equipe de la S. a. F.
Authors: Koutchmy, S.
1982O&T.....2....3K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Measurements of the Magnetic Field in Solar Prominences with
a Spectrally Scanning Magnetograph
Authors: Nikolskii, G. M.; Kim, I. S.; Koutchmy, S.
1982SoPh...81...81N Altcode:
We describe observations with a new magnetograph capable of recording
the whole profile of emission lines in prominences. Two recordings
are used simultaneously to study the Zeeman effect in circularly
polarized light. The spectral scan is produced by the action of piezo
ceramics of a Perot-Fabry inter ferometer combined with a narrow band
interference filter.

---------------------------------------------------------
Title: Magnetic field in solar prominences measured with a new
spectrally scanning magnetograph
Authors: Kim, I. S.; Nikolsky, G. M.; Koutchmy, S.; Stellmacher, G.
1982A&A...114..347K Altcode:
Observations of the longitudinal field strength in quiescent prominences
obtained with the new redesigned spectrally scanning magnetograph
installed in the Coude focus of the 53 cm coronograph of the Kislovodsk
station are presented. With the instrument one can obtain magnetographic
data as well as central intensities, equivalent widths, line widths,
and shifts of the analyzed prominence lines. A first discussion,
correlating magnetographic and spectroscopic data, is given

---------------------------------------------------------
Title: Large-scale Photographic Observations, Photometry, Colorimetry
and Polarimetry of Cometary Tails
Authors: Lamy, P. L.; Koutchmy, S.
1982ncgb.conf..243L Altcode: 1982gbhc.work..243L
The use of large-scale photographic observations to characterize
the dust tails of comets is discussed, with emphasis on plans being
developed for observing Halley's Comet in 1986. The techniques used to
investigate the geometric structure of the dust tail and its evolution
(including detached structures, bursts, striae, and large-scale
extensions), the integrated magnitude from blue to far IR, and color
and polarization parameters are reviewed and illustrated with data
and images from recent studies of other comets. The requirements
for a network of identical cameras for Halley observations are
examined: minimum 30-deg field of view, spectral coverage and filter
separation, polarizers, calibration, color emulsions, and data-reduction
schemes. Many of the problems inherent in ground observations programs
could be avoided by using a space instrument such as the very-wide-field
camera flown on the first Spacelab mission; this device is briefly
described.

---------------------------------------------------------
Title: About the Foreshortening Effect on Sunspot Umbral Dots
Authors: Adjabshirzadeh, A.; Koutchmy, S.
1982SoPh...75...71A Altcode:
Using high-resolution pictures of the core of a unipolar sunspot
observed with several cos θ values, we studied the center limb effect
on the form of the bright umbral dots. The ratio of the apparent sizes
in radial and tangential direction do not show the foreshortening
effect typically observed in granular structures.

---------------------------------------------------------
Title: Study of the Interplanetary Dust at High Ecliptic Latitudes:
Doppler-Fizeau Shifts
Authors: Robley, R.; Bucher, A.; Koutchmy, S.
1982ASSL...96..255R Altcode: 1982spls.meet..255R
No abstract at ADS

---------------------------------------------------------
Title: Soviet-French observations of the total solar eclipse.
Authors: Koutchmy, S.; Nikol'Skij, G. M.
1982ZemVs...1...65K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A Search of Short-Period Coronal Waves
Authors: Koutchmy, Serge
1981SSRv...29..375K Altcode:
In 1973, during the total solar eclipse, we flew an experiment aboard
the Concorde supersonic airliner in order to investigate the possible
presence of white-light coronal waves. Our experiment failed to detect
any significant effects, so it became clear that such waves should be
searched for by use of finer, i.e., spectroscopic methods.

---------------------------------------------------------
Title: An Opportunity for the Observations of Comets with Widefield
Cameras Aboard the Salyut Space Station
Authors: Lamy, P. L.; Koutchmy, S.
1981motc.conf..190L Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Soviet-French joint study of the solar corona. III - The
structure and certain dynamic features of the corona of June 30, 1973
Authors: Vsekhsvyatsky, S. K.; Dzyubenko, N. I.; Ivanchuk, V. I.;
Popov, O. S.; Rubo, G. A.; Koutchmy, S.; Koutchmy, O.; Shtelmacher, G.
1981AZh....58..810V Altcode:
The overall, as well as the detailed and fine, structure of the corona
extending to approximately 3.0-4.0 solar radii is studied. The structure
is compared with formations on the solar surface, and certain changes in
the structure are traced for periods of 80-90 min. The structure of the
rays in the outer corona is studied out to 12 solar radii by reproducing
computer-enhanced negatives from a short-focus camera. New phenomena
are detected, namely, quasi-continuous dynamic disturbances occurring in
and near coronal holes (rifts); they appear to be hydromagnetic in the
same way as coronal transients. Data are obtained on the fine-filament
structure of the corona, on the relationship between this structure and
the magnetic fields and current layers, on the spatial arrangement of
large helmet-like rays, on the width of the visibility zone, and on
the relationship between the overall structure of the corona and the
N-S asymmetry of the activity of the 20th cycle.

---------------------------------------------------------
Title: Joint Soviet - French Investigations of the Solar Corona -
Part Three - Structure and Some Dynamic Features of the Solar Corona
of 1973JUN30
Authors: Vsekhsvyatskii, S. K.; Dzyubenko, N. I.; Ivanchuk, V. I.;
Popov, O. S.; Rubo, G. A.; Koutchmy, S.; Koutchmy, O.; Stellmacher, G.
1981SvA....25..463V Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Photometric Analysis of the Sunspot Umbral Dots - Part Two -
Size Shape and Temperature
Authors: Koutchmy, S.; Adjabshirzadeh, A.
1981A&A....99..111K Altcode:
We use several selected very high resolution pictures obtained
at 4680 Å and 6000 Å at the prime focus of the Sacramento Peak
Vacuum Telescope to study the sizes, shape, and typical brightness
temperatures of the umbral bright dots observed well inside the core
of a unipolar sunspot. A two-dimensional photometric analysis was
performed. Results are consistent with the picture of a core composed
of a cool background atmosphere at a constant level with many extremely
bright embedded dots. The average diameter of dots is 190 km and their
brightness temperature, 6185 °K. Sizes of dots as well as their rounded
shape are approximately constant whatever the values of cos θ are;
conversely, their intensities show a decrease with increasingly center
limb distances.

---------------------------------------------------------
Title: Sensitometry during Orbital Missions Aboard the Salyut
Space Station
Authors: Koutchmy, S.
1981asph.conf...11K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Joint Soviet / French Investigations of the Solar Corona -
Part Two - Photometry of the Solar Corona of 1973JUN30
Authors: Vsekhsvyatskii, S. K.; Dzyubenko, N. I.; Ivanchuk, V. I.;
Popov, O. S.; Rubo, G. A.; Koutchmy, S.; Koutchmy, O.; Stellmacher, G.
1981SvA....25..211V Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Measurement of the Continuum Background of Solar Prominences
Using a Large Coronagraph
Authors: Koutchmy, S.; Nikolskij, G. M.
1981PAZh....7..183K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Joint Soviet-French studies of the solar corona. II -
Photometry of the solar corona on June 30, 1973
Authors: Vsekhsvyatsky, S. K.; Dzyubenko, N. I.; Ivanchuk, V. I.;
Popov, O. S.; Rubo, G. A.; Koutchmy, S.; Koutchmy, O.; Shtelmacher, G.
1981AZh....58..376V Altcode:
Results are presented of a study of negatives obtained on June 30,
1973 during the total solar eclipse in Africa; the study was part of
a joint Soviet-French experiment on white corona dynamics, carried
out by expeditions of Kiev University (Atar, Mauritania) and the
Paris Astrophysical Institute (Moussoro, Chad). The distribution of
total corona brightness up to 4.5 solar radii and its K and F corona
components for east and north directions were found on the basis of
novel methods of photometry and colorimetry using star images up
to 8.5m as the photometry standards. Neither the color effect nor
flattening is found in the inner part (less than 2.5 solar radii)
of the F corona. Integral corona brightness in the standard zone of
1.03-6.00 solar radii was found to be 0.64 x 10 to the -6th solar-E.

---------------------------------------------------------
Title: Infrared Imaging and Speckle Observations with a TV Camera
Authors: Lamy, P.; Koutchmy, S.
1981Msngr..23....5L Altcode:
The lack of suitable two-dimensional detectors has been a major
problem for infrared imaging in astronomy, and most results so far have
been obtained by scanning the object with a single detector (e. g.,
Terrile and Westphal,lcarus, 30, 730, 1977). The relative merit of
both techniques was thoroughly investigated by Hall (Applied Optics,
10, 838, 1971) who concluded that, below about 2.5 ~lm, camera tubes
should be preferred to scanners. Besides, sufficiently long times
required by the scanning technique are not always available for some
astronomical applications. These considerations led us to acquire a
standard television camera equipped with an infrared vidicon tube N156
manufactured by Hamamatsu Co. (Japan).

---------------------------------------------------------
Title: Measurements of the Background Continuum of Prominences with
a Large Coronagraph
Authors: Koutchmy, S.; Nikolskii, G. M.
1981SvAL....7..102K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On TV Observations of Polarization of Green Coronal Line at
the Eclipse Time of 1981JUL31
Authors: Popov, O. S.; Ivchenko, V. N.; Lapchuk, V. P.; Milinevsky,
G. P.; Osminkina, K. I.; Koutchmy, S.; Begot, J.; Lebeq, C.;
Stellmacher, G.
1981ATsir1202....1P Altcode: 1981ATsir1202Q...1P
No abstract at ADS

---------------------------------------------------------
Title: Spectrophotométrie de fond du ciel et dynamique du nuage
zodiacal
Authors: Koutchmy, S.; Bucher, A.; Robley, R.
1981hrse.conf...39K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Detection of 160 min solar intensity variations: sampling
effects.
Authors: Koutchmy, S.; Koutchmy, O.; Kotov, V. A.
1980A&A....90..372K Altcode:
The theory that the 2 h 40 min period in the Crimean and Stanford
global solar velocity oscillation measurements may have resulted
partly by 1-day sampling is verified using the IR center-limb
intensity variations measurements. It was shown that (1) the power
spectrum of these data has a peak near the 2 h 40 min period, and (2)
the power spectra of the series with the observing windows 'filled'
with a constant do not manifest a significant peak at the 9th harmonic
of the day. It was concluded that the analysis of the really observed
data is not biased by the influence of data windows and 1-day sampling
regularity of observations.

---------------------------------------------------------
Title: Photometric analysis of the sunspot umbral dots. I - Dynamical
and structural behaviour
Authors: Adjabshirzadeh, A.; Koutchmy, S.
1980A&A....89...88A Altcode:
A sequence of selected high resolution white light pictures
of a unipolar sunspot was studied in order to measure the main
characteristics of umbral dots size, contrast value, and lifetime. Using
a statistical analysis, the behavior of a typical dot was deduced. The
large effect of smearing on the values of umbral intensities and sizes
of umbral dots is discussed. This study considers the computed values
of radiative flux, as obtained from measured sizes and contrasts;
this parameter is presumably free of instrumental effects. An analytic
function is proposed to describe the time variation of some of the
umbral dots.

---------------------------------------------------------
Title: The solar granulation. I - Two dimensional power-spectrum
analysis using optical data processing methods
Authors: Koutchmy, S.; Legait, A.
1980A&A....88..345K Altcode:
Optical data processing methods are used to analyze a good time sequence
of selected high resolution solar granulation pictures obtained at
the Vacuum solar telescope of Sacramento Peak Observatory. Several
two-dimensional power spectra were composited and averaged by rotation
to deduce a statistically significant distribution. No regularities
appear on the deduced spectra. The speckles of partly instrumental
origin seen on individual two-dimensional power spectra are stable,
their characteristic life time being up to 7 min, indicating a similar
lifetime for solar granulation.

---------------------------------------------------------
Title: The effect of the equation of time on the 160-min solar
oscillation
Authors: Kozov, V. A.; Koutchmy, S.; Severnyi, A. B.; Tsap, T. T.
1980PAZh....6..421K Altcode:
If the Crimean and Stanford experiments to measure the sun's pulsations
of 160.010 m period (approximately 1/9 day) have actually recorded not
a solar oscillation but the ninth harmonic of a diurnal wave in the
terrestrial atmosphere, then the power spectrum and the exact value of
the period should depend on the equation of time (the difference between
true solar time and mean solar time). However, analysis of the Crimean
Doppler-shift measurements for 1974-1979 reveals no such relationship,
thereby supporting a solar interpretation of the 160.010 m period.

---------------------------------------------------------
Title: The Effect of the Equation of Time on the 160-MINUTE Solar
0SCILLATION
Authors: Kotov, V. A.; Koutchmy, S.; Severnyi, A. B.; Tsap, T. T.
1980SvAL....6..233K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Two-Dimensional Photographic Photometry of the Zodiacal Light
from Spatial Observations
Authors: Lamy, P. L.; Llebaria, A.; Koutchmy, S.
1980IAUS...90...37L Altcode:
No abstract at ADS

---------------------------------------------------------
Title: 2-D observations of IR-stellar speckles.
Authors: Lamy, P.; Koutchmy, S.
1979JOpt...10..331L Altcode: 1979JOp....10..331L
The first observations of speckle images of Alpha Orionis as obtained
at the Cassegrain focus of the 193-cm Telescope of the Haute Provence
Observatory using an IR-TV camera are discussed. The specific nature
of the 2-micron images is outlined.

---------------------------------------------------------
Title: Astronomical applications of infrared television imaging.
Authors: Lamy, P. L.; Nguyen-Trong, T.; Adjabschirzadeh, A.;
Koutchmy, S.
1979A&A....77..257L Altcode:
Infrared imaging between 1 and 2.4 microns was realized with a
television camera operated at the conventional video rate. A M2 star
of visual magnitude 5.6 was detected at 1.2 and 1.6 microns. Alpha
Ori was further observed at 2 microns and the corresponding smearing
function was found to improve with increasing wavelength. The image
structure (speckle) of Alpha Ori was visualized in the infrared and is
briefly characterized as compared to the visible. Solar observations
at 1.6 microns included direct imagery of sunspots and simultaneous
spectrography of the photosphere and sunspot umbra. The Zeeman splitting
of the 1.5648 microns Fe I line was observed and measurements are
shown to be possible on processed CRT pictures.

---------------------------------------------------------
Title: Comet West 1975n. I. Observations near and after perihelion
passage.
Authors: Koutchmy, S.; Coupiac, P.; Elmore, D.; Lamy, P.; Sevre, F.
1979A&A....72...45K Altcode:
Photographic observations of Comet West 1975n from a high altitude site
are reported. A small value of the absolute magnitude of the Comet 1.5
d after perihelion passage is deduced. Morphological characteristics
of the strongly structured dust tail are obtained, using a statistical
analysis based on the optical data processing of a transparency. The
deduced two-dimensional power spectrum is considered. The temporal
behavior of the main features of the tail is discussed using several
selected pictures.

---------------------------------------------------------
Title: Comet West 1975n part II: study of the striated tail.
Authors: Lamy, P. L.; Koutchmy, S.
1979A&A....72...50L Altcode:
The dynamical evolution of the striae in the tails of comet West
1975n is investigated. A synchrone-syndyne analysis of the overall
tail structure is attempted, but it is found that the classical
synchrone-syndyne description does not apply to the dynamical evolution
of the striae. A subsequent examination of the main properties of
the stria structure strongly suggests that all striae within a given
tail appear to originate from a synchronic edge. A scenario for
the formation of striae is proposed, according to which the bulk of
the dust constituting a tail is released at or around perihelion and
subsequently swept out under the influence of some unknown interaction
that organizes the dust into narrow streaks, or striae. It is concluded
that the unknown interaction involves the solar wind and a convected
magnetic field.

---------------------------------------------------------
Title: Salyut-6: a new look at the ionosphere.
Authors: Koutchmy, S.
1979Rech...10...63K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Observatoires en URSS: Description de quelques instruments
nouveaux
Authors: Koutchmy, S.
1978LAstr..92..433K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Photometrical analysis of the June 30, 1973 solar corona.
Authors: Koutchmy, S.; Stellmacher, G.; Koutchmy, O.; Dzubenko, N. I.;
Ivanchuk, V. I.; Popov, O. S.; Rubo, G. A.; Vsekhsviatskii, S. K.;
Lamy, P.
1978A&A....69...35K Altcode:
In order to deduce reliable values of the K and F coronal, a method
of photographic photometry has been applied to study compensated
high-resolution pictures obtained during the June 30, 1973, solar
total eclipse, including a color one. The correctly exposed images of
calibration stars are used to obtain intensities in units of the mean
brightness of the sun. An account is made, in both the blue and the
red spectral ranges, for the sky background as well as for the coronal
aureola effects. The N-polar and E-equatorial regions are shown to be
relatively homogeneous; their intensities are especially studied in
the radial direction and compared with published values of the K and F
coronae. No flattening and no color effect are found in the inner part
(distance less than 2.5 solar radii) of the F corona.

---------------------------------------------------------
Title: Bright points in sunspot umbrae: morphology, intensities.
Authors: Adjabshirzadeh, A.; Koutchmy, S.
1978CRASB.286..335A Altcode:
The bright point distribution in a sunspot umbra was determined by
applying precise photographic photometry to three photographic plates
obtained at time intervals of several minutes. The size and intensity
distribution along two orthogonal axes is examined. The distance
between bright points seems to be about 0.40 arcsec or about 300 km,
but if a correction is applied, the distance might be approximately
40 km. While the asymmetric distribution of the bright points seems
to indicate that the points have an elongated form, it is suggested
that the elongations are composed of a series of more or less circular
points which lie close together.

---------------------------------------------------------
Title: Propagating inhomogeneities in the dust tail of comet West 1975
Authors: Koutchmy, S.; Lamy, P.
1978Natur.273..522K Altcode:
COMET West has displayed some remarkable
properties. Sekanina1 has studied the multiple splitting
of its nucleus and also discussed the strange structure of its
dust tail. This tail is characterised by a system of bright bands
which do not correspond to the true synchronous band2 and
which are shown by very few comets. We call these striae (striated
tail) and to study them we have examined numerous original and
duplicate pictures, and selected four observations (Table 1) which
reveal that the morphology was relatively well conserved during the
evolution of the dust tail over a period of more than 4 days. We have
identified three striae (Fig. 1) which seem to propagate in space
while retaining their basic form. This phenomenon is not unusual in
plasmas, such as gas tails of comets3 or streamers in the
solar K-corona4,5. However, this is apparently the first
time that it has been observed in dust `clouds'. These striae, which we
describe here, are made of dust grains which can be readily demonstrated
by the wide-field colour photographs made by comet observers: the gas
tail (type I) appears distinctly blue because of CN emission and is
directly in the anti-solar direction as well as being well separated
from the large dust tail (type II) which has a neutral colour.

---------------------------------------------------------
Title: Photospheric faculae. II. Line profiles and magnetic field
in the bright network of the quiet sun.
Authors: Koutchmy, S.; Stellmacher, G.
1978A&A....67...93K Altcode:
Smnmary. Spatially high resolution spectra ( 0"75) of the three
iron lines. Fe 5576 A (non split), Fe 6301.5 A and Fe 6302.5 A
(triplet) observed in maguetic regions (network) of the quiet Sun,
were analysed. For the model computations, recent values of filigree
continuum contrast and diameter were used [1f/1P -18, 4) -0"24 (174
km), =6000 A]. High values of the maguetic field strength (10001500
Gauss) are found for the quiet network regions. A fit of the observed
profiles with the calculated proffles can be obtained only when a
strong maguetic field is also assumed in the intergranular regions
that surround the filigrees; the dimension of the magnetic field patch
is found to be structured and larger than that of the proper line gap
(ffligree). For the model calculations, a good fit is obtained when
the filigree width r is assumed to increase with height h as r =0.12
h+87 [km]. Key words: Sun - photo sphere - filigrees - facularpoints -
gap-profiles - concentrated magnetic fields

---------------------------------------------------------
Title: Workshop on cometary missions. ESOC Darmstadt, 17 - 19
April 1978. Chairmen's summaries and extended abstracts of invited
contributions.
Authors: Arpigny, C.; Bertaux, J. L.; Bodechtel, J.; Dalmann, B. -K.;
Fechtig, H.; Festou, M.; Giese, R. H.; Grün, E.; Haser, L.; Hughes,
D. W.; Ip, W. -H.; Jockers, K.; Keller, H. U.; Keppler, E.; Kissel,
J.; Koutchmy, S.; Krankowsky, D.; Lämmerzahl, P.; Lamy, P. L.;
Levasseur-Regourd, A. -C.; Lukoshhus, D.; Malaise, D.; Mariani, F.;
Michel, K. W.; Neukum, G.; Orfei, R.; Rosenbauer, H.; Röser, S.;
Schlude, F.; Schmidt, H. U.; Schubart, J.; Schwehm, G. H.; Sieber,
A.; Wänke, H.; Wallis, M. K.; Zerull, R. H.
1978wocm.book.....A Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Super Granulation in the Deep Photosphere
Authors: Koutchmy, S.
1978pfsl.conf..155K Altcode: 1978ESPM....2..155K
No abstract at ADS

---------------------------------------------------------
Title: Practical work on colour emulsions using filtered duplicates
Authors: Koutchmy, S.
1978mtap.conf..225K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Photospheric faculae: the contrasts at the center of the
solar disk using filigree pictures.
Authors: Koutchmy, S.
1977A&A....61..397K Altcode:
Summary. Fine structure of photo spheric faculae embedded
in intergranular lanes has been observed at the continuum
level. 2-dimensional restoration of the best filigree pictures obtained
by R. B. Dunn was tentatively achieved, using a Quasi-conventional
method of deconvolution and assuming largest values of the modulation
transfer function. The restored pictures show a typical filigree
contrast of 100 %, but we think that this limited restoration
gives only a lower limit to the actual constrast. Key words: solar
filigree - faculae - intergranular lanes - granulation two-dimensional
deconvolution - image processing - restoration

---------------------------------------------------------
Title: Etude polarimétrique de la couronne solaire observe a
l'èclipse totale du 30 juin 1973 à l'aide d'un filtre neutre radial.
Authors: Koutchmy, S.; Picat, J. P.; Dantel, M.
1977A&A....59..349K Altcode:
Photographs of the white-light solar corona were obtained during the
total solar eclipse of June 30, 1973 in two orthogonal components of
polarization. The total intensity and fraction of polarization of
the white-light corona were determined by means of a photographic
method and also by a numerical method of reduction of the plates
with a computer-controlled microdensitometer. The simple and quick
photographic method provided results which were in very good agreement
with the numerical ones. A procedure is described which permits the
total intensity and fraction of polarization of the K corona alone to
be computed and mapped, and a model for the transpolar coronal hole
is deduced.

---------------------------------------------------------
Title: Measurements of the solar limb-darkening in the 1 - 4 µm
range.
Authors: Koutchmy, S.; Koutchmy, O.; Kotov, V.
1977A&A....59..189K Altcode:
Radial scans in selected spectral regions near the opacity minimum,
in both equatorial and polar directions, have been performed for the
purpose of obtaining improved values for the limb darkening of the very
undisturbed quiet solar atmosphere. Equipment and correction procedures
are described. The new data are compared with earlier values, and the
HSRA model is found to be inadequate for predicting values near the
opacity minimum. The data are more in accord with the new model M of
Vernazza et al. (1976) and also with the BCA model. No pole-equator
difference of limb darkening due to the presence of faint faculae
was found.

---------------------------------------------------------
Title: Study of the June 30, 1973 trans-polar coronal hole.
Authors: Koutchmy, S.
1977SoPh...51..399K Altcode:
Radially and tangentially polarized pictures of the solar corona
obtained near 4500 Å during the 30 June, 1973 solar total eclipse
have been used to derive a model of a trans-polar coronal hole. The
hole is identified by using OSO-7 EUV spectroheliograms. The line of
sight coincides with the privileged plan of the hole over the N-polar
region. A new method of absolute calibration is used. The Saito (1970)
method is applied to determine the electron densities. Extrapolated
values of densities down to the surface are lower than have ever
been observed although derived hydrostatic temperatures are certainly
not: Ne × 107 cm−3 and T = 2 ×
106 K. The morphological peculiarities of polar regions
are considered.

---------------------------------------------------------
Title: The Contrast of Solar Filigrees
Authors: Koutchmy, S.; Stellmacher, G.
1977MitAG..42..142K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Solar Corona
Authors: Koutchmy, S.
1977ASSL...69...39K Altcode: 1977igss.conf...39K
White-Light Corona Ellipticity or Flattening Coronal Streamers Polar
Plumes Coronal Cavity Rifts Coronal Condensation and Enhancement
E-Corona or Emission Line Corona Coronal Loops EUV and X-Ray Corona
Magnetic Arcades Coronal Holes Coronal Bright Points Coronal Events
or Coronal Transients T-Corona Lyot-Coronagraph Externally Occulted
Coronagraph

---------------------------------------------------------
Title: Photometric study of chromospheric and coronal spikes observed
during the total solar eclipse of 30 June 1973.
Authors: Koutchmy, S.; Stellmacher, G.
1976SoPh...49..253K Altcode:
A photometric and colorimetric analysis of a color picture of the very
inner solar corona, near the South pole region, is performed. Dimensions
and average electron densities of both chromospheric and very fine
resolved coronal spikes are deduced. For the coronal spike a half
width of 1″.67 is measured, the estimate of electron density yields
ne = 1010 cm−3. Some conclusions
are attempted on the light of a simultaneously observed spectrum of
the same region which appeared to be a "disappearing coronal hole." The
observations seem to support the concept of a "striated" corona.

---------------------------------------------------------
Title: Comet West (1975n)
Authors: Sinvhal, S. D.; Babu, G.; Ketelsen, D. A.; Neff, J. S.;
Young, J.; Bortle, J.; Sekanina, Z.; Farrell, J. A.; Willmarth, D.;
Elmore, D.; Koutchmy, S.; Mayo, M. J.; Truxton, J.; Apeldoorn, B.;
Cosmovici, C.; Geyer, E. H.; Hoffmann, M.; Boyd, R.; O'Meara, S.
1976IAUC.2924....3S Altcode:
S. D. Sinvhal, Uttar Pradesh State Observatory, reports that
observations by G. Babu on Mar. 6.00 UT showed very strong Na emission,
strong Swan bands and detectable CN 3883 A and 4214 A and C3 4050
A; on Mar. 7.00 all emissions except the Swan bands had considerably
weakened. D. A. Ketelsen and J. S. Neff, University of Iowa, report that
observations of the nuclear region (resolution 16 A) on Mar. 7.5 showed
a strong continuum, strong emission features due to CN and C2 and rather
weaker emissions due to Na and C3. J. Young, Table Mountain Observatory,
reports the following visual tail lengths: Mar. 2.58 UT, &gt; 10o;
6.54, 25o; 7.55; 28o; 8.55, 30o. J. Bortle, Brooks Observatory,
reports the following observations of tail structure: Mar. 7.41 UT,
5o.5 long in p.a. 295o (a pair of gas tails); 8o.5 in 305o and 11o.5
in 310o and 19o in 330o (dust); 8.40, 8o.5 in 298o (gas), 11o in 307o
and 16o in 310o and 25o in 320o (dust). Corrigendum: on IAUC 2919,
the p.a. for the Feb. 29.47 observation should read 340o. Z. Sekanina,
Center for Astrophysics, comments on photographic observations of
the tail: "On photographs (4.5-cm f/4 camera, Royal Pan emulsion)
taken on Mar. 5.51 and 6.50 UT J. A. Farrell, Los Alamos, New Mexico,
noted a broad, dust tail composed of a number of 'synchronic bands',
similar to those observed in comet 1957 V; the breadth of the tail
had increased by the latter date, while the bands showed a systematic
translational motion of about 1o.6 per day and rotated at about 13o
per day relative to the faint plasma tail; Farrell also detected
two streamers superimposed on the dust tail, one of them essentially
coinciding with its southern border. On a print (f = 135 mm camera,
IIIa-J emulsion) obtained on Mar. 5.50 UT by D. Willmarth, Mount
Hopkins Observatory, I find the main body of the tail to be between
p.a. 310o and 357o, but a fainter glow can also be detected in the
north-northeast, apparently terminating in p.a. 40o; the bright section
of the dust tail consists of as many as 20 'synchronic bands', those
nearest the nucleus being directed toward p.a. 320o, the farthest ones
toward p.a. 330o; the most distant bands reach to at least 19o from the
nucleus, but traces of the dust tail extend out to some 25o. This bright
section of the dust tail consists of postperihelion particle emissions,
while the faint northeast section, which can be followed for a few
degrees, is made up of somewhat heavier particles emitted during the
week before perihelion. Willmarth's print also shows a plasma tail &gt;
15o long in the form of a 15o sector centered on p.a. 300o." D. Elmore
and S. Koutchmy, Sacramento Peak Observatory, report that daylight
photographic measurements on Feb. 26.81 UT at an effective wavelength
of 8750 A (passband 800 A) give an integrated magnitude of -3.65 +/-
0.40 (30' field). Selected recent total visual magnitude estimates:
Mar. 2.56 UT, 0 (M. J. Mayo and J. Truxton, Agoura, California, 7
x 50 binoculars); 3.23, 0 to -0.5 (B. Apeldoorn et al., Hoeven, The
Netherlands, naked eye); 4.2, 0 (C. Cosmovici, Lecce, Italy, naked eye);
5.55, &lt; 1.0 (Mayo and Truxton); 6.56, 1.2 (Mayo and Truxton); 7.41,
1.3 (Bortle, 10 x 50 binoculars); 7.56, 1.4 (Mayo and Truxton); 8.40,
1.8 (Bortle). Visual observations of secondary nuclei: Mar. 5.23 UT,
separation 3", p.a. 50o, magnitude difference 0.5 (E. H. Geyer and
M. Hoffmann, Hoher List Observatory, 36-cm refractor, 250 x); 7.46,
-, 120o, 0 (R. Boyd, Miami, Florida, 20-cm reflector, 210 x); 7.55,
4" 1 (Young, 61-cm reflector, 500 x); 8.40, &lt; 5", 340o, 1 (Bortle,
32-cm reflector, 100 x); 8.42, 1".5, 350o, 0.5 (S. O'Meara, Harvard
Observatory, 23-cm refractor, 300 x); 8.55, 2", -, - (Young).

---------------------------------------------------------
Title: JointSoviet-French studies of the solar corona. I. Structural
properties and photometry of solar corona of July 10, 1972
Authors: Vsekhsviatskii, S. K.; Dziubenko, N. I.; Nesmianovich, A. T.;
Popov, O. S.; Koutchmy, S.
1976SvA....19..477V Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Study of the Anti-Tail of Comet Kohoutek from an Observation
on 17 January 1974
Authors: Lamy, Ph. L.; Koutchmy, S.
1976LNP....48..343L Altcode: 1976IAUCo..31..343L
As part of our program of observation of Comet Kohoutek at Pic-du-Midi
observatory, we obtained, on January 17.8 UT, 1974 a photograph in
polarized light showing dramatically the (dust) antitail extending
for almost 1° from the Comet's head (reported in Sky and Telescope,
June 1974); indeed the comet is visible in polarized light further
away than in total light as noticed by Weinberg and Beeson (IAU
Colloquium No. 25, 1974) for Comet Ikeya-Seki. A photometric
and polarimetric study was performed (Bücher, A., Robley, R.,
and Koutchmy, S., 1975, Astron. Astrophys. 39, 289) showing that
the anti-tail is strongly polarized (up to 50 %). These large
degrees of polarization are of the same order of magnitude as those
reported for the tail of Comet Ikeya-Seki by Matjagin Sabitov and
Kharitonov (1967, Astron. Zh. 44, 1075) and by Weinberg and Beeson
(op. cit.). As discussed by these latter authors, particle alignment
is precluded as a significant contributor to polarization in the tail
of comets. Polarization by large spheres as obtained from the Fresnel
reflection coefficients applies only in the case of perfect surface,
a circumstance very unlikely in interplanetary space; the scattering
is in fact controlled by the surface microstructures (Van de Hulst,
private communication). Therefore we hypothesized that submicronic
grains should play an important role in the anti-tail. The classical
method of Finson and Probstein (1968, Astrophys. J. 154, 327, 353)
was used to draw the sky plane view of the syndynes for the day of
observation. Since the ratio β of the radiation pressure force to
the gravitational attraction is proportional to the third power of
the grains' radius s for ≲z 0.1 μ, submicronic grains with typical
radii of 0.02 μ may indeed be present in the anti-tail and provide a
straight-forward explanation of the observed polarization. This size
is of the same order of magnitude as that inferred for interstellar
grains which may well be embedded in the comet's nucleus as well as
meteorites for which there exists good evidence. Our conclusion does
not rule out the presence of millimeter-size grains as proposed by
Sekanina and Gary and O'Dell in their preliminary investigations (1974,
Icarus 23, 502, 519) which did not take into account the polarimetric
result; such grains may well coexist with the submicronic ones. Finally,
the line of maximum intensity is close to a synchrone corresponding to
a time of emission 100 days before perihelion passage. This supports
the synchronic formation of anomalous tails and possibly of tails as
proposed by Vsekhsvyatsky (1932, Astron. Zh. 9, 166).

---------------------------------------------------------
Title: Study of the Inner Satellites of Saturn by Photographic
Photometry
Authors: Koutchmy, S.; Lamy, P. L.
1975Icar...25..459K Altcode:
Good photographs of Saturn and its five inner satellites were obtained
on January 2, 1974 with the 105 cm telescope at Pic du Midi Observatory
with exposure times of 45 sec. The spread function is constant over the
field, and isotropic. The true photometric profiles of the satellites
are obtained after deriving a model for the stray light coming from the
rings. The magnitudes, computed by integration, are in good agreement
with published values except for Mimas, which is nearly one magnitude
fainter then previously believed.

---------------------------------------------------------
Title: Saturn's Rings: A Photometric Study of Ring C
Authors: Koutchmy, S.
1975Icar...25..131K Altcode:
A simple computational procedure is proposed for determining the true
photometric profile of ring C using the spread function obtained
from the satellite Dione and also slightly overexposed photographs
of Saturn. No trace of a faint additional ring between ring C and
the disk was found. The decreasing part, toward the planet, of the
recorded photometric profile of ring C exhibits a slight depression
tentatively attributed to a new division.

---------------------------------------------------------
Title: L'étude de la couronne blanche à bord de Concorde 001 au
cours de l'éclipse totale de Soleil du 30 juin 1973
Authors: Koutchmy, S.
1975LAstr..89..149K Altcode:
Preliminary preparations, essential results, and a narrative account
of the high-resolution coronal photography experiment conducted
aboard the Concorde 001 during the recent African solar eclipse are
presented. Scientific and other objectives of the study are considered,
the camera used is described, and the performance of the camera is
evaluated.

---------------------------------------------------------
Title: Dynamic processes in the solar corona of June 30, 1973
Authors: Vsekhsviatskii, S. K.; Dziubenko, N. I.; Nesmianovich, A. T.;
Rubo, G. A.; Koutchmy, S.
1975DoSSR.218..787V Altcode:
High-resolution photographs of the solar corona obtained during a
solar eclipse at two widely spaced points (time difference of 80
to 90 min between the photographs) are analyzed. It is shown that
following processes can occur during one hour in a solar corona whose
global structural characteristics are maintained during this period:
the formation and decay (or pronounced brightness variations) of such
medium-scale formations as polar rays, coronal jets, etc.; formation
and decay of distinct interfaces in the coronal structure; pronounced
shifts of coronal structures at speeds of several kilometers per second;
and separation of solar plasma concentrations, and their ejection from
the sun.

---------------------------------------------------------
Title: Photometric, Colorimetric and Polarimetric Study of Comet
Kohoutek 1973F, on January 17 and 18, 1974
Authors: Bucher, A.; Robley, R.; Koutchmy, S.
1975A&A....39..289B Altcode:
Summary. The photoelectric and photographic observations performed
on 17 and 18 January 1974 of the external parts of the comet Kohoutek
(1973 f) show that the color of the tail is much the same as the solar
color, and that the degree of polarization in the tail and anti-tail
is very strong. Observations of the anti-tail suggest similarity
in the properties with the zodiacal cloud dust. Key words: comet
Kohoutek 1973 F zodiacal light - photometry - polarimetry colorimetry
interplanetary dust

---------------------------------------------------------
Title: Investigation of dynamical processes in the solar corona on
30th June, 1973.
Authors: Vsekhsviatskii, S. K.; Dziubenko, N. I.; Nesmianovich, A. T.;
Rubo, G. A.; Koutchmy, S.
1974DoSSR.218..787V Altcode:
High-resolution photographs of the solar corona obtained during a
solar eclipse at two widely spaced points (time difference of 80
to 90 min between the photographs) are analyzed. It is shown that
following processes can occur during one hour in a solar corona whose
global structural characteristics are maintained during this period:
the formation and decay (or pronounced brightness variations) of such
medium-scale formations as polar rays, coronal jets, etc.; formation
and decay of distinct interfaces in the coronal structure; pronounced
shifts of coronal structures at speeds of several kilometers per second;
and separation of solar plasma concentrations, and their ejection from
the sun.

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Title: Study of low dispersion eclipse spectra: observation of weak
low excitation emission lines in the corona.
Authors: Stellmacher, G.; Koutchmy, S.
1974A&A....35...43S Altcode:
Summary. A spectroscopic experiment, set up to observe simultaneously
the electronic, emission line and F-corona, near the equator between
0.1 and 0.8 R0 above the sun's limb, was carried out successfully
during the total solar eclipse on June 30, 1973 in the Republic of
Tchad. The low excitation line emission in Ca+, H and K, H , H ,
H is observed superimposed over the entire spectrum, including the
lunar background. No radial dependence is observed for the equivalent
width of these lines. The emission is interpreted in terms of double
scattered light of chromospheric origin in the earth's atmosphere. The
color dependence of the double scattered light is correctly reproduced
by a quasi quantitative model confirming the parasitic origin of these
lines. Key words: sun - total solar eclipse chromospheric emission
lines double scattered parasitic light atmospheric optics

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Title: Infrared Photometry of the Outer Corona.
Authors: Lamy, Ph. L.; Koutchmy, S.
1974BAAS....6..311L Altcode:
No abstract at ADS

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Title: Observations photographiques de la comète Kohoutek
Authors: Koutchmy, S.
1974LAstr..88..172K Altcode:
No abstract at ADS

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Title: Photométrie photographique de la couronne solaire. Observée
au cours de l'éclipse totale du 10 juillet 1972
Authors: Koutchmy, S.; Dzubenko, N. I.; Nesmjanovich, A. T.;
Vsekhsvjatsky, S. K.
1974SoPh...35..369K Altcode:
No abstract at ADS

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Title: The coronal aureola in the time of total solar eclipse
Authors: Koutchmy, O.; Koutchmy, S.
1974A&AS...13..295K Altcode:
We propose a computational method allowing to obtain the intensity
of the coronal aureola from the measures of the solar aureola. The
method is applied to 2 very different observations performed at the
solar eclipses at Sept. 22, 1968 and March 7, 1970. In addition, a
scattering function is given for some typical cases observed (clear
sky) showing a large variety in values. We suggest to use this type of
function in order to describe the scattered light superimposed on the
lunar earthshine and the sky background. For good observing conditions,
we show that the coronal aureola is everywhere one order of magnitude
less than the but becomes higher than the minimum electronic corona,
for r &gt;2,5. When the sky background is important, especially because
of the low value of the eclipse magnitude, the intensity of coronal
aureola may be compared to the intensity. Key words: solar corona -
total solar eclipse - aureola effect - coronal model

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Title: Sur les premiers signes de la reprise de l'activité solaire.
Authors: Koutchmy, S.; Bareau, C.; Stellmacher, G.
1974CRASB.278..873K Altcode:
No abstract at ADS

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Title: Comet Kohoutek, 1973f.
Authors: Koutchmy, S.; Chernykh, N. S.; Kastel', G. R.; Pavlenko, P. P.
1974KomTs.169.....K Altcode:
No abstract at ADS

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Title: On the Observation of the F Corona in the Vicinity of the
Solar Limb
Authors: Koutchmy, S.; Magnant, F.
1973ApJ...186..671K Altcode:
Theoretical calculations led Calbert and Beard to predict a much
lower intensity of the F corona near the solar limb than the one
generally accepted. We show that this does not agree with recent
observations, especially airborne ones obtained far above the lower
atmosphere. The measurements made on the ground during the eclipse
of 1970 March 7 confirm the classical models. We suggest that new
observations should be made in order to allow a choice between the
apparently inconsistent interpretations of the measurements concerning
the external F corona. Subject heading: corona, solar

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Title: Rapid Variations Observed during the Total Eclipse of the
Sun on June 30, 1973
Authors: Koutchmy, S.; Fagot, J.
1973Natur.246..414K Altcode:
FOR nearly a century the solar corona has been considered responsible
for the interplanetary corpuscular radiation and in particular large
streamers have been thought to be the main source of this radiation.

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Title: French Eclipse Studies
Authors: Koutchmy, S.
1973S&T....46..215K Altcode:
No abstract at ADS

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Title: Etude photometrique d'un Renforcement Diffus observé dans la
Lumière Zodiacale, à une distance de 100 Rsun du Soleil
Authors: Banos, C.; Koutchmy, S.
1973Icar...20...32B Altcode:
A photograph of the zodiacal light obtained at the Pic du Midi
Observatory is studied in order to measure, in absolute units, the
brightness of the reinforcement, observed 15° above the ecliptic plan
and in a distance of 100R⊙ from the Sun. The obtained brightnesses
are compared to the brightness of the zodiacal light given by other
authors for the elongations ɛ ɛ [23°, 40°]. The calibration of
the image was made using the stars in the field of the image and
isophotes corrected for extinction were obtained, by the method of
isodensities. A discussion of the obtained results is made and the
origin of the reinforcement is investigated. The mass evaluation of
the interplanetary particles producing this reinforcement has been
estimated and permits to us to conclude that it may be due to particles
evaporated from the circumsolar region. The mechanism of transfer of
momentum to the particles in orbit around the Sun by a convecting ma
magnetic field is not elucidated.

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Title: On the origin and the dynamics of interplanetary dust.
Authors: Koutchmy, S. L.
1973pcp..conf...28K Altcode:
No abstract at ADS

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Title: Joint Soviet-French observations of the total solar eclipse
on July 10, 1972.
Authors: Vsekhsvyatskij, S. K.; Koutchmy, S. L.; Nesmyanovich, A. T.;
Dzyubenko, N. I.; Ivanchuk, V. I.; Rubo, G. A.
1973ATsir.789....1V Altcode:
No abstract at ADS

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Title: Observations of the total solar eclipse of June 30, 1973
according to the Soviet-French cooperation programme.
Authors: Vsekhsvyatskij, S. K.; Dzyubenko, N. I.; Nesmyanovich,
A. T.; Popov, O. S.; Rubo, G. A.; Koutchmy, S.; Bareau, C.; Begot,
J.; Fagot, J.
1973ATsir.800....1V Altcode:
No abstract at ADS

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Title: Étude hydrodynamique du grand jet coronal ne onserv&amp;eacute
à I'éclipse du 7 Mars 1970
Authors: Koutchmy, S.
1972SoPh...24..373K Altcode:
No abstract at ADS

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Title: Photometry of a Sunspot at ~ = 3.75 ~s
Authors: Coupiac, P.; Koutchmy, S.
1972A&A....16..272C Altcode:
Photometry of a Sunspot at = 3.75 A sunspot with an umbra of
16" (fig. 2) was observed in the N0 11145 MacMath plage during
Feb. 1971. The ccelostat of the Pic-du-Midi Observatory with an aperture
of 50 cm was used in the infra-red range. Good photometric scans
were obtained by spatial cancellation techniques using a modulation
frequency of 330 Hz and amplitudes &lt;4" with a 0.34 band pass filter
and InSb detector at a wavelength of 3.75 the spatial derivates of
the photometric sunspot profiles were calibrated by scanning the
extreme limb profile (Fig. 1). This technique offers the advantage
of permetting a very effective filtering of low frequency noise of
atmospheric origin. In this range a 0.60 + 0.03 (uncorrected for
the seeing) umbra photosphere contrast was obtained, this giving an
umbral temperature of 4200 + 120 K. This value is in agreement with
the computed predictions of the recent models of H6noux (1969) and
of Stellmacher and Wiehr (1970). We have used Bode (1965) diagrams
to deduce T (5000). Key words: Sun - sunspot - infrared photometry -
solar physic - spatial cancellation technique.

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Title: Contribution à l'étude de la couronne solaire en expansion.
Authors: Koutchmy, S.
1972PhDT........98K Altcode:
No abstract at ADS

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Title: Diffuise External Reinforcements in the Solar Corona from
the March 7 Solar Eclipse Plates
Authors: Koutchmy, S.
1972A&A....16..103K Altcode:
Observations of diffuse external reinforcements (renforcements externes
diffus or R.E.D.) during March 7th total eclipse are reported. The
reality of the R.E.D. is demonstrated by the agreement between the
results obtained using different methods and by different authors, all
these being shown in Table I. The morphology (Fig. 1) and brightness
distribution (Fig. 2) are studied. The visible light of the R.E.D. seems
to be either unpolarized or slightly polarized in a different way
than that, that would be predicted from Thompson scattering. Their
position angles appear well correlated with those of active regions
(Fig. 3). Two effects are proposed to explain the R.E.D.'s: a)wind or
magnetic field effects on circum-solar dust. b)ejection of neutral gas
similar to that of the "disparitions brusques" of the prominences. The
physical process giving the observed radiation from R.E.D. `s is not
elucidated. Many arguinents are given showing that the classical K
and F corona concept is insufficient to explain these observations,
i.e. the morphology, the relation with solar activity, polarization,
the lack of correlation with large coronal streamers, etc. Key words:
Sun-solar corona - circum-solar dust - gaz ejection - solar eclipse
- streamers

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Title: Observation in the Wing of the Hα Line and Identification
of the Spicular Structure near the Solar Limb
Authors: Koutchmy, S.; Macris, C.
1971SoPh...20..295K Altcode:
No abstract at ADS

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Title: Three Dimensional Model of a Large Coronal Streamer with
Active Region Enhancement
Authors: Koutchmy, S.
1971A&A....13...79K Altcode:
A large streamer (Fig. 1) has been studied photometrically (Fig. 8)
using some weighted plates obtained at the total eclipse of the
220d September 1968 in Siberia. The synoptic map as well as the green
coronal line observations are used (Figs. 4, 6a, 6b) for identification
with chromospheric structure. At the center, a coronal enhancement
rises above a well defined active region (Figs. 2, 3), around which a
650000 km diameter chain of quiescent prominances has been identified,
the streamer rising above the latter. This streamer is composed of
two parts: the bulb and "stalks". The proffles (Figs. 5, 7) show the
characteristic edge brightening and discontinuity (Fig. 17). A model of
the enhancement (Fig. 10) is given; typical value of electronic density
is 5- 108 at r = 1.15, in good agreement with radio observations. The
quasi-cylindrical edges of the large streamer form the bulb and
the measured photometrical proffles (Fig. 9) are well described by
electronic density distribution obtained by the formula: fle( r) =
n0(r) exp cc (P- )1 H( - , where cc-parameters take values given in
Table land the Heaviside function corresponds to the discontinuity;
the "stalks" are assumed to have a gaussian density distribution
perpendicular to their axis. The values of the edges density (Fig. 14)
are not so much higher than the double value of the Newkirk (1961)
active region coronal model; the streamer thickness at hall-height
of density distribution curve (Fig. 16) is about 30000 km at r = 1.5
and decreases to the sun surface. The differential edge brightening
is explained (Fig. 13); this confirming the validity of the model and
assumed geometry. The discontinulty is separately studied (Section 4)
with a model of linear decrease. Original results concerning the lower
limit of transversal gradient density are shown (Table 2); at r =
1.5 this gradient is in the order of 0.25 e-- , that is to say more
than 300 times the value of the radial gradient; interpretation is
proposed as a tangential discontinuity and a 0.8 Gauss longitudinal
magnetic field is found for r = 1.5; its decrease is stronger than the
sun center localized dipolar field. The life time of the discontinuity
is estimated (4-19) and the obtained values suggest that this thickness
can be considerably lower than the measured value, i.e. 4000 km at r =
1.5. Hydrostatic temperature for streamer's edges are lower than the
average whereas "stalks" give higher values (Fig. 15); in the central
area, above the enhancement, the density is lower, but temperature
seems abnormally high; this suggests a model of coronal streamer in
expansion with a heating source (Fig. 18) probably constituted by the
enhancement; the discontinnity shape confirms this model as well as
the application of the continuity equation (Fig. 19). Corpuscular
emission associated with the large streamer appeared clearly more
efficient than the spherical coronal models' one. The main results
are the identification of the large streamer and the enhancement with
underlying chromospheric fflaments and plages respectively (Section
2) the model of the streamer for which the lower part (bulb) has
a completely different structure compared with those of the models
rewiewed (Section 1) previously; the demonstration of the existence
of a tangential discontinuity (Section 4) and large magnetic fields
in the midcorona, and finally the confirmation of the dominant role
of the large streamer as a contributor to corpuscular emission (solar
wind). Key words: solar corona - streamers - enhancement - eclipse -
corpuscular emission - solar activity - solar wind

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Title: Observations and Discussions Concerning `High' Polarization
Features in the Solar Corona
Authors: Koutchmy, Serge; Schatten, Kenneth H.
1971SoPh...17..117K Altcode:
Photographic observations were obtained of the radial and tangential
polarization of the solar corona for the 1970, March 7, solar
eclipse. The corona was photographed using a neutral density filter and
rotating linear polaroid sectors to allow the polarization structure
to be seen from 1 to 6 solar radii. Anomalously high polarizations were
found for structures with the E-tangential intensity being predominantly
larger than the E-radial intensity. These structures are generally
filamentary in nature and radial in direction. One case with a high
radial polarization was also found. The photographs were calibrated
accurately against the Earth shine from the Moon. Possible source
mechanisms are discussed that may explain this new component in the
solar corona. Most sources may be ruled out on physical grounds. One
possibility appears to be synchrotron radiation from 10 GeV electrons
in a 0.4 G field. The existence of these electrons, however, is unlikely
in that spacecraft observations at 1 AU do not confirm their presence.

---------------------------------------------------------
Title: More March 7th eclipse results.
Authors: Lilliequist, C.; Schmahl, E.; Laffineur, M.; Koutchmy, S.;
Kanno, M.; Sinzi, A. M.; Saito, K.
1970S&T....40...77L Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Photometric Study of the Solar Corona
Authors: Koutchmy, S.; Laffineur, M.
1970Natur.226.1141K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Study of the Solar Continuum in the Intermediate Infra-Red
Spectral Range 3.5-24.4 4u
Authors: Koutchmy, S.; Peyturaux, R.
1970A&A.....5..470K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Observation de la lumière cendrée au cours d'une éclipse
totale.
Authors: Koutchmy, S.
1970CRASB.271..259K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Weighted Observation of the Corona during the Total Solar
Eclipse of September 22, 1968
Authors: Laffineur, M.; Burnichon, M. -L.; Koutchmy, S.
1969Natur.222..461L Altcode:
WE compare here the prediction of the coronal features made by
Schatten1 with the photographic observation made by us in
Yurgamish, Siberia.

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Title: The radio telescope for millimetre waves at the Simeis
Observatory.
Authors: Laffineur, M.; Koutchmy, S.
1969LOEle..49..246L Altcode:
No abstract at ADS

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Title: Sur un type nouveau de jet coronal associé à des éruptions
chromosphériques et à des "bulbes coronaux".
Authors: Burnichon, M. -L.; Koutchmy, S.; Laffineur, M.
1969CRASB.269..139B Altcode:
No abstract at ADS

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Title: Some Morphological Particularities of the Solar Corona on 22
September 1968
Authors: Koutchmy, S.
1969ApL.....4..215K Altcode:
No abstract at ADS