Author name code: rompolt
ADS astronomy entries on 2022-09-14
author:"Rompolt, Bogdan"
------------------------------------------------------------------------
Title: A confined prominence eruption on May 7, 1979
Authors: Duchlev, P.; Koleva, K.; Dechev, M.; Petrov, N.; Rompolt,
B.; Rudawy, P.
Bibcode: 2010BlgAJ..14...89D
Altcode:
A confined prominence eruption at the solar limb on 7 May 1979
associated with slow coronal mass ejection was observed and
reported. The aim was to probe the kinking of the eruptive prominence
(EP) loop and its relation to the processes coronal field confinement
on erupting flux rope. The EP represents helically writhed (kinked)
loop with fixed feet that presents a disturbed segment of a long-lived
filament, located within a multipolar magnetic configuration. The rising
of the EP apex and its velocity range suggest that the observation
span late stage of the eruption. In terms of magnetic flux rope
hypothesis, the kinking evolution of the EP flux rope was estimated by
the normalized difference between heights of the flux rope apex and
projected cross-point of its kinked legs, and the angle α between
the kinked legs below the cross-point. The results suggest that the
kink instability was in progress at the onset of observations and to
the end of the eruption, the EP flux rope presented a large amount
of kinking. Oscillations of the angle α with a period of 14 minutes,
accompanying its increasing, suggest oscillations of the EP flux rope
during the eruption. A possible scenario for confined eruption at the
limb on 7 May 1979 was suggested, in which a breakout-type reconnection
could occur above the EP but within a flux rope itself.
Title: Kinetics of the post-eruptive phase of an eruptive prominence
on 8 May, 1979
Authors: Duchlev, P.; Dechev, M.; Koleva, K.; Kokotanekova, J.;
Rompolt, B.; Rudawy, P.
Bibcode: 2010BlgAJ..13...69D
Altcode:
The kinetic pattern of the post-eruptive phase of the quiescent
prominence which erupted on 8 May, 1979, was studied. The eruption of
the helically-twisted polar prominence originated in the southern leg
of the huge magnetic system (HMS) that later produces a coronal mass
ejection (CME). The kinetic evolution of the post-eruptive process was
estimated by time profiles of the heights of the two main flux ropes
(FRs), composing the body of the eruptive prominence (EP) and the
horizontal expansion between the main FRs feet. The inflow velocity of
the prominence plasma back to the chromosphere increased with constant
acceleration of 76 m/s^{2} and it reached a value of up to 200 km/s. The
horizontal expansion between the main FRs feet of the EP increased with
an average constant velocity of 12 km/s in first order approximation,
but in fact it has changed non-linearly. The obtained results were
discussed as indicative ones for the kinetics and evolution of the
magnetic field at the bottom of the erupting HMS.
Title: Kinematics and evolution of eruptive prominences of two
different basic types
Authors: Duchlev, P.; Koleva, K.; Kokotanekova, J.; Dechev, M.;
Petrov, N.; Rompolt, B.; Rudawy, P.
Bibcode: 2010BlgAJ..13...47D
Altcode:
The kinematics and the evolution of three eruptive prominences (EPs)
observed in Wroclaw, Poland were studied. Two of them are classical
examples for the two basic different types of eruption (type I and type
II, according to Rompolt, 1984). Their basic kinematic characteristics
were compared and discussed from the point of view of their associations
with topologically different parts of the erupting huge magnetic
system. Some essential differences in their kinematics and evolution
were established. The kinematics and evolution of type I arch EP
of 5 May 1980 and the type II EP of 8 May 1979, associated with coronal
mass ejections (CMEs), are radically different. The arch EP of 5 May
1980, associated with fast CME, rose with increasing acceleration
up to its complete disappearing, while the eruption of the EP of
8 May 1979, associated with slow CME, was consisted of two phases:
acceleration and constant velocity. The eruption of EP of type II was
followed by a final, post-eruptive phase when the prominence plasma
fell back to the chromosphere. The EPs of types I and II showed two
kind of horizontal expansions (HE): large-scale, apparent horizontal
expansion and small-scale displacements between threads feet composing
the EP legs. These two kinds of HE are strongly distinguished for the
EP of type I. The large-scale expansion of the arch legs lasts up to
the end of the eruption and the alternative small-scale displacement
change of the threads feet in the arch legs is still present. The two
kinds of HE take place in two consecutive stages during the evolution of
the EP of type II. The first stage is characterized by an alternative
small-scale displacement change of the threads feet in the EP leg
occurred during the eruptive phase up to the full untwisting of the
EP body threads. Second stage is presented by a large-scale HE of the
fully untwisted threads occurred during the EP post-eruptive phase. The EP of 14 August 1979 associated with fast CME shows kinematics
and evolution of the eruption, as well as a horizontal expansion
very similar to these ones of the type II EPs. Some differences in
kinematic patterns of the EP of 14 August 1979 and those one of 8
May 1979 are probably due to its different topologies of the magnetic
field configuration (normal and inverse), as well as its association
with a different type of CMEs (fast and slow).
Title: Fine structure and Alfven string-mode oscillations of a
quiescent prominence
Authors: Petrov, Nicola; Duchlev, Peter; Rompolt, Bogdan; Rudawy, Pawel
Bibcode: 2007BlgAJ...9...93P
Altcode:
Series of Hα spectra and slit-jaw Hα filtergrams of a quiescent
prominence taken at Pic du Midi Observatory on November 7, 1977, are
studied. The image processing of the Hα filtergrams reveals an internal
structure of the prominence consisting of several arches. Series of
high-resolution Hα spectra obtained with the slit position located
on a selected part of one of the prominence arches have been chosen
for Doppler shift analysis. We got a good correspondence between the
prominence structural elements identified in the Hα filtergrams and
the corresponding spectral cuts. The prominence arch shows cyclic
displacement along the line-of-sight direction implying Alfvén
string-mode oscillations.
Title: Processing of the Eruptive Prominence Images
Authors: Koleva, K.; Duchlev, P.; Dechev, M.; Petrov, N.; Kokotanekova,
J.; Rompolt, B.; Rudawy, P.
Bibcode: 2006vopc.conf..317K
Altcode:
The films of eruptive prominences (EPs) registered at the Astronomical
Institute of the Wroclaw University, Poland (1979 and 1980 years)
were digitized with the automatic microdensitometer at the National
Astronomical Observatory Rozhen, Bulgaria. The basic algorithms for
processing of the digitized prominence images, determination of the
kinematic parameters (velocity and acceleration) of the EP, as well
as the dynamics and the evolution of the EP internal structure, are
considered. The same magnetic structure is thought to be involved in
the EPs and flares but at different spatial and energetic scales.
Title: Search for 1-10 Hz modulations in coronal emission with SECIS
during the August 11, 1999 eclipse
Authors: Rudawy, P.; Phillips, K. J. H.; Gallagher, P. T.; Williams,
D. R.; Rompolt, B.; Keenan, F. P.
Bibcode: 2004A&A...416.1179R
Altcode:
Results of the search of the periodic changes of the 530.3 nm line
intensity emitted by selected structures of the solar corona in the
frequency range 1-10 Hz are presented. A set of 12 728 images of the
section of the solar corona extending from near the north pole to
the south-west were taken simultaneously in the 530.3 nm (``green'')
line and white-light with the Solar Eclipse Coronal Imaging System
(SECIS) during the 143-seconds-long totality of the 1999 August
11 solar eclipse observed in Shabla, Bulgaria. The time resolution
of the collected data is better than 0.05 s and the pixel size is
approximately 4 arcsec. Using classical Fourier spectral analysis tools,
we investigated temporal changes of the local 530.3 nm coronal line
brightness in the frequency range 1-10 Hz of thousands of points within
the field of view. The various photometric and instrumental effects
have been extensively considered. We did not find any indisputable,
statistically significant evidence of periodicities in any of the
investigated points (at significance level α=0.05).
Title: Fine structure and oscillations of a quiescent prominence
Authors: Petrov, N.; Duchlev, P.; Rompolt, B.; Rudawy, P.
Bibcode: 2004IAUS..223..293P
Altcode: 2005IAUS..223..293P
Series of H_alpha spectra and slit-jaw H_alpha filtergrams of
a quiescent prominence (QP) taken at Pic du Midi Observatory on
7 November 1977 are studied. The image processing of the H_alpha
filtergrams reveals an internal structure of the prominence consisting
of several arches. Series of high-resolution H_alpha spectra obtained
with the slit located on selected parts of one of the prominence
arches chosen for Doppler shift analysis. The prominence arch show
cyclic displacement along the line-of-sight (L.O.S.) direction implying
Alfven string-mode oscillations.
Title: Relationship between solar radio spikes observed at 1420 MHz
and solar active phenomena
Authors: Dabrowski, B.; Rompolt, B.; Falewicz, R.; Rudawy, P.;
Siarkowski, M.
Bibcode: 2003ESASP.535..491D
Altcode: 2003iscs.symp..491D
Numerous solar radio narrow-band spikes have been observed with the
RT-15 radio telescope of Toruń Observatory between March 15, 2000 and
May 14, 2001. We present here a brief description of three interesting
events (from 11 events collected during 2000 hours of observations) and
first results of analysis of the relationship between the spikes, solar
flares and coronal mass ejections. We have found that solar spikes were
emitted from solar flares of various scenario of evolution and various
configuration of the interacting magnetic fields. Moreover, some groups
of spikes were not correlated in time with any solar flare recorded by
GOES or Yohkoh. It is very interesting to note, that on the basis of
the GOES database merely 2% of the solar flares emit the radio spikes.
Title: 3D evolution of an eruptive prominence of 15 May 2000 and
the associated active phenomena
Authors: Rudawy, P.; Cader-Sroka, B.; Rompolt, B.; Szuszakiewicz,
E.; Garczyńska, I.
Bibcode: 2003ESASP.535..507R
Altcode: 2003iscs.symp..507R
An eruptive prominence associated with solar flare and CME was observed
at the eastern part of the solar limb on 15 May 2000 with the Small
Coronagraph, Large Coronagraph and the MSDP (spectral imagery) of the
Astronomical Institute of the Wroclaw University. A 3D evolution of the
prominence was established on the basis of Hα images and spectra. The
same prominence was observed also by Karlický and co-authors 2001 with
a classical multi-camera spectrograph of the Ondrejov Observatory. The
presented report briefly compares the results of the both analyses
of the prominences' structure and evolution, obtained on the basis of
the classical spectroscopic and MSDP spectra-imagery data.
Title: Complex analysis of two eruptive events associated with CMEs
observed on 2 August 2000
Authors: Radziszewski, K.; Rompolt, B.
Bibcode: 2003ESASP.535..503R
Altcode: 2003iscs.symp..503R
We present the results of a detailed analysis of two eruptive events
associated with CMEs occurred at the eastern solar limb on 2 August
2000. The analysis was performed on the basis of observations taken
at the Astronomical Institute of Wroclaw University (Hα), SOHO/LASCO
(C2 and C3), SOHO/EIT (EUV), Pic du Midi (Hα) and Meudon (Hα and Ca
II). The first eruption which started at about 08:27 UT was associated
with a solar flare of GOES class C7.9 and produced a faint and not
very conspicuous CME. After this eruption a large quiescent prominence
situated to the North from the flare on the eastern limb, was activated
and strongly changed. The observed destabilization of the activated
prominence, evidently caused by the first eruption, brought about
to the eruption of this prominence and a large-scale CME. This second
eruption occurred at about 17:50 UT. After the C7.9 flare the GOES X-ray
level was rather low and oscillated between B7 and C1 through the next
twenty or so hours. This evidences that the second large-scale CME
was associated with the eruption of the prominence but not with a flare.
Title: Solar flares in active region NOAA 9042 on 21 June 2000
Authors: Rudawy, P.; Rompolt, B.; Falewicz, R.; Dabrowski, B.;
Siarkowski, M.
Bibcode: 2002ESASP.506..741R
Altcode: 2002svco.conf..741R; 2002ESPM...10..741R
During an analysis of the observations collected in the frame of
the year 2000 observing season we have found an interesting event
of two sympathetic flares in active regions NOAA 9042. Up to now we
have analysed visible, UV, X-ray and radio data taken on 21 June 2000
(observations taken between 05 UT and 14 UT). We have found that an
increase of the optical emission in the secondary flare occurred,
at least partially, as a consequence of the exchange of the kinematic
energy of the macroscopic motion of material, falling down onto the
chromosphere, into the thermal energy in the loop anchorage regions,
it means by the infall mechanism. The energy release of the primary
flare was associated by emission of numerous millisecond radio spikes
recoreded with the 80 μs time resolution.
Title: Search for short period coronal plasma oscillations. SECIS
results from 1999 and 2001 total eclipses
Authors: Rudawy, P.; Phillips, K. J. H.; Read, P.; Gallagher, P. T.;
Rompolt, B.; Berlicki, A.; Williams, D.; Keenan, F. P.; Buczylko, A.
Bibcode: 2002ESASP.506..967R
Altcode: 2002ESPM...10..967R; 2002svco.conf..967R
Results of the analysis of the high-cadence observations of the solar
corona, taken with the Solar Eclipse Coronal Imaging System instrument
during joint British-Polish expeditions during the total solar eclipses
of 1999 August 11 in Bulgaria (12768 images) and 2001 June 21 in Zambia
(16000 images) are presented. Using data collected during the both solar
eclipses we searched for possible periodic changes of the 530.3 nm line
intensity emitted by the selected points of the solar corona in the
frequency range up to 10 Hz. The time resolution of the collected data
is close to 0.05 sec and the pixel size is approximately 4 seconds of
arc. The standard photometric processing and correction of the image
motions caused by temporal drifts of the instrument pointing were
made. Using classical Fourier spectral analysis and wavelet analysis
tools we investigated temporal changes of the 530.3 nm coronal line
brightness of many thousands of points at various heights and position
angles above the solar limb. We did not find any statistically important
evidence of periodicity in the frequency range from 1 to 10 Hz in any
of the investigated points.
Title: Optical thickness and 3D dynamics of solar plasma in post-flare
loops
Authors: Radziszewski, K.; Rompolt, B.
Bibcode: 2002ESASP.506..729R
Altcode: 2002svco.conf..729R; 2002ESPM...10..729R
Results of analysis of two post-flare loops systems observed in Hα
line at the solar limb on 10 May 1998 are presented. The well-developed
post-flare loops systems appeared as a result of two M 1.6 and M 3.9
GOES class solar flares in the NOAA 8220 active region. We analysed
optical thickness and dynamics of separate blobs of the matter,
using MSDP Hα spectra and Hα high spatial resolution filtergrams
collected with the Large Coronagraph of Wroclaw University. The full
(3-dimensional) velocity vectors of the individual blobs, which moved
along the loops, were reconstructed on the basis of long series of
filtergrams and spectral-images. The optical thicknesses were evaluated
using Hα line-center images compiled from the MSDP data. The velocities
of the individual blobs moving along the loops were of the order of 20
- 60 percent of the free-fall velocity. The optical thicknesses were
equal to τ = 0.1-0.8, but when taking into account the influence
of the velocities on determination of the true value of the optical
thicknesses of the order of τ = 1.0-1.2.
Title: JOSO national report 2000-2001 - Poland
Authors: Rompolt, B.; Sylwester, J.
Bibcode: 2002joso.book...83R
Altcode:
In 2000-2001 investigations of the Sun in Poland were reported by:
The Astronomical Institute of Wroclaw University, The Solar Physics
Division of Space Research Centre of Polish Academy of Sciences,
The Astronomical Observatory of Jagiellonian University, Cracow.
Title: Interpretation of the MSDP Hα line profiles recorded during
the gradual phase of a solar flare
Authors: Berlicki, A.; Rudawy, P.; Rompolt, B.
Bibcode: 2002AdSpR..30..595B
Altcode:
In our paper we presented the results of analysis of Hα line profiles
emitted by some bright flaring structures observed during the gradual
phase of the C7.2 X-ray class flare. The flare was observed in NOAA 8088
active region on 25 September 1997 at 11:50 UT. We have used Hα line
spectra obtained with the Wrocław Multichannel Subtractive Double Pass
Spectrograph for all the points of the recorded field of view with the
temporal resolution of the order of 2 minutes. We analysed the time
evolution of the Hα profiles emitted by some selected structures of
the flare. We found that during the gradual phase of the flare the
Hα spectra exhibited mainly redshifts. The line of sight velocities,
corresponding to these shifts, did not exceed +13 km s -1. We
found that only few very small areas outside the flare structures
showed blueshifted spectra. Hα emission kernels located probably
close to X-ray loops footpoints also exhibited redshifted line
profiles. In contrast, the modelling made by Antiochos and Sturrock
(1978) as well as by Acton et al. (1982) predict the existence of a
"gentle evaporation" of plasma heated during the thermal phase of the
flares. Such a gentle upward motion of the chromospheric plasma should
produce mostly blueshifted profiles of the observed chromospheric
spectral lines (Schmieder et al., 1987).
Title: High-frequency oscillations in a solar active region coronal
loop
Authors: Williams, D. R.; Phillips, K. J. H.; Rudawy, P.; Mathioudakis,
M.; Gallagher, P. T.; O'Shea, E.; Keenan, F. P.; Read, P.; Rompolt, B.
Bibcode: 2001MNRAS.326..428W
Altcode:
The Solar Eclipse Corona Imaging System (SECIS) was used to record
high-cadence observations of the solar corona during the total solar
eclipse of 1999 August 11. During the 2min 23.5s of totality, 6364
images were recorded simultaneously in each of the two channels:
a white light channel, and the Fexiv (5303Å) `green line' channel
(T~2MK). Here we report initial results from the SECIS experiment,
including the discovery of a 6-s intensity oscillation in an active
region coronal loop.
Title: Line-of-Sight Velocity Fluctuations of a Quiescent Prominence
Authors: Dermendjiev, V. N.; Petrov, N. I.; Detchev, M. Tz.; Rompolt,
B.; Rudawy, P.
Bibcode: 2001SoPh..202...99D
Altcode:
Series of Hα spectra and slit-jaw Hα filtergrams of a quiescent
prominence taken at Pic du Midi Observatory on 7 November 1977
are studied. The observations have been digitized by means of an
automated Joyce Loebl microdensitometer. The image processing of the Hα
filtergrams reveals an internal structure of the prominence consisting
of several arches. Series of high-resolution Hα spectra obtained with
the slit position located on a selected part of one of the prominence
arches have been chosen for Doppler-shift analysis. The obtained time
series of the line-of-sight velocity reveal large velocity variations
near the periphery of the arch and a strong dependence of the velocity
(in sign and magnitude) on the position along the slit. The prominence
arch shows also cyclic displacements along the line-of-sight direction
implying Alfvén string-mode oscillations.
Title: Cornoal Heating by MHD Waves: Results from the SECIS Instrument
during the 1999 Eclipse
Authors: Phillip, K. J. H.; Gallagher, P. T.; Williams, D. R.; Keenan,
F. P.; Rudawy, P.; Rompolt, B.; Berlicki, A.
Bibcode: 2001IAUS..203..467P
Altcode:
We report on observational evidence for the rôles that small flare-like
events and short-period MHD waves play in the heating of the solar
corona. In several studies of SOHO and Yohkoh data, we examine the
numbers and energies of small events in the EUV and in soft X-rays
can account for the necessary energetics of the quiet-Sun corona,
finding that EUV events at least might be sufficient to provide the
heating, at least in closed-field regions. Results will be summarized
in this paper. However, MHD waves may still play an important part,
and in a separate investigation we have used fast-cadence imaging of
the white-light and green-line corona during the total eclipse of 1999
August 11 to search for short-period modulations. The imaging system
is the Solar Eclipse Coronal Imaging System (SECIS), and consists of a
pair of CCD cameras and an adapted PC to form images of the corona at
a frame rate of 44 s-1. Preliminary analysis of the data
suggests the presence of fast changes over the 2-minute-long period
of eclipse totality. This paper will also report on the SECIS data.
Title: Some Eruptive Events of Summer 2000 Observed at Wroclaw
Observatory
Authors: Garczynska, I.; Szuszakiewicz, E.; Rudawy, P.; Rompolt, B.;
Cader-Sroka, B.
Bibcode: 2001pre5.conf..487G
Altcode:
A number of energetic ejection events of the present maximum of Solar
activity were observed with the Small Cononagraph (SC), the Large
Coronagraph (LC) and the MSDP at the Wroclaw Astronomical Institute
during summer 2000. We observed the Eruptive Prominences (EPLs),
which gained considerable velocities and heights and showed also the
connection with intensive flares and Coronal Mass Ejections (CMEs). The
most interesting of them are presented, and possible relations to the
respective CMEs are discussed.
Title: SECIS: The Solar Eclipse Coronal Eclipse Imaging System
Authors: Phillips, K. J. H.; Read, P. D.; Gallagher, P. T.; Keenan,
F. P.; Rudawy, P.; Rompolt, B.; Berlicki, A.; Buczylko, A.; Diego,
F.; Barnsley, R.; Smartt, R. N.; Pasachoff, J. M.; Babcock, B. A.
Bibcode: 2000SoPh..193..259P
Altcode:
The Solar Eclipse Coronal Imaging System (SECIS) is an instrument
designed to search for short-period modulations in the solar corona
seen either during a total eclipse or with a coronagraph. The CCD
cameras used in SECIS have the capability of imaging the corona at a
rate of up to 70 frames a second, with the intensities in each pixel
digitised in 12-bit levels. The data are captured and stored on a
modified PC. With suitable optics it is thus possible to search for
fast changes or short-period wave motions in the corona that will
have important implications for the coronal heating mechanism. The
equipment has been successfully tested using the Evans Solar Facility
coronagraph at National Solar Observatory/Sacramento Peak and during
the 11 August 1999 eclipse at a site in north-eastern Bulgaria. The
instrument is described and preliminary results are outlined.
Title: Velocity Fluctuations in Oscillating Arch-type Quiescent
Prominences
Authors: Detchev, M. Tz.; Dermendjiev, V. N.; Petrov, N. I.;
Rompolt, B.
Bibcode: 1999ESASP.448..485D
Altcode: 1999ESPM....9..485D; 1999mfsp.conf..485D
No abstract at ADS
Title: Hα Spectral Observations of Bright Rim Underlying a Quiescent
Prominence on 10 June 1998
Authors: Rudawy, P.; Rompolt, B.
Bibcode: 1999ESASP.448..445R
Altcode: 1999ESPM....9..445R; 1999mfsp.conf..445R
No abstract at ADS
Title: Physical Characteristics of the September 23, 1998 Solar Flare
Authors: Kotrc, P.; Karlický, M.; Kupryakov, Yu. A.; Kaltman, T. I.;
Kasparova, J.; Rompolt, B.
Bibcode: 1999ESASP.448..841K
Altcode: 1999ESPM....9..841K; 1999mfsp.conf..841K
No abstract at ADS
Title: Analysis of evolution of NOAA 7912 active region on 19
October 1995
Authors: Rudawy, P.; van Driel-Gesztelyi, L.; Cader-Sroka, B.; Mein,
P.; Mein, N.; Schmieder, B.; Malherbe, J. -M.; Rompolt, B.
Bibcode: 1999A&AS..139...89R
Altcode:
An analysis of a minor (B3.2) flare related to an X-ray jet in the
reversed polarity NOAA 7912 active region is presented, focusing
on various kinds of activity observed in the Hα line with the MSDP
instrument. Using complementary Yohkoh soft X-ray observations and a
Kitt Peak magnetic field map we study the influence of a rather low
and graduate energy release on filaments, fibrils and chromospheric
brightenings and their relevant coronal features. We find that this
small flare affected the entire AR and was associated with strong up-
and downflows along remote fibrils and filaments, which appear to be
connected by large-scale loops. It is shown that at least one of the
observed brightenings was caused by downflow of the matter, thus, by
the kinematic heating of the material. The filament in the vicinity
of the flare footpoints changed the most: it broke into two parts,
temporarily rose to higher altitudes inside the AR and even erupted
outside of the AR, re-forming only three hours later. We show that
even a minor flare can lead to important morphological and dynamical
changes in an active region.
Title: Explosion in a loop on October 11, 1990.
Authors: Rompolt, B.; Falewicz, R.; Garczyńska, I.; Magun, A.
Bibcode: 1999joso.proc..180R
Altcode:
On October 11, 1990 the authors succeeded to observe an unusual
process of explosion occurring in an expanding loop (Rompolt,
1995). They present the results of a more detailed investigation
of this event. According to their knowledge such an event was never
observed before.
Title: Structure, internal motion and oscillation of a quiescent
prominence.
Authors: Dermendjiev, V. N.; Detchev, M.; Petrov, N.; Rompolt, B.
Bibcode: 1999joso.proc..122D
Altcode:
Series of Hα spectra and slit-jaw Hα filtergrams of a quiescent
prominence are studied. The prominence consists of several arches. One
of the arches oscillates with a frequency ω = 3·10-4s and
shows displacement of ±55.8 km in the line of sight direction. Its
internal velocity variations are larger near the periphery of the
arch. The sign and magnitude of the velocity depend strongly on the
position along the slit. For interpretation of these results a model
of secondary plasma flow generated by bending oscillation propagating
along the arch is developed.
Title: Analysis of besom-like ejections observed on June 9, 1998
during the MEDOC campaign.
Authors: Rudawy, P.; Rompolt, B.; Falewicz, R.
Bibcode: 1999joso.proc..182R
Altcode:
On June 9, 1998 the authors observed a series of recurrent besom-like
ejections of material from the vicinity of the huge quiescent prominence
being the target of the MEDOC June 1998 Campaign. An analysis of
these ejections based on MSDP spectral images and Hα filtergrams
is presented.
Title: Photospheric line-of-sight velocity field under quiet Hα
filaments.
Authors: Bumba, V.; Klvaňa, M.; Rompolt, B.; Rudawy, P.
Bibcode: 1999joso.proc..190B
Altcode:
The authors present some preliminary results concerning the positional
correlation of four active region Hα filaments in their quiet phase
with the photospheric line-of-sight velocity field lying beneath them,
measured with a scanning photoelectric magnetograph.
Title: Multi-wavelength observations of POST flare loops in two long
duration solar flares
Authors: Harra-Murnion, L. K.; Schmieder, B.; van Driel-Gesztelyi,
L.; Sato, J.; Plunkett, S. P.; Rudawy, P.; Rompolt, B.; Akioka, M.;
Sakao, T.; Ichimoto, K.
Bibcode: 1998A&A...337..911H
Altcode:
We have analysed two Long Duration solar Events (LDEs) which produced
large systems of Post Flare Loops (PFLs) and which have been observed by
Yohkoh and ground-based observatories. Using the Maximum Entropy Method
(MEM) image synthesis technique with new modulation patterns we were
able to make hard X-ray (HXR) images of the post flare loops recorded
in the L Channel (13.9-22.7 keV) of the Yohkoh Hard X-ray Telescope. We
obtained co-aligned 2-D maps in Hα (10(4) K), in soft X-rays (5x 10(6)
K) and in hard X-rays (20x 10(6) K). We conclude that the soft X-ray
(SXR) loops lie higher than the Hα loops and the former are overlaid
by HXR emission. This is suggestive of the magnetic reconnection
process. However some details are not consistent with the standard
models. Firstly the separation between the HXR source and the SXR
loop increases with time, with the HXR source being approximately
a factor of five larger than the equivalent source in impulsive
flares. Secondly the cooling times deduced from observations are longer
than the theoretically expected ones and the discrepancy increases
with time. We review the current models in view of these results.
Title: XIVth consultation on solar physics : conference proceedings
Authors: Rompolt, B.; Jakimiec, J.; Heinzel, P.
Bibcode: 1998PAICz..88.....R
Altcode:
No abstract at ADS
Title: Negative energy waves and the local brightening changes in
the solar prominences.
Authors: Detchev, M. T.; Dermendjiev, V. N.; Rompolt, B.
Bibcode: 1998joso.proc..143D
Altcode:
The authors construct and examine a simple model of local brightening
changes in a solar prominence thread in presence of negative energy
waves.
Title: Chromospheric Activity above Changing Photospheric Magnetic
and Velocity Fields of Developing Active Regions
Authors: Bumba, V.; Klvaña, M.; Kálmán, B.; Rompolt, B.; Rudawy, P.
Bibcode: 1998ASPC..155..224B
Altcode: 1998sasp.conf..224B
No abstract at ADS
Title: Horizontal Expansion of Eruptive Prominences
Authors: Rompolt, B.
Bibcode: 1998ASPC..150..330R
Altcode: 1998npsp.conf..330R; 1998IAUCo.167..330R
No abstract at ADS
Title: Rotational motion of material in surges
Authors: Rompolt, B.; Mińko-Wasiluk, A.; Berlicki, A.
Bibcode: 1998PAICz..88..225R
Altcode:
No abstract at ADS
Title: Prominence investigations at the Wroclaw observatory
Authors: Rompolt, B.
Bibcode: 1998PAICz..88..182R
Altcode:
No abstract at ADS
Title: Height variations of prominence plasma parameters
Authors: Kotrč , P.; Heinzel, P.; Vial, J. -C.; Rompolt, B.
Bibcode: 1998PAICz..88..208K
Altcode:
No abstract at ADS
Title: Internal motions and oscillatory phenomena in a quiescent
prominence.
Authors: Petrov, N. I.; Dermendjiev, V. N.; Rompolt, B.
Bibcode: 1998joso.proc..145P
Altcode:
The magnitude and variation of the internal motions in a quiescent
prominence are studied on the basis of long series of Hα spectra
and slit jaw Hα filtergrams obtained at Pic du Midi Observatory. A
discussion is made on the possible interpretation of the obtained line
of sight velocity.
Title: Evolution of a reversed polarity active region NOAA 7912 in
the photosphere, the chromosphere and the corona.
Authors: van Driel-Gesztelyi, L.; Baranyi, T.; Mein, N.; Cader-Sroka,
B.; Rudawy, P.; Mein, P.; Rompolt, B.; Schmieder, B.; Malherbe,
J. -M.; Willson, R.; Kile, J. N.; Raoult, A.
Bibcode: 1998joso.proc..103V
Altcode:
The authors follow the evolution and activity of NOAA 7912, a reversed
polarity region, in the photosphere (Kitt Peak magnetograms and Debrecen
white-light photoheliograms), chromosphere (MSDP instrument mounted
on the German VTT at Tenerife), and the corona (Yohkoh/SXT, Nançay
radioheliograph and the VLA) between October 12-20, 1995. They find
that in spite of the high shear and creation of several mixed-polarity
regions through flux emergence, the flares in the group did not
exceed the M-class level. This might be due to the fact that the
highly inclined bipolar fields emerging in the following part of the
primary reversed dipole were relatively small and quickly "consumed"
by cancellation enhanced by sunspot motions. On the other hand, the
presence of high shear and minor fast-moving parasitic polarities in
NOAA 7912 was sufficient to produce eruptive events like X-ray jets
with important coronal and interplanetary effects.
Title: X-Ray Jets and Their Radio Signatures at Metric and Centimeter
Wavelenths
Authors: van Driel-Gesztelyi, L.; Willson, R. F.; Kile, J. N.; Raoult,
A.; Klein, L.; Mein, N.; Rudawy, P.; Cader, B.; Rompolt, B.; Schmieder,
B.; Mein, P.; Malherbe, J. M.
Bibcode: 1998ASPC..154..707V
Altcode: 1998csss...10..707V
On October 19, 1995 at 10:30 UT and 17:00 UT, two semi-homologous X-ray
jets were observed with the Yohkoh/SXT from AR 7912, a region having a
reversed polarity group with vortex-like Hα fibril pattern and X-ray
loops. The jets appeared over a mixed magnetic polarity region in
the vicinity of the leading spot. The first event was also observed
with the Nancay radio heliograph at 167, 236, and 327 MHz. Type III
activity, indicating the presence of electron beams, superimposed on
a noise-storm was clearly visible. Type III activity first appeared
at 10:25 UT, coincident with the onset of the X-ray jet, at 164 MHz
and 236 MHz close to the storm position, and in the direction of the
X-ray jet. At 10:28:40 UT a new group of sources appeared eastward
of the former activity, which may correspond to another jet branch
along a more easterly path seen in the ohkoh} images. The second X-ray
jet event was also observed with the Very Large Array (VLA) at 6.2,
20.7, and 91.6 cm. For this event, VLA snapshot maps at 6.2 and 20.7
cm reveal low-brightness temperature changes in source structure at
the site of the X-ray jet during the preburst, impulsive, and decay
phases. The VLA 91.6 cm observations also show noise storm emission
above the active region but there is no clear temporal correlation
between this later X-ray jet and the impulsive decimetric bursts that
were observed during this period. Although the X-ray observations
show that the two jets had similar temperatures, emission measures,
speeds and trajectories they appear to have had dissimilar metric
responses to these events. This surprising result may question our
understanding of the process of electron beam acceleration in jets.
Title: Radio Emission Associated with Mass Ejection Events from
Active Regions of the Sun-Event of 1992 August 5
Authors: Garczynska, I. N.; Rompolt, B.; Raoult, A.; Cader-Sroka,
B.; Tomczak, M.
Bibcode: 1997pre4.conf..409G
Altcode:
This paper has been realized in the frame of the collaboration of
the Wroclaw and Nancay investigators. The spray, observed in Wroclaw
by means of the Small Coronograph, was connected with radio sources
observed by the Nancay Radioheliograph. The radio sources were situated
in two active regions; the first one - close to the spray and the
second one - far from it. The connection between these active regions
was confirmed by the YOHKOH-SXT image, where the giant magnetic loop
interconnecting them can be seen.
Title: Analysis of long duration flares
Authors: Harra-Murnion, L. K.; Plunkett, S. P.; Helsdon, S. F.;
Phillips, K. J. H.; van Driel-Gesztelyi, L.; Schmieder, B.; Rompolt,
B.; Akioka, M.
Bibcode: 1997AdSpR..20.2333H
Altcode:
Yohkoh has observed many long duration events permitting a statistical
study of the properties of these interesting events. We have selected
ten flares for analysis which have durations between 5 and 20 hours, and
size ranging from C to X GOES class. Employing the Soft X-ray Telescope,
the Bragg Crystal Spectrometer, GOES spacecraft, and ground-based
H_alpha data, we examine the morphology, temperature, emission measure,
location of the hard X-ray source, non-thermal velocities and upflows
of the plasma at different stages in the flare development. Our results
are used to address the question of the energy source that maintains the
hot plasma at temperatures of several million degrees for many hours.
Title: Fine structure of the sunspots penumbra and umbra observed
in Hα.
Authors: Rompolt, B.; Rudawy, P.
Bibcode: 1997joso.proc...78R
Altcode:
No abstract at ADS
Title: "Prominences, filaments and chromospheric activity" June 1996
campaign with SOHO, YOHKOH and Wrocław.
Authors: Wiik, J. E.; Rudawy, P.; Schmieder, B.; Kucera, T.; Rompolt,
B.; Poland, A.
Bibcode: 1997joso.proc...93W
Altcode:
No abstract at ADS
Title: Plasma velocity field of two quiescent prominences with
different morphology
Authors: Petrov, N.; Dermendjiev, V. N.; Rompolt, B.
Bibcode: 1997jena.confE..52P
Altcode:
We processed by means of the automated microdensitometer MDM6 Joyce
Loebl of the Institute of Astronomy of BAS series of H-alpha prominence
spectrograms taken with the Large Coronagraph of the Astronomical
Institute of Wroclaw University. The spectrograms were taken from two
quiescent prominence at various locations of the spectrograph slit
against the prominences bodies. The spectra represent a small part
(of about 15 AA) of the prominences spectra centered at H-alpha. The
corresponding range of the spectrum of the terrestrial atmosphere is
supperimposed on the spectrograms. Some of the atmospheric lines have
been used for determination of the wavelenght-pixel ratio and a point
of eparture, necessary in the procedure of computation of the H-alpha
emission location, H-alpha line profiles and the line-of-light velocity
components of the prominence plasma in the observed spectral range. In
the sequences of the H-alpha slit jaw filtegrams, taken simultaneosly
with the spectra, the slit position against the prominence body is
clearly seen. We got a good correspondence between the prominence
structural elements identified in the H-alpha filtegrams and the
corresponding spectral cuts. This permits us to construct isomaps of
the prominences line-of-sight velocity component. The obtained isomaps
are used for the analysis of the prominence plasma kinematics. Some
peculiarities in the velocity picture near the prominences surface is
explained as a result of the momentum transmission by the surface wave
modes of the supporting large scal local magnetic field.
Title: Evidence for prolonged acceleration based on a detailed
analysis of the long-duration solar gamma-ray flare of June 15, 1991
Authors: Akimov, V. V.; Ambrož, P.; Belov, A. V.; Berlicki, A.;
Chertok, I. M.; Karlický, M.; Kurt, V. G.; Leikov, N. G.; Litvinenko,
Yu. E.; Magun, A.; Minko-Wasiluk, A.; Rompolt, B.; Somov, B. V.
Bibcode: 1996SoPh..166..107A
Altcode:
Gamma-ray emission extending to energies greater than 2 GeV and lasting
at least for two hours as well as 0.8-8.1 MeV nuclear line emission
lasting 40 min were observed with very sensitive telescopes aboard
the GAMMA and CGRO satellites for the well-developed post-flare loop
formation phase of the 3B/X12 flare on June 15, 1991. We undertook
an analysis of optical, radio, cosmic-ray, and other data in order to
identify the origin of the energetic particles producing these unusual
gamma-ray emissions. The analysis yields evidence that the gamma-rays
and other emissions, observed well after the impulsive phase of the
flare, appear to be initiated by prolonged nonstationary particle
acceleration directly during the late phase of the flare rather than by
a long-term trapping of energetic electrons and protons accelerated at
the onset of the flare. We argue that such an acceleration, including
the acceleration of protons up to GeV energies, can be caused by
a prolonged post-eruptive energy release following a coronal mass
ejection (CME), when the magnetic field above the active region,
strongly disturbed by the CME eruption, relaxes to its initial state
through magnetic reconnection in the coronal vertical current sheet.
Title: Flare-like dynamic phenomena
Authors: Rompolt, B.; Švestka, Z.
Bibcode: 1996AdSpR..17d.115R
Altcode: 1996AdSpR..17..115R
Using data from Skylab, SMM, and Yohkoh spacecraft, as well as Hα
observations on the ground, we summarize the present knowledge about
dynamic phenomena on the Sun which usually are not classified as
flares, although they resemble processes observed in flares, often are
associated with flares, and sometimes can be considered for special
kinds of flares. This involves field openings outside active regions
(eruptive flares without chromospheric response), loop eruptions,
with emphasis on brightenings (and possibly eruptions) of loops which
interconnect active regions, sprays, flaring arches (injections of
hot and cool plasma into closed field configurations), Hα and X-ray
surges (injections of hot and cool plasma into `open' fields), X-ray
jets, recently discovered by Yohkoh, as well as Hα jets observed at
Wroclaw and Ottawa. We will try to find relationships between all the
latter phenomena so that one gets a more homogeneous picture of plasma
injections and jets observed on the Sun. There are many active phenomena
on the Sun which usually are not classified as flares, although they
closely resemble processes observed in flares, or are very often,
and quite typically, associated with flares. Some of them are even
caused by the same kind of instability that produces flares.
Title: New CCD-based guiding system for a Jensch-type coelostat.
Authors: Rudawy, P.; Rompolt, B.; Bogdan, M.; Szarapanowski, C.;
Szybiak, A.
Bibcode: 1996joso.proc..158R
Altcode:
No abstract at ADS
Title: Flare morphology.
Authors: Rompolt, B.
Bibcode: 1996joso.proc..112R
Altcode:
Some characteristic features of flare morphology derived from the
observations performed in the optical range of the electromagnetic
spectrum - mainly in Hα hydrogen line - are reviewed.
Title: Book reviews
Authors: Rompolt, B.; Sýkora, J.
Bibcode: 1995SoPh..159..207R
Altcode:
No abstract at ADS
Title: Book-Review - Reports on Astronomy - Transactions of the
International Astronomical Union - V.22A
Authors: Bergeron, J.; Rompolt, B.
Bibcode: 1995SoPh..159..207B
Altcode:
No abstract at ADS
Title: Material Ejection
Authors: Webb, David F.; Forbes, Terry G.; Aurass, Henry; Chen, James;
Martens, Piet; Rompolt, Bogdan; Rusin, Vojtech; Martin, Sara F.
Bibcode: 1994SoPh..153...73W
Altcode:
This paper reviews the major discussions and conclusions of the Flares
22 Workshop concerning the physical processes involved in mass ejecta
events, with an emphasis on large-scale phenomena, especially Coronal
Mass Ejections (CMEs). New insights have been gained from recent
data obtained from the SMM andYohkoh spacecraft and from several new
ground-based radio and optical instruments, as well as from theoretical
advances concerning the origins, driving mechanisms and long-term
evolution of CMEs.
Title: Energy Transport and Dynamics
Authors: Schmieder, B.; Peres, G.; Enome, S.; Falciani, R.; Heinzel,
P.; Hénoux, J. C.; Mariska, J.; Reale, F.; Rilee, M. L.; Rompolt, B.;
Shibasaki, K.; Stepanov, A. V.; Wülser, J. P.; Zarro, D.; Zharkova, V.
Bibcode: 1994SoPh..153...55S
Altcode:
We report findings concerning energy transport and dynamics in flares
during the impulsive and gradual phases based on new ground-based and
space observations (notably fromYohkoh). A preheating sometimes occurs
during the impulsive phase. CaXIX line shifts are confirmed to be
good tracers of bulk plasma motions, although strong blue shifts are
not as frequent as previously claimed. They often appear correlated
with hard X-rays but, forsome events, the concept that electron beams
provide the whole energy input to the thermal component seems not
to apply. Theory now yields: new diagnostics of low-energy proton
and electron beams; accurate hydrodynamical modeling of pulse beam
heating of the atmosphere; possible diagnostics of microflares (based
on X-ray line ratio or on loop variability); and simulated images of
chromospheric evaporation fronts. For the gradual phase, the continual
reorganization of magnetic field lines over active regions determines
where and when magnetic reconnection, the mechanism favoured for energy
release, will occur. Spatial and temporal fragmentation of the energy
release, observed at different wavelengths, is considered to be a
factor as well in energy transport and plasma dynamics.
Title: Relationship between magnetic field evolution and flaring
sites in AR 6659 in June 1991
Authors: Schmieder, B.; Hagyard, M. J.; Guoxiang, Ai; Hongqi, Zhang;
Kalman, B.; Gyori, L.; Rompolt, B.; Demoulin, P.; Machado, M. E.
Bibcode: 1994SoPh..150..199S
Altcode:
During the international campaign of June 1991, the active region AR
6659 produced six very large, long-duration flares (X10/12) during its
passage across the solar disk. We present the characteristics of four
of them (June 4, 6, 9, 15). Precise measurements of the spot motions
from Debrecen and Tokyo white-light pictures are used to understand the
fragmentation of the main sunspot group with time. This fragmentation
leads to a continuous restructuring of the magnetic field pattern
while rapid changes are evidenced due to fast new flux emergence
(magnetograms of MFSC, Huairou). The first process leads to a shearing
of the field lines along which there is energy storage; the second one
is the trigger which causes the release of energy by creating a complex
topology. We conjecture that these two processes with different time
scales are relevant to the production of flares.
Title: Tall Coronal Jets Seen Occasionally in H alpha
Authors: Rompolt, B.
Bibcode: 1994scs..conf..353R
Altcode: 1994IAUCo.144..353R
Some features of tall coronal jets observed at rare occasions in Hα
above the solar limb after the prominence eruptions are discussed. The
jets usually reach the height of a few hundred thousands kilometers
above the solar surface and exhibit filamentary structure.
Title: Evolution of an Eruptive Prominence and its Magnetic System
on 2 September 1991
Authors: Rudawy, P.; Rompolt, B.; Kotrič, P.; Heinzel, P.; Knižek,
M.; Garczyńska, I.; Cader-Sroka, B.
Bibcode: 1994emsp.conf...95R
Altcode:
No abstract at ADS
Title: Dragging out of the near-surface magnetic fields during the
prominence eruptions
Authors: Rudawy, P.; Rompolt, B.; Kotrč, P.; Heinzel, P.; Knižek, M.
Bibcode: 1994smf..conf..372R
Altcode:
No abstract at ADS
Title: The Mass Ejection Event of 1986 May 4 and the Associated
Phenomena
Authors: Garczynska, I. N.; Rompolt, B.; Aurass, H.; Burkepile, J. T.;
Cader-Sroka, B.; Cherlok, I. M.
Bibcode: 1994scs..conf..135G
Altcode: 1994IAUCo.144..135G
A sequence of structural changes in the low and high corona observed
in Hα and white light is investigated in details. Relatively slow Hα
mass ejections have been accompanied by X-ray and radio bursts as well
as CME. Some interconnections between all these events are analysed.
Title: Magnetic Field Reconnection Processes in Eruptive Prominences
Deduced from Hα Observations
Authors: Rompolt, B.
Bibcode: 1994emsp.conf..155R
Altcode:
No abstract at ADS
Title: Observational evidence for magnetic field reconnection in
active prominences
Authors: Rompolt, B.
Bibcode: 1994smf..conf..374R
Altcode:
No abstract at ADS
Title: Kinematics and evolution of twist in the eruptive prominence
of August 18, 1980
Authors: Vrsnak, B.; Ruzdjak, V.; Rompolt, B.; Rosa, D.; Zlobec, P.
Bibcode: 1993SoPh..146..147V
Altcode:
The prominence which erupted at the SE limb on August 18, 1980 is one
of the best observed disparition brusque events: high-resolution
monochromatic ground-based observations in the Hα line were
supplemented by the SMM and Solwind satellite coronographic
observations; the radio wavelength range was well covered by
single-frequency and spectral observations, and the prominence magnetic
fields were measured two days before the eruption.
Title: Book Review: Stellar atmospheres: beyond classical models /
Kluwer, 1991
Authors: Machado, M. E.; Rompolt, Bogdan; Kleczek, Josip; Jackson,
B. V.; Machado, M. E.
Bibcode: 1993SoPh..145..403M
Altcode: 1993SoPh..145..403C
No abstract at ADS
Title: Book Review: The sun: a laboratory for astrophysics /
Kluwer, 1992
Authors: Rompolt, B.
Bibcode: 1993SoPh..145..403R
Altcode: 1993SoPh..145..403S
No abstract at ADS
Title: Stability of Prominences Exposing Helical like Patterns
Authors: Vrsnak, B.; Ruzdjak, V.; Rompolt, B.
Bibcode: 1991SoPh..136..151V
Altcode:
The internal structure of prominences appearing as twisted tubes was
studied. The sample embraced 15 stable and 13 eruptive prominences,
exposing patterns which possibly reflect a helical configuration. The
equivalent pitch angles (ϑ) of twisted fine structure features were
measured. In some cases the evolution of the internal structure was
followed and 49 independent measurements of the parameter ϑ were
performed in total. The results are presented in the plane relating
the parameter ϑ and the normalized prominence height. The eruptive
prominences occupy the region characterized by ϑ > 50° and h
> 0.8d, where h and d are the prominence height and the footpoint
half-separation, respectively. All prominences characterized by h <
0.6d or by ϑ < 35° were stable. Such a result is in good agreement
with an order of magnitude treatment of the forces acting in a curved
magnetic tube, anchored at both ends in the photosphere.
Title: Radio signature and H-alpha limb features of the 1979 March
9 and 1982 July 9 flares
Authors: Aurass, H.; Krueger, A.; Rompolt, B.; Garczynska, I.;
Fomichev, V. V.; Chertok, I. M.; Ishkov, V. N.; Urbarz, H.
Bibcode: 1991AN....312..245A
Altcode:
A comprehensive compilation of data for both events is presented. Some
typical H-alpha limb and type IV radio spectrogram features are found
to be associated. The escape of matter out to loops visible in H-alpha
via blob ejection or loop eruption is associated with fast drift
burst signatures resp. early flare continuum (FCE) emission in radio
spectra and pulses in HXR. The comparison of both events reveals that
the metric radio-HXR association is essentially a matter of particle
escape conditions into the corona.
Title: Small Scale Structure and Dynamics of Prominences
Authors: Rompolt, B.
Bibcode: 1990HvaOB..14...37R
Altcode:
No abstract at ADS
Title: Dynamic Features of a Slowly Evolving Solar Proton Flare
Authors: Rompolt, B.; Urpo, S.; Aurass, H.; Krüger, A.
Bibcode: 1990PDHO....7..206R
Altcode: 1990dysu.conf..206R; 1990ESPM....6..206R
The authors present a study of optical and radio observations of
a limb flare on 10 May 1981. The evolution of the flare volume and
related dynamical processes provide interesting information about a
characteristic example of a class of big slowly evolving flare events.
Title: Solar and interplanetary observations of the mass ejection
on 7 May, 1979
Authors: Jackson, Bernard V.; Rompolt, Bogdan; Svestka, Zdenek
Bibcode: 1988SoPh..115..327J
Altcode:
We present observations of a mass ejection that was observed by five
different instruments along its way from the solar surface to more
than 100 solar radii. The instruments involved are the ground-based
Hα coronagraph at Wrocław, the white-light SOLWIND coronagraph on
board the P78-1 satellite, zodiacal light photometers of the HELIOS
B spacecraft, in situ plasma detectors and magnetometers on board the
HELIOS B spacecraft, and interplanetary scintillation measurements on
the ground. By using a CAT-scan analysis of the images obtained by the
SOLWIND coronagraph near the Earth and HELIOS B photometers placed at
0.3 AU perpendicular to the Earth-Sun line, we have been able to get a
three-dimensional density reconstruction of the mass ejection and fit
the best velocity curve for its propagation. Although problems exist
in smoothly joining the height-time curves (for instance, we had to
reduce the brightness of the SOLWIND data by more than a factor of two
to make the data sets agree photometrically), both this analysis and
direct measurements by the other experiments clearly indicate higher
speeds at greater distances from the Sun. The plasma acceleration
in this case was obviously not limited only to distances within 3
R0, as is usually the case, but continued beyond the outer
limit of the coronagraph view at ∼ 8 R0.
Title: X-ray emission associated with solar prominences, sprays
and surges
Authors: Harrison, R. A.; Rompolt, B.; Garczynska, I.
Bibcode: 1988SoPh..116...61H
Altcode:
Using Hα observations made at the Astronomical Observatory of Wroclaw
University, and 3.5-5.5 keV X-ray data from the Hard X-ray Imaging
Spectrometer on board the Solar Maximum Mission, sites of solar X-ray
emission are identified which are associated with active Hα features,
such as prominences, sprays and surges. The X-ray emission is found to
be highly localized within the active (Hα) structures. For example,
in the prominences examined, 3.5-5.5 keV X-rays were found only in
compact sites near the feet of the prominences. Models predicting that,
during the active phase of these structures, the energy release should
be evenly distributed along the structure are clearly brought into
question. It is argued that these X-ray sites are indicative of the
cause of the expulsion and transport of chromospheric material. Models
which satisfy these observations are discussed.
Title: Formation and eruption of quiescent prominences.
Authors: Rompolt, B.
Bibcode: 1988dssp.conf..125R
Altcode:
On the basis of detailed investigations of high-resolution Hα-images of
quiescent prominences seen on the solar limb under various orientation
with respect to the line of sight, a dynamic model for the formation
of these prominences has been derived. Three possibilities for the
eruption of the quiescent prominences are discussed.
Title: Characteristics of the Expansion Associated with Eruptive
Prominences
Authors: Athay, R. G.; Low, B. C.; Rompolt, B.
Bibcode: 1987SoPh..110..359A
Altcode:
Gradients of Hα and electron scattering intensities derived from
instantaneous radial distributions of erupting prominence material
observed at several solar radii by Illing and Athay (1986) are often
markedly smaller than those inferred by comparing the intensities
observed near several radii to average prominence intensities
observed near the limb. In this paper, we show that gradients derived
by following individual features in their outward progression with
time yield values that are consistent with limb observations and that
usually exceed the values obtained from instantaneous distributions. We
conclude from the diversity of observed gradients that the prominence
eruption cannot be described by a self-similar expansion in which the
expansion velocity is a function of radius and time only. However,
we cannot rule out possible self-similar solutions that allow the
expansion velocity to be a function of angular direction.
Title: On the association of erupting magnetic fields with eruptive
prominences and coronal mass ejections
Authors: Rompolt, Bogdan
Bibcode: 1987sici.symp...21R
Altcode:
A number of space and ground-based observations give evidence that the
eruptive prominences, coronal mass ejections (CMEs) and associated
shocks are generated by a common cause, i.e., the eruption of the
magnetic field on the Sun. Some 60% of the observed CMEs are associated
with the eruptive prominences. It is believed that in reality a
much better correlation should be between these events because of
observational limitations and of the effect of partial eruption. Some
recent results on the formation and evolution of the quiescent and the
active region prominences give an idea on the early phase of eruption
of the magnetic field with the prominence plasma frozen in. In the
latter phase of eruption the magnetic field lifted high into the
corona and is seen (as manifested by the cold plasma frozen in) as
a system of huge loops - evidently the result of some reconnections
at lower heights. The legs of these erupting loops interact sometimes
with the local magnetic field, i.e., it often appears to be an active
region. In consequence of this interaction the activation of prominences
and generation of flares can take place on some occasions as well as
ejection of surges and sprays.
Title: Hydrogen Emission from Moving Solar Prominences
Authors: Heinzel, P.; Rompolt, B.
Bibcode: 1987SoPh..110..171H
Altcode:
Brightness variations of the lines arising from a five-level hydrogen
model atom, depending upon prominence velocities, have been investigated
using a combination of two non-LTE techniques. The importance of the
Doppler brightening and/or Doppler dimming effects is demonstrated
for the lines of the Lyman and Balmer series.
Title: Formation and Eruption of Quiescent Prominences
Authors: Rompolt, B.
Bibcode: 1987dssp.work..125R
Altcode: 1987ASSL..150..125R
No abstract at ADS
Title: Solar and Interplanetary Observations of the Mass Ejection
on 7 May 1979
Authors: Jackson, B. V.; Rompolt, B.; Svestka, Z.
Bibcode: 1987sowi.conf..272J
Altcode:
No abstract at ADS
Title: Non-LTE hydrogen-line formation in moving prominences.
Authors: Heinzel, P.; Rompolt, B.
Bibcode: 1986NASCP2442..163H
Altcode: 1986copp.nasa..163H
The behavior of hydrogen-line brightness variations, depending on the
prominence-velocity changes were investigated. By solving the NON-Local
thermodynamic equilibrium (LTE) problem for hydrogen researchers
determine quantitatively the effect of Doppler brightening and/or
Doppler dimming (DBE, DDE) in the lines of Lyman and Balmer series. It
is demonstrated that in low-density prominence plasmas, DBE in H alpha
and H beta lines can reach a factor of three for velocities around 160
km/sec, while the L alpha line exhibits typical DDE. L beta brightness
variations follow from a combined DBE in the H alpha and DDE in L alpha
and L beta itself, providing that all relevant multilevel interlocking
processes are taken into account.
Title: On the formation of active region prominences (Hα filaments).
Authors: Rompolt, Bogdan; Bogdan, Thomas
Bibcode: 1986NASCP2442...81R
Altcode: 1986copp.nasa...81R
Analysis of sequential Hα images of active region prominence formation
suggests that simple large-scale photospheric mass-motions may play
a key role in the formation of these long, thin, Hα filaments.
Title: Energy Interconnection Between the Plasma Cloud Ejected from
the Active Region and the Shock Wave
Authors: Garczynska, I. N.; Rompolt, B.
Bibcode: 1986SoPh..105..101G
Altcode:
The relation between the ejected plasma cloud and the shock wave
propagating ahead of it is examined for 27 pairs of such events. The
flare sprays and the eruptive prominences observed in Hα line as
well as the fast-moving sources of type-IV radio bursts have been
considered as such ejected plasma clouds. Propagation of the shock
wave in the solar corona has been examined from the observations of
type-II radio bursts. Using the Parker model of the propagation of a
shock wave, the shock wave velocity has been compared with the plasma
cloud velocity. Energy interconnection between these two events has
been studied. In the majority of the investigated cases there exists an
energetic interconnection between the plasma cloud and the shock wave.
Title: Correspondence of cold mass motion and radio signatures in
the events of 9 March 1979 and 9 July 1982
Authors: Aurass, H.; Krüger, A.; Garczinska, I.; Rompolt, B.
Bibcode: 1986CoSka..15..649A
Altcode:
A study of characteristic stages of flare development in Hα and
radio was made for two complex limb events. By means of coronograph
observations (Wroclaw) and radio observations (Tremsdorf) general
conclusions were drawn on the temporal correspondence of signature of
optically visible mass ejection and radiation from hot flare matter.
Title: Non-LTE models of solar prominences
Authors: Heinzel, P.; Vial, J. C.; Gouttebroze, P.; Rompolt, B.
Bibcode: 1986CoSka..15..183H
Altcode:
The authors briefly review some representative non-LTE models of solar
prominences, developed during the past decade. Particular attention is
devoted to recent interpretation of hydrogen Lyman α line profiles
in quiescent prominences and to the solution of the non-LTE problem
for moving active prominences. Finally, the authors outline some of
the most important prospects of prominence plasma diagnostics.
Title: Fast objected events, observed in H-alpha and associated with
them coronal mass ejections (CME) and interplanetary shocks
Authors: Rompolt, B.; Garczynska, I. N.
Bibcode: 1986CoSka..15..691R
Altcode:
The regular observations of the fast ejected events (eruptive
prominences, eruptive loops, sprays and surges) were carried out at
the Astronomical Observatory of the Wroclaw University by means of the
Small Hα Coronograph in the years 1978 - 1984. A number of bright
material ejections have been observed. Some of them were associated
with the coronal mass ejections (CME) and interplanetary shocks.
Title: Optical and microwave observations of limb flares in the Hale
region 17644 on May 10, 1981
Authors: Rompolt, B.; Rudawy, P.
Bibcode: 1986CoSka..15..667R
Altcode:
No abstract at ADS
Title: Microwave emission from the limb of the Sun: the events of
September 8, 1980 and May 10, 1981
Authors: Urpo, S.; Terasranta, H.; Ruzdjak, V.; Vrsnak, B.; Rompolt,
B.; Kren, G.
Bibcode: 1985HvaOB...9...25U
Altcode:
Solar microwave maps at 8 mm performed at the Metsähovi Radio
Research Station in the period 1978 - 1982 revealed some radiation
sources located up to 50000 km outside the optical Sun. The authors
describe two characteristic events which were associated with large
flares occurring close to the solar limb.
Title: The 530 mm coronograph of the Wrocław University.
Authors: Rompolt, B.; Rudawy, P.
Bibcode: 1985PoAst..33..141R
Altcode:
The large Lyot-type coronograph of the Astronomical Institute of the
Wrocław University is described. Aperture of the single lens objective
is 53 cm, effective focal length 14.5 m. The coronograph is equipped
with a coudé spectrograph and a system of Hα filters. The angular
resolving power of the high quality images is not less than 0arcsec.5.
Title: Energetics and Interplanetary Effects of the August 14 and 18,
1979 Solar Flares: Summary of Observations Made during the Smy/stip
Event no.
Authors: Kane, S. R.; Bird, M. K.; Domingo, V.; Gapper, G. R.; Green,
G.; Hewish, A.; Howard, R. A.; Iwers, B.; Jackson, B. V.; Koren, U.;
Kunow, H.; McGuire, R. E.; Muller-Mellin, R.; Rompolt, B.; Sanahuja,
B.; Sawant, H. S.; Stewart, R. T.; von Rosenvinge, T.; Wibberenz,
G.; Zlobec, P.
Bibcode: 1984sii..conf..175K
Altcode:
No abstract at ADS
Title: Eruption of huge magnetic systems from the sun
Authors: Rompolt, B.
Bibcode: 1984AdSpR...4g.357R
Altcode: 1984AdSpR...4..357R
A number of evidences is presented supporting an idea that both the
eruptive prominences as well as the associated white light transients
are generated by eruptions of a huge magnetic field system from the
solar surface. The presented opinion is based on a detailed comparison
of the geometry, the characteristic features during the expansion
and the location on the limb of the white light transients recorded
by coronographs on board of the SKYLAB, P-78 and SMM satellites, with
the eruptive prominences observed in Hα at the Wroclaw Astronomical
Observatory.
Title: Observations and interpretation of a set of limb events of
September 2, 1979.
Authors: Paciorek, J.; Ciurla, T.; Rompolt, B.
Bibcode: 1983PDHO....5..531P
Altcode: 1984PDHO....5..531P
A number of active phenomena, that appeared above the West-limb from S37
to N15 were observed and analysed. Most of the elementary events were
recorded in two limb regions. In the first one, between N02 and N05,
forty recurrent surges and an active prominence were observed. In the
second one, between S30 and S37, about fifty knots of matter moving
down were recorded. The detailed study of all observed events suggest
the existence of a physical connection between these two distant
limb regions.
Title: Hα limb phenomena observed at the Wrocław Astronomical
Observatory between 17 - 22 of May, 1981.
Authors: Rompolt, B.; Garczyńska, I. N.
Bibcode: 1983ITABO..57..209R
Altcode:
No abstract at ADS
Title: Hα limb phenomena and solar noise storms.
Authors: Rompolt, B.
Bibcode: 1983srs..work..291R
Altcode:
From a recent investigation of the correlation of Hα limb surges with
radio bursts it appears that the surges which are not accompanied by
flares have a strong tendency to coincide with type I radio bursts
with drifting chains. Such a correlation does not exist for the surges
accompanied by flares.
Title: The card index of ejections observed at the Wroclaw
Observatory.
Authors: Garczyńska, I. N.; Majer, P.; Rompolt, B.
Bibcode: 1983PDHO....5..543G
Altcode: 1984PDHO....5..543G
The regular observations of the solar corona have been carried out at
Astronomical Observatory of the Wroclaw University by means of the
Small Hα Coronagraph since 1966. A number of ejections of bright
material (sprays, surges and eruptive prominences at the limb) have
been observed. Some of these events have already been analysed, and the
results were published. Recently a homogeneous method of treatment of
the observations has been devised and a card index of strong ejections
has been initiated.
Title: Compression of the Venusian ionosphere on May 10, 1979, by the
interplanetary shock generated by the solar eruption of May 8, 1979
Authors: Dryer, M.; Perez-de-Tejada, H.; Taylor, H. A., Jr.;
Intriligator, D. S.; Mikalov, J. D.; Rompolt, B.
Bibcode: 1982JGR....87.9035D
Altcode:
An interplanetary shock wave that was produced by a solar
eruption and its associated coronal transient on May 8, 1979,
has been `tracked' through interplanetary space to a rendezvous 2
days later with Venus. The interaction of the shock wave with the
ionospheric obstacle at Venus produced a significant compression of
the dayside ionosphere. It is believed that the tracking, as it were,
was accomplished for the first time via the diagnostic observations
provided by Hα and white light imagery near the sun and the plasma
and field measurements of two, nearly radially aligned, spacecraft.
Title: The Relation Between the Surges and Solar Radio Emission
Authors: Garczynska, I. N.; Rompolt, B.; Benz, A. O.; Slottje, C.;
Tlamicha, A.; Zanelli, C.
Bibcode: 1982SoPh...77..277G
Altcode:
The 120 limb surges which have been observed by means of Wrocław
Observatory coronagraph from September 1966 to November 1977 are
investigated. The evolution of surges was compared with the radio
data during the surges. A correlation between radio bursts and the
surges was found, particularly with chains of type I radio bursts,
which is the first reliable correlation found of these bursts with
non-radio events. The type I correlation only applied for surges
without accompanying flare, of which 43% are correlated with this type
of radio emission. In 23 of 30 associated events the start of a surge
coincided within 5 minutes with the start or an enhancement of the type
I storm. If flares were present, the association was not significant.
Title: Hα limb phenomena and solar noise storms
Authors: Rompolt, B.
Bibcode: 1982srs..work..291R
Altcode:
No abstract at ADS
Title: The Solar Origin of An Interplanetary Shock
Authors: Sheeley, N. R., Jr.; Howard, R. A.; Koomen, M. J.; Michels,
D. J.; Rompolt, B.; Schwenn, R. W.; Mihalov, J. D.
Bibcode: 1980BAAS...12..920S
Altcode:
No abstract at ADS
Title: Doppler dimming of active prominences in hydrogen Ly-alpha line
Authors: Rompolt, B.
Bibcode: 1980HvaOB...4...55R
Altcode:
No abstract at ADS
Title: Doppler brightening effect in H-alpha line for opticaly thin
moving prominences
Authors: Rompolt, B.
Bibcode: 1980HvaOB...4...39R
Altcode:
No abstract at ADS
Title: The solar mass ejection of 8 May 1979
Authors: Michels, D. J.; Howard, R. A.; Koomen, M. J.; Sheeley, N. R.,
Jr.; Rompolt, B.
Bibcode: 1980IAUS...91..387M
Altcode:
The solar mass ejection of May 8, 1979 is characterized using images
from the NRL SOLWIND coronagraph on board the P78-1 satellite. The
eruption of the polar crown filament began at about 0810 UT and reached
maximum distance of 1.5 solar radii from the center of the sun at 1021
UT. The eruptive prominence subsequently faded, and some of the material
fell back to the solar surface. Vestiges of the H-alpha prominence
disappeared by 1120 UT. The bulk of the prominence material displayed
radial velocities averaging 40 km/sec with 165 km/sec the maximum
velocity observed. From 1028 UT to 1246 UT, the leading edge of the
ejecta moved outward with a constant radial velocity of approximately
500 km/sec. Projected back to the solar limb, this indicated an onset
near 0950 UT.
Title: Doppler brightening of active prominences in hydrogen Blmer
lines
Authors: Rompolt, B.
Bibcode: 1980HvaOB...4...49R
Altcode:
No abstract at ADS
Title: On the Rotational Velocity of Fine Solar Structures Deduced
from the Inclination to the Direction of Dispersion of Their Spectral
Streaks.
Authors: Rompolt, B.; Mzyk, S.
Bibcode: 1979phsp.coll..242R
Altcode: 1979IAUCo..44..242R; 1979phsp.conf..242R
No abstract at ADS
Title: Discussion
Authors: Anzer, U.; Raadu, M. A.; Rompolt, B.; Rust, D. M.; Sheeley,
N.; Spicer, D. S.
Bibcode: 1979phsp.coll..171A
Altcode: 1979IAUCo..44..171A
No abstract at ADS
Title: On the Location of Quiescent Prominences with Respect to
Coronal Holes.
Authors: Rompolt, B.
Bibcode: 1979phsp.coll..209R
Altcode: 1979phsp.conf..209R; 1979IAUCo..44..209R
It is generally known that quiescent prominences are located at
some distance from coronal hole boundaries. In the present paper an
attempt is made to determine whether the average distance between the
nearest border of a coronal hole and the prominence is comparable to
the average x horizontal extension of a helmet structure overlying
the prominence. In addition, an attempt is made to determine whether
this average distance depends on the orientation of the long axis of
the prominence with respect to the nearest boundary of the coronal hole.
Title: On the Need for a Routine Coronagraphic Active-Prominence
Patrol.
Authors: Rompolt, B.
Bibcode: 1979phsp.coll..278R
Altcode: 1979IAUCo..44..278R; 1979phsp.conf..278R
Routine observations of active solar prominences by means of small-size
coronagraphs equipped with birefringent broad-bandpass filters are
discussed as a means of gathering coronal data unavailable by other
means. The usual method of obtaining prominence evolution data as
a by-product of routine flare patrol observations is shown to be
limited to observations of the less active prominences, due to the
extreme line-of-sight velocities of the most active prominences which
are often Doppler shifted past the bandpass of the narrowband filters
employed. Prominence features requiring investigation are discussed,
including electromagnetic emission, kinematics, dynamics and magnetic
fields. The need for routine coronagraphic active-prominence patrols
is concluded, and an actual patrol underway is outlined.
Title: Discussion
Authors: Anzer, U.; Chiuderi-Drago, F.; Kundu, M. R.; Leroy, J. L.;
Malville, J.; Rompolt, B.; Sheeley, N.; Stenflo, J.; Tandberg-Hanssen,
E.; Öhman, Y.
Bibcode: 1979phsp.coll...77A
Altcode: 1979IAUCo..44...77A
No abstract at ADS
Title: Line Profiles Resulting from Expanding and Escaping Fine
Filaments of Prominences
Authors: Ciurla, T.; Rompolt, B.
Bibcode: 1977BAICz..28..217C
Altcode:
Hydrogen-alpha line profiles are given for an optically thin expanding
prominence filament, simultaneously escaping from the sun's surface. The
line profiles were computed for a filament in the shape of a cylinder
or a cylindrical shell, for different kinds of radial-velocity
distributions, and for several accepted values of the expansion rate,
escape velocity, and Doppler width. It was assumed that the filament
scatters incident solar radiation.
Title: Doppler-brightening effect in rotating and expanding optically
thin filaments
Authors: Rompolt, B.; Çiurla, T.
Bibcode: 1976CoSka...6..117R
Altcode:
No abstract at ADS
Title: Profiles of H-alpha line resulting from rotating optically
thin filaments of prominences
Authors: Rompolt, B.
Bibcode: 1976CoSka...6..103R
Altcode:
No abstract at ADS
Title: Events associated with the outburst on 23 September, 1974.
Authors: Garczynska, I.; Rompolt, B.
Bibcode: 1976eear.conf..111G
Altcode:
No abstract at ADS
Title: Profiles of Halpha -line resulting from rotating optically
thin filaments of prominences.
Authors: Rompolt, B.
Bibcode: 1976str..book..103R
Altcode:
No abstract at ADS
Title: Doppler-brightening effect in rotating and expanding optically
thin filaments.
Authors: Rompolt, B.; Cçiurla, T.
Bibcode: 1976str..book..117R
Altcode:
No abstract at ADS
Title: Rotational motions in fine solar structures
Authors: Rompolt, B.
Bibcode: 1975STIN...7614007R
Altcode:
Papers are presented concerning spiral structures in the sun's
atmosphere, spiral and rotational mass motions, appearance of spectral
features resulting from rotational and expansional motion, and twisted
magnetic fields.
Title: Spectral Features to be Expected from Rotational and
Expansional Motions in Fine Solar Structures
Authors: Rompolt, B.
Bibcode: 1975SoPh...41..329R
Altcode:
The shapes of spectral features (lines) to be expected from rotating
or expanding fine solar filaments, loops, and knots (oriented variously
to the spectrograph slit) are given and discussed. Only the appearance
of the lines in the spectrum (i.e., their orientation to the direction
of dispersion and the shape of their area) is considered. It is shown
that the observed inclination to the direction of dispersion of some
spectral features can be produced by rotation but not by expansion. The
observational evidences are given.
Title: Positions of Filament Feet in Relation to the Supergranular
Calcium Network
Authors: Płocieniak, S.; Rompolt, B.
Bibcode: 1973SoPh...29..399P
Altcode:
On the basis of Hα and K Ca II spectroheliograms the positions
of filament feet with regard to the supergranular network was
established. It was found that 65% of the filament feet is located
at the junctions of three or four supergranular cells, 25% at the
junctions of two cells, and 10% in the area of the cells.
Title: Observations of Mercury's Transit Across the Solar Disk on
1970 May 9
Authors: Rompolt, B.; Rybka, P.; Spodenkiewicz, A.; Szczodrowska, B.
Bibcode: 1971AcA....21..245R
Altcode:
The results of observations of the Mercury transit across the solar
disk obtained visually and photographically at the Wroclaw Astronomical
Observatory on May 9, 1970 are given.
Title: Thermostatic control of the birefringent filter of the Wroclaw
Observatory coronograph
Authors: Romer, A.; Rompolt, B.
Bibcode: 1969csph.conf..177R
Altcode:
No abstract at ADS
Title: The region of limb flares and active prominences of July
6, 1968.
Authors: Rompolt, B.; Kozar, T.; Szumiejko, E.
Bibcode: 1969VeGG...13...55R
Altcode:
No abstract at ADS
Title: A statistical investigation of sunspots and chromospheric
flares
Authors: Garczyńska, I.; Jakimcowa, M.; Kordylewski, Z.; Mergentaler,
J.; Rompolt, B.
Bibcode: 1969csph.conf..133G
Altcode:
No abstract at ADS
Title: The influence of the filamentary structure of prominences
and flares on the equivalent widths of lines
Authors: Ciurla, T.; Rompolt, B.
Bibcode: 1969csph.conf..107C
Altcode:
No abstract at ADS
Title: Illumination in Hα of a moving prominence by the photosphere
Authors: Rompolt, B.
Bibcode: 1969csph.conf..117R
Altcode:
No abstract at ADS
Title: The Wrocław Observatory coronograph
Authors: Rompolt, B.; Kraus, T.
Bibcode: 1969csph.conf..171R
Altcode:
No abstract at ADS
Title: The Hα Radiation Field in the Solar Corona for Moving
Prominences
Authors: Rompolt, B.
Bibcode: 1967AcA....17..329R
Altcode:
The paper presents the results of computation of the profiles of the
mean intensity photospheric H_alpha radiation for prominences moving
in the solar corona. Variations of the profiles depending upon the
height, the velocity, and the direction of motion of the prominences
are shown. Calculations were carried out with the aid of a digital
computer Elliott-803.
Title: The Hα Radiation Field in the Solar Corona
Authors: Rompolt, B.
Bibcode: 1967AcA....17..147R
Altcode:
The profiles of the mean photospheric radiation in H_alpha line were
calculated for 45 different heights above the photosphere with the
aid of the digital computer Elliott-803. In the calculations the limb
darkening effect was taken into account.
Title: Relation between surge phenomenon and magnetic field in solar
active region
Authors: Rompolt, B.
Bibcode: 1965BAICz..16..227R
Altcode:
No abstract at ADS
Title: The source function of a quiescent prominence
Authors: Rompolt, B.
Bibcode: 1963BAICz..14...87R
Altcode:
No abstract at ADS