makarov

explanation blue bibcodes open ADS page with paths to full text

Author name code: makarov
ADS astronomy entries on 2022-09-14
author:"Makarov, Valentine I."

---------------------------------------------------------
Title: Quasars with large proper motions: A selection from the
LQAC-5 catalogue combined with Gaia EDR3. Focusing on astrometric
and photometric properties
Authors: Souchay, J.; Secrest, N.; Lambert, S.; Zacharias, N.; Taris,
F.; Barache, C.; Arias, F.; Makarov, V.
2022A&A...660A..16S Altcode:
Context. Thanks to the cross-identification between the Gaia EDR3
(E-Data Release 3) catalogue and the quasars' compiled catalogue
LQAC-5 (Large Quasar Astrometric Catalogue-5), accurate astrometric
parameters as well as photometric measurements were available for a
set of 416 113 quasars. Aims: After analysing the astrometric
and photometric properties of these quasars,we concentrate our study on
objects characterized by significant proper motion, which contradicts
the postulate that they are fixed in the celestial sphere. Methods: We derived statistical properties of the positions,
parallaxes, and proper motions of the quasars cross-matched with Gaia
EDR3. We carried out a specific investigation of quasars with a proper
motion larger than 10 mas yr−1, and used colour-colour
diagrams in mid-infrared to discriminate these quasars from stellar
contamination. We discuss, in detail, a few cases where the abnormal
proper motion could be caused by misidentifications. Results: We
note that 43% of LQAC-5 quasars were not detected by Gaia EDR3, mainly
because of the cut-off magnitude at G = 21. The comparison between
r(G) (Gaia) and r (SDSS) shows a normal distribution. The normalized
distributions of parallaxes and proper motions are identical to that
of the Gaia CRF2, as well as the distribution of the GBP
− GRP colour index. We have identified 937 LQAC-5 objects
(0.27% of the sample) with Gaia EDR3 proper motion which is significant
at the 5σ level. We have clearly shown that below z = 0.35, the
integrated magnitude G(r) obtained from SDSS spectra is smaller than
G (Gaia), leading to the statement that the quasars are generally
resolved under this threshold, which should lead to a bad determination
of proper motion. Moreover, to discriminate quasars from stellar
contamination, we have plotted them in a mid-infrared colour-colour
diagram. Finally, we have made a final selection of 41 objects with μ
&gt; 10 mas yr−1, satisfying drastic constraints, which
makes them potential candidates for considering their proper motion
as real. Conclusions: In this paper we carried out a complete
analysis of the quasars of the LQAC-5 which were cross-identified
with Gaia EDR3 ; this serves as an alternative and complementary
study with respect to Gaia CRF2, involving a different population of
quasars. We selected a set of 41 quasars with a proper motion exceeding
10 mas yr−1, which can be considered as very high for
objects which are a priori fixed in the celestial sphere. Full
Table A.1 is only available at the CDS via anonymous ftp to <A
href="http://cdsarc.u-strasbg.fr/">cdsarc.u-strasbg.fr</A>
(ftp://130.79.128.5) or via <A
href="http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/660/A16">http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/660/A16</A>

---------------------------------------------------------
Title: VizieR Online Data Catalog: Quasars with large proper motions
(Souchay+, 2022)
Authors: Souchay, J.; Secrest, N.; Lambert, S.; Zacharias, N.; Taris,
F.; Barache, C.; Arias, F.; Makarov, V.
2022yCat..36600016S Altcode:
We have constructed an improved version of the LQAC5 catalogue (Souchay
et al., 2019A&amp;A...624A.145S, Cat. J/A+A/624/A145), which we called
LQAC5+, by matching its total sample of 592809 quasars with the Gaia
EDR3 catalogue (Gaia Collabaration, 2020, Cat. I/350). We present
a sample of the 41 LQAC-5 quasars selected from Gaia EDR3 data with
μ&gt;10 mas/yr, {chi}μ&gt;5, π/σπ&lt;4 and
located in the quasars central zone . (1 data file).

---------------------------------------------------------
Title: The Atmospheric Chemistry Suite (ACS) of Three Spectrometers
for the ExoMars 2016 Trace Gas Orbiter
Authors: Korablev, O.; Montmessin, F.; Trokhimovskiy, A.; Fedorova,
A. A.; Shakun, A. V.; Grigoriev, A. V.; Moshkin, B. E.; Ignatiev,
N. I.; Forget, F.; Lefèvre, F.; Anufreychik, K.; Dzuban, I.; Ivanov,
Y. S.; Kalinnikov, Y. K.; Kozlova, T. O.; Kungurov, A.; Makarov, V.;
Martynovich, F.; Maslov, I.; Merzlyakov, D.; Moiseev, P. P.; Nikolskiy,
Y.; Patrakeev, A.; Patsaev, D.; Santos-Skripko, A.; Sazonov, O.;
Semena, N.; Semenov, A.; Shashkin, V.; Sidorov, A.; Stepanov, A. V.;
Stupin, I.; Timonin, D.; Titov, A. Y.; Viktorov, A.; Zharkov, A.;
Altieri, F.; Arnold, G.; Belyaev, D. A.; Bertaux, J. L.; Betsis, D. S.;
Duxbury, N.; Encrenaz, T.; Fouchet, T.; Gérard, J. -C.; Grassi, D.;
Guerlet, S.; Hartogh, P.; Kasaba, Y.; Khatuntsev, I.; Krasnopolsky,
V. A.; Kuzmin, R. O.; Lellouch, E.; Lopez-Valverde, M. A.; Luginin,
M.; Määttänen, A.; Marcq, E.; Martin Torres, J.; Medvedev, A. S.;
Millour, E.; Olsen, K. S.; Patel, M. R.; Quantin-Nataf, C.; Rodin,
A. V.; Shematovich, V. I.; Thomas, I.; Thomas, N.; Vazquez, L.;
Vincendon, M.; Wilquet, V.; Wilson, C. F.; Zasova, L. V.; Zelenyi,
L. M.; Zorzano, M. P.
2018SSRv..214....7K Altcode:
The Atmospheric Chemistry Suite (ACS) package is an element of the
Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter
(TGO) mission. ACS consists of three separate infrared spectrometers,
sharing common mechanical, electrical, and thermal interfaces. This
ensemble of spectrometers has been designed and developed in response to
the Trace Gas Orbiter mission objectives that specifically address the
requirement of high sensitivity instruments to enable the unambiguous
detection of trace gases of potential geophysical or biological
interest. For this reason, ACS embarks a set of instruments achieving
simultaneously very high accuracy (ppt level), very high resolving
power (&gt;10,000) and large spectral coverage (0.7 to 17 μm—the
visible to thermal infrared range). The near-infrared (NIR) channel
is a versatile spectrometer covering the 0.7-1.6 μm spectral range
with a resolving power of ∼20,000. NIR employs the combination of
an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as
diffraction order selector. This channel will be mainly operated in
solar occultation and nadir, and can also perform limb observations. The
scientific goals of NIR are the measurements of water vapor, aerosols,
and dayside or night side airglows. The mid-infrared (MIR) channel is
a cross-dispersion echelle instrument dedicated to solar occultation
measurements in the 2.2-4.4 μm range. MIR achieves a resolving
power of &gt;50,000. It has been designed to accomplish the most
sensitive measurements ever of the trace gases present in the Martian
atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double
pendulum Fourier-transform spectrometer encompassing the spectral
range of 1.7-17 μm with apodized resolution varying from 0.2 to 1.3
cm-1. TIRVIM is primarily dedicated to profiling temperature
from the surface up to ∼60 km and to monitor aerosol abundance in
nadir. TIRVIM also has a limb and solar occultation capability. The
technical concept of the instrument, its accommodation on the
spacecraft, the optical designs as well as some of the calibrations,
and the expected performances for its three channels are described.

---------------------------------------------------------
Title: Quantum teleportation over a 143-km free-space link
Authors: Herbst, T.; Ma, X.; Scheidl, T.; Wang, D.; Naylor, W.;
Wittmann, B.; Kofler, J.; Anisimova, E.; Makarov, V.; Jennewein, T.;
Ursin, R.; Zeilinger, A.
2017SPIE10563E..0VH Altcode:
Quantum teleportation is a quintessential prerequisite of many quantum
information-processing protocols.

---------------------------------------------------------
Title: VizieR Online Data Catalog: AGNs in the MIR using AllWISE data
(Secrest+, 2015)
Authors: Secrest, N. J.; Dudik, R. P.; Dorland, B. N.; Zacharias,
N.; Makarov, V.; Fey, A.; Frouard, J.; Finch, C.
2016yCat..22210012S Altcode:
The WISE survey is an all-sky mid-IR survey at 3.4, 4.6, 12, and 22um
(W1, W2, W3, and W4, respectively) conducted between 2010 January 7 and
August 6. WISE has angular resolutions of 6.1", 6.4", 6.5", and 12.0"
in its four bands. The AllWISE data release, which we use for this
work, incorporates data from the WISE Full Cryogenic, 3-Band Cryo,
and NEOWISE Post-Cryo survey (Mainzer et al. 2014ApJ...792...30M)
phases. (1 data file).

---------------------------------------------------------
Title: Identification of 1.4 Million Active Galactic Nuclei in the
Mid-Infrared using WISE Data
Authors: Secrest, N. J.; Dudik, R. P.; Dorland, B. N.; Zacharias,
N.; Makarov, V.; Fey, A.; Frouard, J.; Finch, C.
2015ApJS..221...12S Altcode: 2015arXiv150907289S
We present an all-sky sample of ≈1.4 million active galactic nuclei
(AGNs) meeting a two-color infrared photometric selection criteria
for AGNs as applied to sources from the Wide-field Infrared Survey
Explorer final catalog release (AllWISE). We assess the spatial
distribution and optical properties of our sample and find that the
results are consistent with expectations for AGNs. These sources have
a mean density of ≈38 AGNs per square degree on the sky, and their
apparent magnitude distribution peaks at g ≈ 20, extending to objects
as faint as g ≈ 26. We test the AGN selection criteria against a large
sample of optically identified stars and determine the “leakage”
(that is, the probability that a star detected in an optical survey
will be misidentified as a quasi-stellar object (QSO) in our sample)
rate to be ≤4.0 × 10-5. We conclude that our sample
contains almost no optically identified stars (≤0.041%), making
this sample highly promising for future celestial reference frame
work as it significantly increases the number of all-sky, compact
extragalactic objects. We further compare our sample to catalogs of
known AGNs/QSOs and find a completeness value of ≳84% (that is, the
probability of correctly identifying a known AGN/QSO is at least 84%)
for AGNs brighter than a limiting magnitude of R ≲ 19. Our sample
includes approximately 1.1 million previously uncataloged AGNs.

---------------------------------------------------------
Title: 1.4 Million Mid-Infrared AGNs for the Optical Reference Frame
Authors: Secrest, N.; Dudik, R. P.; Dorland, B. N.; Zacharias, N.;
Makarov, V.; Fey, A.; Frouard, J.; Finch, C.
2015deam.confE..99S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On Mercury's entrapment into the 3:2 spin-orbit resonance
Authors: Noyelles, Benoit; Frouard, J.; Makarov, V.; Efroimsky, M.
2013DPS....4510201N Altcode:
The rotational dynamics of Mercury is a peculiar case in the Solar
System, since it is a supersynchronous, 3:2 resonant state, with the
spin period being 2/3 of the orbital one. While it is widely accepted
that the significant eccentricity (0.206) favours this configuration,
the history of Mercury's despinning remains nonetheless a matter of
discussion. At least three scenarios can be found in the scientific
literature. The first one considers a homogeneous Mercury that was
trapped after several crossings of the resonance, these crossings made
possible by the chaotic evolution of the eccentricity (Correia &amp;
Laskar 2004). The second scenario includes friction at the core-mantle
boundary, which increases the probabilities of capture during one
crossing (Peale &amp; Boss 1977, Correia &amp; Laskar 2009). The third
scenario assumes that Mercury had had a retrograde rotation, then a
synchronous one, and only later came into the current 3:2 resonance. We
here use a realistic model of tides, based on the Darwin-Kaula
expansions combined with both the elastic rebound and anelastic
creep of solids. Within this model, we find that the 3:2 spin-orbit
resonance is the most probable for a homogeneous Mercury. Moreover,
we find that leaving a resonance after being trapped is impossible or
virtually impossible, thus excluding the possibility of a past 2:1
resonance. This also indicates that entrapment is likely to happen
before the differentiation of Mercury takes place.

---------------------------------------------------------
Title: No Pseudosynchronous Rotation for Terrestrial Planets and Moons
Authors: Makarov, V.; Efroimsky, M.
2012epsc.conf..815M Altcode: 2012espc.conf..815M
We reexamine the popular belief that a telluric planet or satellite on
an eccentric orbit can, outside a spinorbit resonance, be captured in
a quasi-static tidal equilibrium called pseudosynchronous rotation. The
existence of such configurations was deduced from oversimplified tidal
models assuming either a constant tidal torque or a torque linear
in the tidal frequency. A more accurate treatment requires that the
torque be decomposed into the Darwin-Kaula series over the tidal modes,
and that this decomposition be combined with a realistic choice of
rheological properties of the mantle. This development demonstrates
that there exist no stable equilibrium states for solid planets and
moons, other than spin-orbit resonances.

---------------------------------------------------------
Title: Quantification Of Errors In The Hipparcos Catalog
Authors: Hennessy, Gregory S.; Dudik, R.; Dorland, B.; Zacharias,
N.; Makarov, V.
2012AAS...22032801H Altcode:
The HIPPARCOS Catalog (Perrymann, et al. 1997) produced positions,
proper motions, and parallaxes to the milliarcsecond for almost 120,000
objects. Over the last fifteen years much research has accrued from
HIPPARCOS astrometry, including the cosmic distance scale, kinematic
motions of the solar neighborhood, precise luminosities for stellar
motions, and confirmation of the Einstein prediction on deflection of
starlight. However the errors on the astrometric values provided in this
widely used catalog have degraded over time. The current state of the
art in ground based observations allow us to attempt to quantify the
errors in the proper motions of HIPPARCOS stars. This poster outlines
the moving cluster methodology we have used to estimate the astrometric
errors on HIPPARCOS stars as well as calculated effect on HIPPARCOS
position, proper motion and parallax accuracies.

---------------------------------------------------------
Title: Quasometry, its use and purpose
Authors: Makarov, V.; Berghea, C.; Boboltz, D.; Dieck, C.; Dorland,
B.; Dudik, R.; Fey, A.; Gaume, R.; Lei, X.; Schmitt, H.; Zacharias, N.
2012MmSAI..83..952M Altcode: 2012arXiv1202.5283M
Quasometry is precision measurement of celestial positions and
apparent motion of very distant extragalactic objects, such as
quasars, galactic nuclei, and QSOs. We use this term to identify a
specific area of research, the methodology of which differs from
that of general astrometry. The main purpose of quasometry is to
link the sub-milliarcsecond radio frame (ICRF) with the existing and
emerging optical reference frames of similar accuracy, constructed
by astrometric satellites. Some of the main difficulties in achieving
this goal are discussed, e.g., the extended structures of quasar hosts,
apparent motion on the sky, optical variability, galactic companions,
faintness. Besides the strategic purpose, quasometry is undoubtedly
useful for global astrometric surveys, as it helps to verify or even
correct the resulting reference frames. There are two options of using
measurements of distant quasars in a global astrometric solution: 1)
hard constraints embedded in the fabric of observational equations;
2) a posteriori fitting of zonal errors. The relative benefits and
shortcoming of the two options are reviewed. A relatively small set
of about 200 carefully selected reference quasars can go a long way
in improving the astrometric value of a space mission, if they are
sufficiently bright, stable, fairly uniformly distributed on the sky,
and are defining sources in the ICRF. We present an ongoing program
at the USNO to construct a quality set of optical quasars with the
required properties and to enhance the ICRF with new sources in the
areas where known, well-observed quasars are scarce.

---------------------------------------------------------
Title: The Third US Naval Observatory CCD Astrograph Catalog (UCAC3)
Authors: Zacharias, N.; Finch, C.; Girard, T.; Hambly, N.; Wycoff, G.;
Zacharias, M. I.; Castillo, D.; Corbin, T.; DiVittorio, M.; Dutta,
S.; Gaume, R.; Gauss, S.; Germain, M.; Hall, D.; Hartkopf, W.; Hsu,
D.; Holdenried, E.; Makarov, V.; Martinez, M.; Mason, B.; Monet, D.;
Rafferty, T.; Rhodes, A.; Siemers, T.; Smith, D.; Tilleman, T.; Urban,
S.; Wieder, G.; Winter, L.; Young, A.
2010AJ....139.2184Z Altcode: 2010arXiv1003.2136Z
The third US Naval Observatory (USNO) CCD Astrograph Catalog, UCAC3,
was released at the IAU General Assembly on 2009 August 10. It is
the first all-sky release in this series and contains just over
100 million objects, about 95 million of them with proper motions,
covering about R = 8-16 mag. Current epoch positions are obtained from
the observations with the 20 cm aperture USNO Astrograph's "red lens,"
equipped with a 4k × 4k CCD. Proper motions are derived by combining
these observations with over 140 ground- and space-based catalogs,
including Hipparcos/Tycho and the AC2000.2, as well as unpublished
measures of over 5000 plates from other astrographs. For most of the
faint stars in the southern hemisphere, the Yale/San Juan first epoch
plates from the Southern Proper Motion (SPM) program (YSJ1) form the
basis for proper motions. These data are supplemented by all-sky Schmidt
plate survey astrometry and photometry obtained from the SuperCOSMOS
project, as well as 2MASS near-IR photometry. Major differences of
UCAC3 data as compared with UCAC2 include a completely new raw data
reduction with improved control over systematic errors in positions,
significantly improved photometry, slightly deeper limiting magnitude,
coverage of the north pole region, greater completeness by inclusion
of double stars, and weak detections. This of course leads to a catalog
which is not as "clean" as UCAC2 and problem areas are outlined for the
user in this paper. The positional accuracy of stars in UCAC3 is about
15-100 mas per coordinate, depending on magnitude, while the errors
in proper motions range from 1 to 10 mas yr-1 depending on
magnitude and observing history, with a significant improvement over
UCAC2 achieved due to the re-reduced SPM data and inclusion of more
astrograph plate data unavailable at the time of UCAC2.

---------------------------------------------------------
Title: Detectability of Earth-like Planets in Multi-Planet Systems:
Preliminary Report
Authors: Traub, W. A.; Beichman, C.; Boden, A. F.; Boss, A. P.;
Casertano, S.; Catanzarite, J.; Fischer, D.; Ford, E. B.; Gould, A.;
Halverson, S.; Howard, A.; Ida, S.; Kasdin, N. J.; Laughlin, G. P.;
Levison, H. F.; Lin, D.; Makarov, V.; Marr, J.; Muterspaugh, M.;
Raymond, S. N.; Savransky, D.; Shao, M.; Sozzetti, A.; Zhai, C.
2010EAS....42..191T Altcode: 2009arXiv0904.0822T
We ask if Earth-like planets (terrestrial mass and habitable-zone
orbit) can be detected in multi-planet systems, using astrometric and
radial velocity observations. We report here the preliminary results
of double-blind calculations designed to answer this question.

---------------------------------------------------------
Title: Zonal Error Propagation for JMAPS
Authors: Hennessy, Gregory S.; Makarov, V.
2009AAS...21460009H Altcode:
Propagation of accidental zonal errors of parallax is analyzed
for J-MAPS. A method based on orthogonal spherical functions and a
simplified setup of observational grid equations is proposed. Using
this method, a full-scale simulation can be performed for a limited
number of large-scale zonal errors, including the zero-point error,
on a regular personal computer. Covariances of parallax zonal errors
and their dependence on the density of grid quasars, the density and
overlap of grid stars, the observing scenario, etc., can be investigated
by this technique and the accompanying Matlab software.

---------------------------------------------------------
Title: The Joint Milli-arcsecond Pathfinder Survey (JMAPS):
Introduction and science possibilities
Authors: Gaume, R.; Dorland, B.; Dudik, R.; Hennessy, G.; Dugan, Z.;
Makarov, V.; Barrett, P.; Dieck, C.; Veilette, D.; Zacharias, N.
2009jsrs.conf..219G Altcode:
JMAPS is a small, space-based, all-sky visible wavelength astrometric
and photometric survey mission for 0th through 14th V-band magnitude
stars with a 2012 launch. The primary objective of the JMAPS mission
is the generation of an astrometric star catalog with better than 1
milliarcsecond positional accuracy and photometry to the 1% accuracy
level or better at 1st to 12th mag. A 1-mas all-sky survey will have
a significant impact on our current understanding of galactic and
stellar astrophysics. JMAPS will improve our understanding of the
origins of nearby young stars, provide insight into the dynamics of
star formation regions and associations, investigate the dynamics and
membership of nearby open clusters, and discover the smallest brown
dwarfs at distances up to 5 pc after a 2-year mission, and Jupiter-like
planets out to 3 pc after 4 years.

---------------------------------------------------------
Title: UCAC3 Catalogue (Zacharias+ 2009)
Authors: Zacharias, N.; Finch, C.; Girard, T.; Hambly, N.; Wycoff, G.;
Zacharias, M. I.; Castillo, D.; Corbin, T.; Divittorio, M.; Dutta,
S.; Gaume, R.; Gauss, S.; Germain, M.; Hall, D.; Hartkopf, W.; Hsu,
D.; Holdenried, E.; Makarov, V.; Martines, M.; Mason, B.; Monet, D.;
Rafferty, T.; Rhodes, A.; Siemers, T.; Smith, D.; Tilleman, T.; Urban,
S.; Wieder, G.; Winter, L.; Young, A.
2009yCat.1315....0Z Altcode:
UCAC3 is a compiled, all-sky star catalog covering mainly the 8 to
16 magnitude range in a single bandpass between V and R. Positional
errors are about 15 to 20 mas for stars in the 10 to 14 mag range. It is
supplemented by proper motions and SuperCosmos and 2MASS photometric
data, as well as various flags. The proper motions of bright
stars are based on about 140 catalogs, including Hipparcos and
Tycho, as well as all catalogs used for the Tycho-2 proper motion
construction. Proper motions of faint stars are based on a re-reduction
of early epoch SPM data (-90 to -10 deg Dec) plus Schmidt plate data
from the SuperCosmos project (down weighted due to systematic errors
of order 100 mas). The proper motions of faint stars (R &gt;= 13.5)
therefore should be used with caution. The unpublished plate measure
data from the AGK2, the Hamburg Zone Astrograph, the USNO Black Birch
Astrograph, and the Lick Astrograph have considerably contributed
to improve proper motions for stars mainly in the 10 to 14 mag range
(down to the UCAC3 limit for Lick data); however, these data do not
cover all sky. UCAC3 features a number of major differences with
respect to UCAC2: - complete sky coverage - re-reduction of the pixel
data with better modeling - double stars are resolved to the limit of
the data - significantly improved photometry from CCD data - slightly
deeper limiting magnitude with larger number of stars/area - reduced
systematic errors of CCD observations - the addition of several new
catalogs for improved proper motions - photometry in the B, R, and I
bands from the SuperCosmos project - minor planet observations have
been sorted out - identification of more high proper motion stars -
match with 2MASS extended sources and LEDA galaxies Additional
details will be published in the upcoming release paper (Zacharias
et al. 2009) and in several technical papers describing details of
the reduction procedures and results. For the latest updates see
http://www.usno.navy.mil/usno/astrometry . Requests for the data
DVD should be sent to ucac3@usno.navy.mil; technical questions can be
addressed to nz@usno.navy.mil . (2 data files).

---------------------------------------------------------
Title: The Joint Milli-Arcsecond Pathfinder Survey (J-MAPS) Mission:
Introduction and Science Goals
Authors: Gaume, Ralph A., Jr.; Dorland, B.; Hennessy, G.; Dudik,
R.; Barrett, P.; Dugan, Z.; Veillette, D.; Dieck, C.; Bartlett, J.;
Zacharias, N.; Johnston, K.; Makarov, V.
2009AAS...21423904G Altcode:
J-MAPS is a small, funded, space-based, all-sky visible wavelength
astrometric and photometric survey mission for 0th through 14th
V-band magnitude stars with a 2012 launch. The primary objective of
the J-MAPS mission is the generation of an astrometric star catalog
with better than 1 milliarcsecond positional accuracy and photometry
to the 1 percent accuracy level or better for 1st to 12th mag stars. A
1-mas all-sky survey will have a significant impact on our current
understanding of galactic and stellar astrophysics. J-MAPS will
improve our understanding of the origins of nearby young stars,
provide insight into the dynamics of star formation regions and
associations, investigate the dynamics and membership of nearby open
clusters, and discover the smallest brown dwarfs at distances up to 5
pc after a 2-year mission, and Jupiter-like planets out to 3 pc after
4 years. J-MAPS will provide critical milliarcsecond-level parallaxes
of tens of millions of stars in the difficult 8-14th magnitude range,
which when combined with stellar spectroscopy and relative radii
determined from exoplanet transit surveys, allows a determination of
stellar radii and exoplanet densities. In addition, the 20-year baseline
between the groundbreaking Hipparcos mission and the J-MAPS mission
allows a combination of the J-MAPS and Hipparcos catalogs to produce
common proper motions on the order of 50-100 microarcseconds per year.

---------------------------------------------------------
Title: The Joint Milli-Arcsecond Pathfinder Survey (J-MAPS) Mission:
Introduction and Science Goals
Authors: Gaume, Ralph A., Jr.; Dorland, B.; Hennessy, G.; Dudik, R.;
Bartlett, J.; Dugan, Z.; Zacharias, N.; Johnston, K.; Makarov, V.
2009AAS...21345101G Altcode: 2009BAAS...41Q.344G
The Joint Milli-Arcsecond Pathfinder Survey (J-MAPS) mission is a small,
space-based, all-sky visible wavelength astrometric and photometric
survey for 2nd through 15th magnitude stars with a 2012 launch goal. The
primary mission goal for J-MAPS is the generation of a nearly 40 million
star astrometric catalog with better than 1 milliarcsecond positional
accuracy, and photometry to the 1% accuracy level, or better. A 1-mas
(or better) all-sky survey will have a significant impact on our
current understanding of galactic and stellar astrophysics. J-MAPS will
impact our understanding of the origins of nearby young stars, provide
insight into the dynamics of star formation regions and associations,
investigate the dynamics and membership of nearby open clusters, and
discover the smallest brown dwarfs at distances up to 5pc after a 2 year
mission, and Jupiter-like planets out to 3pc after 4 years. J-MAPS will
provide critical milliarcsecond level parallaxes of tens of millions
of stars in the difficult 8-15th magnitude range, which when combined
with stellar spectroscopy and relative radii determined from exoplanet
transit surveys, allows a determination of stellar radii and exoplanet
densities. In addition, the 20 year baseline between the groundbreaking
Hipparcos mission and the J-MAPS mission allows the combination of
J-MAPS and Hipparcos catalogs to produce common proper motions on the
order of 50-100 microarcseconds per year.

---------------------------------------------------------
Title: Overview Of The SIM-RV Double-blind Simulation To Detect
Earths In Multi-planet Systems
Authors: Traub, Wesley A.; Ford, E.; Laughlin, G.; Levison, H.; Lin,
D.; Raymond, S.; Makarov, V.; Casertano, S.; Fischer, D.; Kasdin, J.;
Muterspaugh, M.; Shao, M.; Beichman, C.; Boss, A.; Gould, A.; Marr, J.
2009AAS...21330001T Altcode: 2009BAAS...41..267T
We report the results of a double-blind study of the ability to detect
Earth-mass exoplanets in multi-planet systems using a combination of
the proposed astrometric space mission SIM-Lite and ongoing ground-based
radial velocity (RV) observations. Three independent teams contribute to
this study. Team A comprises five groups of exoplanet system modelers
who each contribute over 100 theoretical systems that are consistent
with current expectations of the distribution functions of mass and
orbital parameters of nearby exoplanet systems. Team B takes these
models as input and generates simulated data sets of SIM-Lite and RV
observations, using appropriate observing constraints and expected
noise levels. Team C groups analyze the simulated data sets to extract
the underlying planet mass and orbital parameters. The input models
depend on current theoretical estimates of the distribution functions
of parameters in multi-planet systems. The results of this study have
significant implications for future searches for terrestrial-mass
planets.

---------------------------------------------------------
Title: Is There a Need for an Improved Celestial Reference Frame ?
Authors: Johnston, Kenneth; Wehrle, A. E.; Makarov, V.; Murphy, D. W.;
Unwin, S. C.; Zacharias, N.; Fey, A. L.; Ojha, R.; Boboltz, D. A.;
Lazio, T. J.; Olling, R. F.; Gaume, R. A.
2009astro2010S.143J Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Gravitational bending of light by planetary multipoles and
its measurement with microarcsecond astronomical interferometers
Authors: Kopeikin, S.; Makarov, V.
2008IAUS..248..391K Altcode:
General relativistic deflection of light by mass, dipole, and quadrupole
moments of gravitational field of a moving massive planet in the Solar
system is derived in the approximation of the linearized Einstein
equations. All terms of the order of 1 μas and larger are taken into
account, parameterized, and classified in accordance with their physical
origin. We discuss the observational capabilities of the near-future
optical and radio interferometers for detecting the Doppler modulation
of the radial deflection, and the dipolar and quadrupolar light-ray
bending by Jupiter and Saturn.

---------------------------------------------------------
Title: Indices for the epochs of the solar activity minima
Authors: Tlatov, A. G.; Makarov, V. I.
2007IJGA....7.2003T Altcode: 2007IJGA....7I2003T
[1] New solar activity indices for the sunspot cycle minima
were obtained from the Hα synoptic charts for 1887-2005, Ca II K
observational data of the solar disk at Kodaikanal for 1907-1995. The
Apz index determines the area of the polar zone occupied by the
magnetic field of one polarity, and A(t) is the sum of squares of
dipole and octupole magnetic moments. The L(t) index is the total
length of magnetic neutral lines on the Hα synoptic chart, and K(t)
characterizes the complexity of the topology pattern of the general
magnetic field of the Sun. It is determined by the inverse number of
crossings of neutral lines with the meridian net on the Hα chart. The
R(t) index characterizes the correlation factor of the magnetic field
polarities in the latitude zones +/-40o. The solar rotation
index SSPD(t) is determined by the sum of the spectral density of the
power of the magnetic field sector structures. The area of the Ca II K
bright points at high latitudes is the S K (t) index. It has
been shown that the 11-year cycles of Apz(t), A(t), L(t), K(t), R(t),
SSPD(t), and S K (t) have maxima at the sunspot activity
minimum and that they are ahead of the cycles of Wolf numbers, W(t),
by 5-6 years.

---------------------------------------------------------
Title: Space Astrometry With The Milli-Arcsecond Pathfinder Survey
(MAPS): Mission Overview And Science Possibilities
Authors: Gaume, Ralph A., Jr.; Dorland, B.; Zacharias, N.; Hennessy,
G.; Johnston, K.; Makarov, V.
2007AAS...210.8601G Altcode: 2007BAAS...39R.194G
The Milli-Arcsecond Pathfinder Survey (MAPS) mission is a space-based,
all-sky, visible wavelength astrometric and photometric survey for
2nd through 15th magnitude stars with a 2012 launch date goal. The
primary mission goal for MAPS is the generation of a 1-milliarcsecond
(mas) all-sky astrometric catalog for bright stars. The instrument
consists of a 15-cm telescope, a large (64 megapixel) CMOS-hybrid
detector, associated processing electronics, and is carried aboard a
microsatellite bus in a 900-km, sun-synchronous, low Earth orbit. The
status of the MAPS mission will be reviewed, including current risk
reduction activities. A 1-mas (or better) all-sky survey through
approximately 15th magnitude will have a significant impact on
our current understanding of galactic and stellar astrophysics. In
particular, the combination of the MAPS and Hipparcos catalogs will
produce common proper motions on the order of 0.1 mas/yr level.

---------------------------------------------------------
Title: Binarity Jitter In Hipparcos Parallax for HD 48097
Authors: Pan, Xiaopei; Makarov, V.
2007AAS...210.0306P Altcode: 2007BAAS...39...98P
Hipparcos mission measured parallax with claimed measurement error
of 1 mas for 120000 targets. Arguments about systematic errors of the
Hipparcos parallax have never been stopped. One of the major systematic
error sources is the binarity jitter because the Hipparcos parallax
is deeply troubled by the binary stars. In this work we demonstrate
significant binarity jitters for star HD 48097. Although the Hipparcos
has determined its orbit and made correction for fitting of parallax
determination, we show that the systematic error in Hipparcos parallax
for that target is as big as two and half times than it should
be. Our new calculation algorithm use high precision radial velocity
measurements combining with Hipparcos intermediate data and obtained
new parallax for HD 48097. Our results indicate that the precision of
Hipparcos parallax for that target has been improved by the factor of
3. We conclude that it is necessary to dig out systematic errors of
Hipparcos parallax by using other high precision techniques, such as
long baseline optical/IR interferometers, high accuracy spectrometers,
etc.

---------------------------------------------------------
Title: Monopolar structure of the Sun in between polar reversals
and in Maunder Minimum
Authors: Callebaut, D. K.; Makarov, V. I.; Tlatov, A. G.
2007AdSpR..40.1917C Altcode:
After a polar reversal in one hemisphere the Sun has two polar caps of
the same sign, leaving it in a kind of monopolar state. It may take
months before a polar reversal occurs in the other hemisphere. The
situation may have been extreme in the Maunder Minimum where the
northern hemisphere most probably did not have polar reversals during
several cycles, while the southern hemisphere may have had some. This
may affect the interplanetary field and thus the cosmic rays reaching
the Earth. Using the relation between the Wolf number and the speed of
the global magnetic field regions the yearly mean Wolf number has to
exceed 40 in order to have polar reversals, hence per hemisphere we
expect that it must exceed 20. This may be used to give a definition
of a deep minimum.

---------------------------------------------------------
Title: The Origins Billions Star Survey: Galactic Explorer
Authors: Johnston, K. J.; Dorland, B.; Gaume, R.; Hennessy, G.;
Olling, R.; Zacharias, N.; Behr, B.; Efroimsky, M.; Hajian, A.;
Harris, H.; Hilton, J.; Kaplan, G.; Monet, D.; Munn, J.; Pier, J.;
Vrba, F.; Seidelmann, K.; Seager, S.; Pravdo, S.; Coste, K.; Danner,
R.; Grillmair, C.; Stauffer, J.; Boss, A.; Currie, D.; Danchi, W.;
Gould, A.; Kopeikin, S.; Majewski, S.; Makarov, V.; McMillan, R.;
Peterson, D. M.; Shaya, E.; Unwin, S.
2006PASP..118.1428J Altcode:
The Origins Billions Star Survey is a mission concept addressing the
astrophysics of extrasolar planets, Galactic structure, the Galactic
halo and tidal streams, the Local Group and local supercluster
of galaxies, dark matter, star formation, open clusters, the solar
system, and the celestial reference frame by determining the position,
parallax, and proper motion, as well as photometry, for billions of
stars down to 23rd visual magnitude. It is capable of surveying the
entire celestial sphere or dwelling on a star field by varying the
cadence of observations. The mission's ability to measure objects
fainter than 17th magnitude allows a large number of extragalactic
compact objects to be observed, making the astrometric measurements
absolute. The project mission accuracy is comparable to Gaia for a
survey mission. Improved accuracy can be achieved by dwelling on a
particular star field or by using the Gaia positions at 14th magnitude
to improve the positions of objects at the 18th-23rd visual magnitudes.

---------------------------------------------------------
Title: Space Astrometry With The Milli-Arcsecond Pathfinder Survey
(MAPS): Mission Overview And Science Possibilities
Authors: Gaume, R.; Dorland, B.; Makarov, V.; Zacharias, N.; Johnston,
K.; Hennessy, G.
2006IAUJD..16E..26G Altcode:
MAPS is a space-based, all-sky astrometric and photometric survey from
2nd through 15th magnitude with a 2010 launch date goal. The primary
mission goal for MAPS is the generation of a 1-milliarcsecond (mas)
all-sky astrometric catalog for the 2010 epoch. The instrument consists
of a 15-cm telescope, a large (64 megapixel) active pixel sensor focal
plane, and associated processing electronics, and is carried aboard a
microsatellite bus in a 900-km, sun-synchronous low Earth orbit. MAPS
technology, including the very large format detector, the onboard
processing electronics, and next generation space-based GPS-receiver,
will serve as a pathfinder in support of future space missions. A 1-mas
(or better) all-sky survey through approximately 15th magnitude will
have a tremendous impact on our current understanding of the galaxy
and stellar astrophysics. MAPS science topics include: a kinematic
and photometric exploration of the nearest star forming regions and
associations; an understanding of the dynamics and membership of nearby
open clusters; a survey of nearby stars that addresses the 130 missing
systems within 10 pc; recalibration of the cosmic distance scale via
distances to nearby clusters, and the period-luminosity relationship
using high accuracy proper motion (Hipparcos and MAPS positions and a
twenty year baseline) and parallax measurements; discovery of giant
planets and brown dwarfs orbiting nearby stars; kinematic detection
of galactic cannibalism and mergers in the Milky Way; and discovery
of low-mass black holes and neutron stars in astrometric binaries.

---------------------------------------------------------
Title: Temperature of Polar Corona of the Sun According to Kislovodsk
Observations During 1957 2002
Authors: Makarov, V. I.; Tlatov, A. G.; Callebaut, D. K.
2006SoPh..237..201M Altcode:
We continued a study of the long-term variations of temperature in
the solar corona at all latitudes (Makarov, Tlatov, and Callebaut,
2002a). The series of the green (Fe xiv 530.3 nm; KI5303)
and red (Fe x 637.4 nm; KI6374) coronal intensities for
1957-2002 has been obtained using the coronal observations at the
Kislovodsk Solar Station. The mean monthly coronal intensities have
been calculated at all latitudes (0-90˚) and in the high
latitude (45-90˚) zones. It was found that the value
of KI6374/KI5303increased about 2.0 times
at the high latitudes during the last 45 years. This corresponds
to a decrease of the average temperature by 0.1 ×106K
of the polar corona. We suppose that a polar decrease of coronal
temperature is connected with an increase of the area of polar zones
APZoccupied by unipolar magnetic fields (Makarov et al.,
2002) and, probably, with an increase of the area of polar coronal
holes. The maximum ratio KI6374/KI5303is observed
during the minimum sunspot activity.

---------------------------------------------------------
Title: Decrease of hot regions in the polar corona of the Sun during
1957 2002
Authors: Callebaut, D. K.; Tlatov, A. G.; Makarov, V. I.
2006IAUS..233..247C Altcode:
The Kislovodsk series of the green (FeXIV 530.3 nm; KI_{5303})
and red (FeX 637.4 nm; KI_{6374}) corona has been used to calculate
the mean monthly intensities at high latitude (45°-90°) zones for
1957-2002. The ratio KI_{6374}/KI_{5303} was observed during the
minimum sunspot activity. It was shown that this ratio increased by
more than a factor 2 during the last 45 years at the high latitudes
(45°-90°). This may be interpreted that the fraction of cool regions
in the polar corona has more than doubled over these years. We suggest
that this increase in the amount of cool regions is related to the
increase in the area of the polar zones occupied by magnetic field of
a single polarity at the solar minimum and possibly to a corresponding
increase in the area occupied by polar coronal holes, while the magnetic
field strength itself has not or barely increased.

---------------------------------------------------------
Title: Maunder Minimum According to New and Archive Data
Authors: Callebaut, D. K.; Makarov, V. I.; Tlatov, A. G.
2005ESASP.600E..49C Altcode: 2005dysu.confE..49C; 2005ESPM...11...49C
No abstract at ADS

---------------------------------------------------------
Title: Indices of Solar Activity in Minimum of Sunspot Cycles
Authors: Tlatov, A. G.; Makarov, V. I.
2005ASPC..346..415T Altcode:
New indices of solar activity in minimum of sunspot cycles were obtained
from the Hα synoptic charts during 1887 - 2004, CaII K
observational data of solar disk during 1907 - 1995 at the Kodaikanal
observatory in India and observations of the Sun at the Kislovodsk
Solar Station in 1950 - 2004. Index Apz determines the area of polar
zone occupied by magnetic field of one polarity and the A(t) is a sum
of squares of dipole and oktopole magnetic moments. Index L(t) is a
general length of magnetic neutral lines on Hα synoptic
chart and the K(t) characterizes the complexity of topology pattern
of general magnetic field of the Sun. It is determined by inverse
number of crossing neutral lines with meridian net on Hα
chart. Index R(t) determines correlation factor of polarity of the
magnetic field in the latitude zones ± 40°. Index of solar rotation
SSPD(t) is determined by a sum of spectral density of the power of
sector structures of the magnetic field. The area of CaII K bright
points at the high - latitudes is the index SK(t). It was shown that
the 11-year cycles of Apz(t), A(t), L(t), K(t), R(t), SSPD(t) and SK(t)
have the maximum in the minimum of sunspot activity and they precede
the Wolf number cycles, W(t), for 5 - 6 years.

---------------------------------------------------------
Title: 22-Year Variations of the Solar Rotation
Authors: Tlatov, A. G.; Makarov, V. I.
2005ASPC..346..409T Altcode:
We have studied the rotation of the solar atmosphere on the basis of
Hα synoptic charts for 117 years (1887 - 2003) and derived
the latitude-time diagrams for variation of the rotation periods in
the interval of latitude ± 45°. We determined the periods within
8 to 12 year “windows”, subsequently shifting the “window” along
the data set, which makes it possible to reveal long-term variations
in the solar rotation. It has been shown, that within the interval of
latitude ± 20°, the basic rotation period of the background magnetic
field of the Sun is 22 years. During odd cycles of solar activity, the
rotation rate decelerates, while during even cycles, more rapid rotation
is observed. When the sampling “window” increases to around 17 years,
the 55 to 60 year quasi - period of rotation can be recognized. In this
case, the maximum rotation velocity falls roughly on years 1930 and
1990. We consider possible generation of the solar cycle by 22-year
period torsion waves interacting with relic magnetic field.

---------------------------------------------------------
Title: The Milli-Arcsecond Pathfinder Survey (MAPS) mission
Authors: Dorland, B.; Zacharias, N.; Gaume, R.; Johnston, K.; Hennessy,
G.; Makarov, V.; Rollins, C.
2005AAS...207.2306D Altcode: 2005BAAS...37.1196D
The Milli-Arcsecond Pathfinder Survey (MAPS) is a U.S. Naval
Observatory-proposed astrometric survey mission designed to observe tens
of millions of stars (and other objects) in the magnitude range 2-14,
with a reference accuracy of &lt; 1 milliarcsecond (mas) position,
&lt; 1 mas/year proper motion, and &lt; 1 mas parallax. For the
about 118,000 Hipparcos stars, new proper motions on the 0.1 mas/yr
level are expected when combining the 1 mas Hipparcos positions at
1991.25 with MAPS data. The instrument consists of a 15-cm, all
reflective telescope and large format, 8k x 8k active pixel sensor (APS)
detector. The instrument will observe a one square degree field of view
(FOV), operating in a step-stare mode. The payload will be carried on
a modular, microsatellite bus and deployed into low earth orbit in
the 2009 time-frame, with a 2-3 year mission life. Astrometry
at the 1 mas level for the 2010 epoch to 14th magnitude enables
astrophysical research not possible from the ground. MAPS will support
a wide variety of astrophysics research. This includes astrometric
detection of potential planets in nearby systems (e.g. Barnard's,
Kapteyn's stars), detection of long-period, low-mass black holes in
accelerating Hipparcos binaries, a search for recent Galactic mergers,
analysis of the internal dynamics of nearby open clusters (Hyades,
Pleiades, Coma Berenices, et al.), dynamics of pre-main-sequence stars
in the nearest star forming regions, quantification of binarity and
kinematics of solar neighborhood stars and measurements of distance
to the Pleiades and other clusters as cosmic distance scale calibrators.

---------------------------------------------------------
Title: Generation of Sunspots and Polar Faculae from a Kinematic
Dynamo
Authors: Callebaut, D. K.; Makarov, V. I.
2005ESASP.600E..48C Altcode: 2005dysu.confE..48C; 2005ESPM...11...48C
No abstract at ADS

---------------------------------------------------------
Title: Magnetic Field Reversal of the Sun in Polarization of
Radioemission at 17GHz
Authors: Tlatov, A. G.; Gelfreikh, G. B.; Makarov, V. I.
2005ASPC..346..281T Altcode:
The distribution of polarized component of the solar radio emission
at wavelength of λ = 1.76 cm over the solar disk was studied using
the observations of the Nobeyama radio heliograph. The latitude-time
diagrams of the circular polarization were constructed for the period
of the years 1992-2003. The method of averaging has been applied for
the noise reduction using several images per day and a filtration
of images. The high-altitude drifts of the polarized radio emission
have been allocated both at latitude band of sunspots and at higher
latitudes. The magnetic field reversal of the large-scale magnetic
field was found as manifested in polarization of radio emission of
the Sun during cycles of solar activity numbers 22-23. The analysis of
polarization of radio emission for the structures of various brightness
temperature has been carried out. Comparison of the radio method of
analysis of the global variation of the solar magnetic fields with the
phase of cycle with the results found from the optical observations
confirmed its effectiveness.

---------------------------------------------------------
Title: The proportion of hot and cold regions in the polar solar
corona during 1957 2002
Authors: Makarov, V. I.; Tlatov, A. G.
2005ARep...49..932M Altcode:
Occultation observations of the intensity of the FeXIV 530.3 nm and FeX
637.4 nm forbidden lines detected at the Kislovodsk Mountain Station
during 1957 2002, indicate long-term changes in the structure of the
solar corona. The monthly average intensities of green (KI530.3) and red
(KI637.4) spectral lines are calculated for all latitudes (0° 90°) and
for a high-latitude zone (45° 90°). A strong correlation (r = 0.91)
between the green KI530.3 line intensity and the Wolf numbers is found
and used to fill gaps in the observations. The ratio KI637.4/KI530.3
takes on its maximum value at the solar minimum. The KI 637.4 p /KI
530.3 p ratio in the high-latitude solar zone (45° 90°) increased
by more than a factor of two during 1957 2002. This means that the
fraction of cool regions in the polar corona has more than doubled
over these years. We suggest that this increase in the number of cool
regions is related to an increase in the area of the polar solar zones
occupied by magnetic field of a single polarity at the solar minimum,
and possibly to an increase in the area occupied by polar coronal
holes. This is associated with long-term variations in the internal
structure of the Sun.

---------------------------------------------------------
Title: Conditions of formation of transpolar coronal holes
Authors: Vasil'eva, V. V.; Makarov, V. I.; Tlatov, A. G.
2005IJGA....6.1006V Altcode: 2005IJGA....6I1006V
[1] The longitudinal distribution of high-latitude coronal holes is
considered. To accomplish the task, polar projections of synoptic
charts of He 10830 Å observations of the Kitt Peak observatory for
the period 1975-2003 were made, and coronal holes were identified
as regions of increased emission. A number of structures could be
interpreted as coronal holes beginning at middle or low latitudes,
reaching the pole, and descending again to the equator along meridians
in another longitudinal interval. Thus such coronal holes are extended
along a meridional line crossing the pole, and their lifetime is several
rotations. Such structures are most distinct 1-2 years after the end
of the polarity reversal of the solar magnetic field in the phase of
solar activity decrease and, in some cases, in the phase of the solar
activity growth. As a rule, at the opposite solar pole, there exist
coronal holes extended along meridional lines in other longitudinal
sectors. Comparison with distribution of magnetic fields for this
period has been performed. The possibility that such coronal holes
can affect recurrent disturbances of geomagnetic indexes is considered.

---------------------------------------------------------
Title: Measurements of brightness and nonradial direction of coronal
streamers according to data of SOHO/Large Angle and Spectrometric
Coronagraph Experiment (LASCO)-C2
Authors: Kim, Gun-Der; Makarov, V. I.; Tlatov, A. G.
2004IJGA....5.2011K Altcode: 2004IJGA....5I2011K
Daily observations of the corona were processed according to the data
of coronagraph SOHO/Large Angle and Spectrometric Coronagraph Experiment
(LASCO)-C2 to study the variations of brightness and nonradial direction
of coronal streamers during 1996.5-2003.5. Photometry of coronal images
was carried out at heights of $2.3~R\odot-5.5~R_{\odot
with a step of 2° along position angle. The total number of processed
days has been about 4300. The latitude-time distributions of coronal
intensity were analyzed at different heights. The maximum brightness of
the corona was observed in the equatorial zone in the solar minimum. The
drifts of coronal intensity were observed in direction to the poles in
the beginning of solar cycle. The maximum brightness of high-latitude
corona was observed during the polar magnetic field reversal of the
Sun in 1999-2001. The drifts of low coronal brightness were observed in
the opposite direction from high latitudes to the equator after polar
magnetic field reversal. The angles of deviation from radial direction
of coronal streamers were determined on daily coronal images. It
was found that coronal streamers were inclined on the whole to the
equator during 1996.5-1999.5, although after 1999.5 the streamers
were inclined to the poles. The angles of nonradial direction of the
streamers reached about 10°-15°. The longitudinal distribution of
coronal brightness at various heights was considered. It was compared
with heliosphere neutral layer and with drift of filament bands in an
epoch of polar magnetic field reversal of the Sun.

---------------------------------------------------------
Title: Long-Term Changes of Polar Activity of the Sun
Authors: Makarov, V. I.; Tlatov, A. G.; Callebaut, D. K.
2004SoPh..224...49M Altcode: 2005SoPh..224...49M
We discuss long-time changes of polar activity of the Sun using the
new observational data sets in the optical range during 1872-2001. A
study of the secular and cycle variations of the magnetic activity at
the high-latitude regions is the main goal that includes polar magnetic
field reversals during 1872-2001 and secular changes of the duration of
polar activity cycles. The secular increase of the area of polar zones
during the minimum activity in the last 120 years and as consequence
a decrease of coronal temperature of the Sun in the high-latitude
zones during the last 50 years. Correlation between the polar cycles
of CaII-K bright points with the Wolf sunspot numbers cycles, W(t),
and the 22-year polar magnetic cycles of CaII-K bright points at the
high latitudes during 1905-1995 is discussed.

---------------------------------------------------------
Title: Brightness of the corona with the height according to
observations of SOHO/EIT during 1996-2003
Authors: Tlatov, A. G.; Makarov, V. I.
2004IAUS..223..399T Altcode: 2005IAUS..223..399T
An analysis of the distribution of coronal brightness in the UV
radiation according to SOHO/EIT in the wavelengths 171Å, 195Å and
304Å was carried out. A change of coronal brightness at the heights
1.02R-1.20R radius of the Sun was considered during 1996-2003. The
distribution of brightness of the corona at the various heights depends
on the phase of the solar cycle. Brightness of the corona at the
heights more 1.05R in the wavelengths 171Å and 195Å has the greatest
brightness during an epoch of the maximum activity. Brightness of the
internal corona at the heights less 1.05R has the lowered brightness
during this period. The maximum intensity of the corona 304Å was
observed in the maximum activity at all heights. Comparison brightness
of the corona with the number bright points in UV was carried out. For
this purpose the bright points in the wavelength 304Å were allocated
on the solar disk of the daily observations. The number of the bright
points has the maximum on the phase of the minimum activity while the
area of the bright regions has maximum in the maximum activity.

---------------------------------------------------------
Title: Magnetic field reversal of the Sun in polarization of
radioemission 17GHz
Authors: Tlatov, A. G.; Makarov, V. I.
2004IAUS..223..145T Altcode: 2005IAUS..223..145T
Polarization of radio emission on the solar disk was studied according
to of Nobeyama radio heliograph observations during 1992-2003. The
latitude-time diagrams of polarization circular radio emission were
constructed. For a decrease of the noises we used several solar images
for a day. We found polarization drifts of radio emission in the
high-latitudes activity and at latitude band of the sunspots. Process
of the magnetic field reversal of the large-scale magnetic field in
polarization of radio emission of the Sun was found during 22-23
cycles. An analysis of polarization for the structures various
brightness temperatures has been carried.

---------------------------------------------------------
Title: 22-years magnetic cycle in polar activity of the Sun
Authors: Makarov, V. I.; Tlatov, A. G.; Singh, J.; Gupta, S. S.
2004IAUS..223..125M Altcode: 2005IAUS..223..125M
We have digitized and processed the daily K-CaII-line full disk
spectroheliograms from the archive of the Kodaikanal Observatory during
1907-1995. The programm has been worked out to determine the boundaries
of the bright areas (plages, decayed plages, enhanced network features,
K-CaII bright points and so on) with contrast that exceeded a level of
the quiet Sun on the given value. About the 1.2 {times} 10^6 K-CaII
active regions of different scales were processed. The coordinates,
areas, the tilt and latitude-time distributions of bright features
were determined. At the high latitudes the K-CaII bright points form a
polar branch of solar activity at the period between the polar magnetic
field reversals. This polar activity shows both 11-year's and 22-year's
cycles. We found that the polar K-CaII bright point cycles proceed on
average 5.5 years the sunspot cycles.

---------------------------------------------------------
Title: Secular and cycle variations of polar activity of the Sun
Authors: Makarov, V. I.; Tlatov, A. G.; Callebaut, D. K.
2004IAUS..223...49M Altcode: 2005IAUS..223...49M
An analysis of polar activity of the Sun was carried out using the
observations in the optical range. The secular and cycle peculiarities
of the magnetic activity on the high latitudes were found: an increase
of the area of polar caps of the Sun, occupied by unipolar magnetic
field at the minimum activity during 1878-2000;a decrease of coronal
temperature at the high-latitude zones during the last 50 years;the
connection between the polar and sunspot activities;outset and duration
of the polar activity cycle;drift of the activity to the poles and
from the poles after the magnetic field reversal.

---------------------------------------------------------
Title: Low-mass Companions to van Maanen 2 and Other Nearby Stars
Authors: Makarov, V.
2003AAS...203.0604M Altcode: 2003BAAS...35.1212M
Most of the presently known low-mass companions and planets in
extrasolar systems have been discovered via a periodic variation
of radial velocity of the primary star. The astrometric method,
although currently less accurate, is an alternative and independent
way to look for brown dwarf and planetary companions. It is based
on the reflex stellar motion caused by the orbital motion in the
system. The astrometric method may provide important information on
the physical size and inclination of the orbit, and, subsequently, a
dynamical estimation of the total and secandary masses. It works fine
for objects that may be difficult for the radial velocity search, e.g.,
very hot primary stars or almost face-on orbits. Using the Hipparcos
Intermediate Astrometry Data, we are conducting a systematic screening
of nearby (distances less than 20-30 pc) stars, paying special attention
to astrometric binaries with considerable accelerations or discrepant
long-term and short-term proper motions. Several new systems have
been discovered with probable brown dwarf or giant planet companions,
including van Maanen 2 (GJ 35), HD 219571, GJ 914A (85 Peg A), GJ 533,
GJ 9616 and GJ 9387. Preliminary astrometric solutions are obtained,
statistical confidence levels are computed, and secondary masses
are estimated. The companion to van Maanen 2 has a mass of about
0.08 Msun, and may be the nearest boundary object between
the classes of brown dwarfs and super-giant planets. It orbits the
nearest cool white dwarf 3.67 Byr of age, at a distance of just 4.4
pc from the Sun. The estimated period is 1.57 yr, and the predicted
semi-amplitude of radial velocity is 0.48 km/s. The maximum separation
between the primary white dwarf and the secondary substellar object
is approximately 0.3 arcsec, which leaves the possibility of direct
imaging of the latter with existing facilities.

---------------------------------------------------------
Title: Relation between "solar magnetic dipole" and filament bands
Authors: Callebaut, D. K.; Makarov, V. I.; Tlatov, A. G.
2003ESASP.535..749C Altcode: 2003iscs.symp..749C
The "solar magnet" consists of several components: (a) the
large-scale unipolar magnetic field regions and their boundaries,
the filament bands; (b) a variable dipole yielding polar plumes;
(c) other effects. The filament bands have a poleward motion (speeds
up to 50 m/s) except for a "recoil" after polar reversal (when the
upper unipolar zone disappears at a pole) and the subsequenc "rest"
during the minimum of solar activity. The filament bands carry huge
currents, which repulse/attract each other. Numerical estimates yield
large accelerations which are roughly compensated by the friction of
the "skin layer" constituting the unipolar regions slipping over the
solar surface as a connected sheet as it is pervaded by a magnetic
field and does not mix with the solar surface. When new large-scale
unipolar zones originate near the equator the additional repulsion
of the filament bands causes the pole-ward motion of the previous
filaments; moreover the upper one interacts with the dipole of the
polar plumes. The surprising "recoil" of the remaining filament bands
may be partially explained by the variation of this dipole and by a
recoil of the "skin layer".

---------------------------------------------------------
Title: Temperature of polar corona of the Sun during the last 50 years
(1952-2001)
Authors: Makarov, V. I.; Tlatov, A. G.; Callebaut, D. K.
2003ESASP.535..217M Altcode: 2003iscs.symp..217M
We investigate the variations of temperature in the polar corona using
the long-term observations of intensity of the coronal lines Fe XIV
530.3 nm and Fe X 637.4 nm at the high latitudes during 1952-2001. We
composed a combined series of the green and red intensities for
1952-2001, using the Kislovodsk data as basis, inserting missing
data from other observatories. The mean monthly coronal intensities
KI5303 and KI6374 have been calculated
in the sunspot (0°-45°) and in the high-latitude (45°-90°)
zones. We found that the average intensity of KI5303
decreased 1.5 times, while the intensity of KI6374
increased 1.7 times at the high-latitude zone during the last 50
years. The ratio KI6374/KI5303 shows the
22-year cycle of temperature of the polar corona. The average value
of KI6374/KI5303 more than doubled during
1957-2001. It corresponds to a decrease of average coronal temperature
at the high latitudes by 0.2×106K. We argue that a decrease
of coronal temperature is connected with the increase (doubling) of the
area of the polar zones Apz occupied by unipolar magnetic
fields (Makarov et al., 2002) and, probably, with an increase of the
area of polar coronal holes.

---------------------------------------------------------
Title: Duration of Polar Activity Cycles and Their Relation to
Sunspot Activity
Authors: Makarov, V. I.; Tlatov, A. G.; Sivaraman, K. R.
2003SoPh..214...41M Altcode:
We have defined the duration of polar magnetic activity as the time
interval between two successive polar reversals. The epochs of the
polarity reversals of the magnetic field at the poles of the Sun
have been determined (1) by the time of the final disappearance
of the polar crown filaments and (2) by the time between the two
neighbouring reversals of the magnetic dipole configuration (l=1)
from the Hα synoptic charts covering the period 1870-2001. It is
shown that the reversals for the magnetic dipole configuration (l=1)
occur on an average 3.3±0.5 years after the sunspot minimum according
to the Hα synoptic charts (Table I) and the Stanford magnetograms
(Table III). If we set the time of the final disappearance of the polar
crown filaments (determined from the latitude migration of filaments)
as the criterion for deciding the epoch of the polarity reversal of the
polar fields, then the reversal occurs on an average 5.8±0.6 years
from sunspot minimum (last column of Table I). We consider this as
the most reliable diagnostic for fixing the epoch of reversals, as the
final disappearance of the polar crown filaments can be observed without
ambiguity. We show that shorter the duration of the polar activity cycle
(i.e., the shorter the duration between two neighbouring reversals),
the more intense is the next sunspot cycle. We also notice that the
duration of polar activity is always more in even solar cycles than
in odd cycles whereas the maximum Wolf numbers W\max is
always higher for odd solar cycles than for even cycles. Furthermore,
we assume there is a secular change in the duration of the polar
cycle. It has decreased by ∼ 1.2 times during the last 120 years.

---------------------------------------------------------
Title: Polar Ring Currents on the sun During a Polar Magnetic Field
Reversal
Authors: Makarov, V. I.; Filippov, B. P.
2003SoPh..214...55M Altcode:
We have studied the variations of the height of polar crown prominences
according to daily observations of the Sun at the Kodaikanal Observatory
(India) during 1905-1975. Polar ring filaments at latitudes 60°-80°
are related to the polar magnetic field reversal. A double decrease of
the height of polar ring filaments was found in the course of their
migration from 40°to the poles. We estimated the limiting height of
the equilibrium of polar ring filaments from the stability condition
of a strong electric current. We found that the transition from
large-scale to small-scale ring filaments reduces the critical height
of the stability for the prominences. A model of an inverse-polarity
filament was used.

---------------------------------------------------------
Title: When does the polar activity cycle start?
Authors: Makarov, V. I.; Tlatov, A. G.; Sivaraman, K. R.
2003AN....324..382M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Polar faculae and sunspot cycles concerning secular variation
of polar magnetic flux
Authors: Makarov, V. I.; Tlatov, A. G.; Callebaut , D. K.
2003AN....324..381M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Secular variation of 1.3-year latitude oscillations of magnetic
zone boundaries during 1915-2000
Authors: Makarov, V. I.; Tavastsherna, K. S.; Tlatov, A. G.; Callebaut,
D. K.
2002ESASP.506..173M Altcode: 2002ESPM...10..173M; 2002svco.conf..173M
We have computed and analyzed the average latitude per solar rotation
of 36 zone boundaries of the large-scale magnetic field, which have
been detected by Hα filaments and prominences during
1915-2000. We have found two types of the latitude oscillations of the
zone boundaries with the quasi-periods of about 1.3 and 2.3-years (17
and 30 solar rotations). We consider that 1.3-year latitude periodicity
of the filament bands connected with the same oscillations at the
tachocline (Komm et al. (2000), Howe et al. (2001)). We have found
the secular variations or an increase of a period of about 1.3-year
oscillations from 1.1 year in 1915 up to 1.4 year in 2000. Second
type of the latitude oscillations is about 2.3-year that concerns
to quasi-biennial cycle. Properties of 1.3 and 2.3-year latitude
oscillations of the filament bands during 1915-2000 are discussed.

---------------------------------------------------------
Title: Deep minimum activity of the Sun and small ice age coming now,
followed by drastic heat
Authors: Callebaut, D. K.; Makarov, V. I.; Tlatov, A. G.
2002ESASP.506..113C Altcode: 2002svco.conf..113C; 2002ESPM...10..113C
We estimate the magnetic activity of the Sun that will decrease
seriously in the next two or three cycles, leading to a deep
minimum. Three arguments are given in favor of this statement. With
the approach of a deep minimum the Earth ocean temperature may
gradually decrease by at least 1°K. However, due to the increase of the
greenhouse effect one may expect during the coming decennia only a small
decrease, say 0.5°K. Nevertheless this may be interpreted wrongly as
if the greenhouse effect is irrelevant and that the present high ocean
temperature is only a casual fluctuation. Governemnts may then allow
an ever increasing use of Earth fuel, leading to an ocean temperature
higher than at present after half a century. After the deep minimum an
extra increase in temperature of at least 1°K is to be expected leading
to drastic, if not catastrophic, effects. It is concluded that (1) more
research on the activity of the Sun is required as well as more research
on the greenhouse effect; (2) the need for nuclear fusion is imperative.

---------------------------------------------------------
Title: Distances of absorbing features in the LDN 1622 direction. An
application of Tycho-2 photometry and Michigan Classification
Authors: Knude, J.; Fabricius, C.; Høg, E.; Makarov, V.
2002A&A...392.1069K Altcode:
With Tycho-2 BT and VT photometry of Hipparcos
stars with π &gt; 8.0 mas, σπ/π &lt; 15% and with
spectral type and luminosity classification from the Michigan
Catalogues we have a presumably unreddened sample for establishing a
(BT-VT_0- MV_T main sequence relation
in the range from A0 to G5. We discuss the location of the median
main sequence relation relative to published ZAMS relations for the
A0-G5 range in some detail since the applications of this relation
will have to assume that the evolutionary status of the calibration
sample is representative of the local disk. If the ZAMS is defined
as the lower envelope of the class V stars the published versions we
discuss seem to be too bright by about half a magnitude in the F0-G5
range. The resulting intrinsic color and absolute magnitude estimates
have errors of the mean of 0.03m and 0.3m-0.4m respectively. From this
relation any given star with Tycho-2 photometry, spectral classification
and luminosity class V can have its color excess E(BT -
VT) and distance modulus estimated. This means that the local
interstellar extinction may be estimated for the ~50% of the sky where
Michigan classification presently is available. The individual color
excesses and distance moduli may not be particularly accurate but we
propose that they may be used to indicate extinction discontinuities
caused by interstellar material at well defined distances. We have
applied this new technique on stars from the Michigan Catalogue in
the direction of LDN 1622 (l, b) = (204.7dg, -11.8dg) supposed to be
associated to the Orion B region 400-500 pc away but color excesses
E(BT - VT) exceeding 0.15m start appearing already
in the distance slot 160-200 pc. Presently we cannot decide whether this
nearby dust is related to LDN 1622 or whether this cloud is associated
to Orion B. In a final comparison we study the color excess -- distance
variation in a 4 deg region centered on LDN 1622 from Hipparcos --
Tycho-1 -- Michigan data and the dust at ~160 pc is confirmed.

---------------------------------------------------------
Title: A study of the development of global solar activity in the
23rd solar cycle based on radio observations with the Nobeyama radio
heliograph. I. Latitude distribution of the active and dark regions
Authors: Gelfreikh, G. B.; Makarov, V. I.; Tlatov, A. G.; Riehokainen,
A.; Shibasaki, K.
2002A&A...389..618G Altcode:
Daily radio maps of the Sun at the wavelength of 1.76 cm were used to
analyze the parameters of solar activity at all heliographic latitudes
for the period 1992-2001. As a criterion of the level of solar activity,
we analyzed the area/number of regions with an excess of brightness
above a certain fixed level as well as regions with brightness below a
certain level. The distribution of such “bright” and “dark” regions
with heliographic latitude as function of time was found. Special
attention was paid to the high latitude polar regions where the ways
of analyzing solar activity are rather limited and have no generally
accepted methods. The results are compared with some other indices
of high latitude solar activity, such as polar faculae and magnetic
field measurements. They appear to be in general agreement with the
radio observations. The advantage of using radio observations is a
more homogeneous database and a stable method of analysis.

---------------------------------------------------------
Title: A study of development of global solar activity in the 23rd
solar cycle based on radio observations with the Nobeyama radio
heliograph. II. Dynamics of the differential rotation of the Sun
Authors: Gelfreikh, G. B.; Makarov, V. I.; Tlatov, A. G.; Riehokainen,
A.; Shibasaki, K.
2002A&A...389..624G Altcode:
An analysis of solar rotation as a function of heliographic latitude
and time is made using daily radio maps of the Sun at the wavelength
of 1.76 cm. Variations of the velocity as a function of the latitude
during the period 1992-2001 have been studied. The mean synodical
rotation rate of the intensity features is best fit by ω = 13.41 -
1.66\sin2 θ -2.19 \sin4 θ (deg/day) where
theta is the latitude. We have found alternating bands of faster and
slower rotation. They travel from higher latitudes towards the equator
during the current solar cycle. Radio observations with high accuracy
and reliability thus confirm the reality of torsional oscillations in
the higher levels of the solar atmosphere.

---------------------------------------------------------
Title: Increase of the Magnetic Flux From Polar Zones of the sun in
the Last 120 Years
Authors: Makarov, V. I.; Tlatov, A. G.; Callebaut, D. K.; Obridko,
V. N.
2002SoPh..206..383M Altcode:
Lockwood, Stamper, and Wild (1999) argued that the average strength of
the magnetic field of the Sun has doubled in the last 100 years. They
used an analysis of the geomagnetic index «aa». We calculated the
area of polar zones of the Sun, Apz, occupied by unipolar
magnetic field on Hα synoptic magnetic charts, following Makarov
(1994), from 1878 to 2000. We found a gradual decrease of the annual
minimum latitude of the high-latitude zone boundaries, θ2m,
of the global magnetic field of the Sun at the minimum of activity from
53° in 1878 down to 38° in 1996, yielding an average decrease of 1.2°
per cycle. Consequently the area of polar zones Apz of the
Sun, occupied by unipolar magnetic field at the minimum activity, has
risen by a factor of 2 during 1878-1996. This means that the behavior
of the index «aa» and consequently the magnetic flux from the Sun
may be explained by an increase of the area of polar caps with roughly
the same value of the magnetic field in this period. The area of the
unipolar magnetic field at the poles (Apz) may be used as a
new index of magnetic activity of the Sun. We compared Apz
with the «aa», the Wolf number «W» and «A»* -index
(Makarov and Tlatov, 2000). Correlations based on `11-year' averages
are discussed. A temperature difference of about 1° between the
Maunder Minimum and the present time was deduced. We have found that
the highest latitude of the polar zone boundaries of the large-scale
magnetic field during very low solar activity reaches about 60°, cf.,
the Maunder Minimum. It is supposed that the θ2m-latitude
coincides with the latitude where ∂rω=0, with ω(r,θ)
being the angular frequency of the solar rotation. The causes of the
waxing and waning of the Sun's activity in conditions like Maunder
Minimum are discussed.

---------------------------------------------------------
Title: Gravitational energy, solar radius and solar cycle
Authors: Callebaut, Dirk K.; Makarov, Valentine I.; Tlatov, Andrej G.
2002ESASP.477..209C Altcode: 2002scsw.conf..209C
A self-consistent approach is used. From the change (1.2
W/m2) in the solar constant (1367 W/m2)
during a solar cycle we deduced a relation between the change in
solar radius ΔR and the depth d = (1-α)R in the convection zone
where the expansion starts. A second relation is obtained by equating
the gravitational energy required for the expansion and the decrease
in luminosity during half a solar cycle. This yields values for ΔR
≍ 8 km, d ≍ 0.96R (super-granular region) and for the change in
gravitational energy ΔE ≍ 1032J. Similar considerations
are made for the Maunder Minimum yielding ΔR ≍ 60 km, d ≍ 0.94R
and ΔE ≍ 1033J. There is some change, say 40 per cent,
if we use a quadratic expansion instead of a linear one. Moreover this
theory suits a qualitative explanation why the Sun expands during a
minimum of the magnetic activity.

---------------------------------------------------------
Title: Rotation Cycles of the Sector Structure of the Solar Magnetic
Field and Its Activity
Authors: Vasil'Eva, V. V.; Makarov, V. I.; Tlatov, A. G.
2002AstL...28..199V Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On a decrease of high-latitude corona temperature of the Sun
in the last 50 years
Authors: Makarov, V. I.; Tlatov, A. G.
2002ESASP.477..241M Altcode: 2002scsw.conf..241M
The ground-based observations of the green Fe XIV 5303 Å and red
Fe X 6374 Å corona forbidden lines obtained at the Kislovodsk Solar
Station since 1952 are used to determine the temperature variations
of the solar corona. The observations of the solar corona at the
Arosa, Pic du Midi, Kislovodsk, Norikura, Kanzelhöhe, Wendelstein
and Lomnický Stit have been used to receive the Kislovodsk series
of the green K I5303 and red K I6374 corona
intensities for 1947-2000. Comparison of the K I5303
with the Wolf numbers W(t) shows high correlation factor 0.91. The
mean monthly corona intensity has been calculated in the sunspot
(0° - 45°) and at the high-latitude (45° - 90°) zones. We found a
decrease of the K I5303 in 1.5 times at the high-latitudes
in this period. It was shown that the ratio K I6374/K
I5303 increased more than two times. We have found a decrease
of temperature in polar zones of the Sun of order 0.1×106
during the last 50 years. It is supposed that a decrease of polar
corona temperature connected with an increase of magnetic flux from
high-latitude regions of the Sun during the last 120 years.

---------------------------------------------------------
Title: Long-term variations of polar magnetic flux of the Sun and
terrestrial climate
Authors: Makarov, V. I.; Tlatov, A. G.; Callebaut, D. K.; Obridko,
V. N.
2002ESASP.477..563M Altcode: 2002scsw.conf..563M
We calculated the area of polar zones of the Sun, Apz, occupied by
unipolar magnetic field on Hα synoptic magnetic charts,
following Makarov (1994), from 1878 to 2000. We found a gradual decrease
of the annual latitude of the high-latitude zone boundaries of the
global magnetic field of the Sun at the minimum of activity from 53°
in 1878 down to 38° in 1996, yielding an average decrease of 1.2° per
cycle. We found that the area of polar zones of the Sun Apz has risen by
a factor of 2 during 1878-1996. The area of the unipolar magnetic field
at high-latitudes Apz may be used as a new index of magnetic activity of
the Sun. We compared Apz with the geomagnetic index and Wolf number. A
temperature difference of about 1.3° between the Maunder Minimum and
the present time was deduced. The causes of the waxing and waning of
the Sun's activity in conditions like Maunder Minimum are discussed.

---------------------------------------------------------
Title: Pole-ward motion and recoils of the boundaries of unipolar
regions
Authors: Callebaut, Dirk K.; Makarov, Valentine I.; Tlatov, Andrej G.
2002ESASP.477...87C Altcode: 2002scsw.conf...87C
The large-scale unipolar zones have boundaries which practically
coincide with filament bands encircling the whole Sun. Huge currents
flow in these filament bands, which attract or repulse each other. When
new unipolar zones are generated near the equator and thus new filament
bands appear after a while. The previously existing filament bands feel
a new repulsion/attraction and their pole-ward motion starts. When
a filament band reaches a pole and disappears (pole reversal) it
releases the amount of "surface mass" it was holding and this pushes
the other filament bands somewhat back, causing a "recoil". A more
or less stationary situation may result as e.g. in the second half of
the sunspot cycle (after a polar reversal), in wich the filament bands
move slightly back and forth of their "equilibrium" latitude. Numerical
estimates give reasonable acceleration and velocities, provided the
filament bands are loaded by much more mass they carry themselves:
indeed they are anchored in the regions of unipolar field and thus
form a connected piece like a sheet which may slip over the Sun.

---------------------------------------------------------
Title: JOSO national report 2000-2001 - Russia
Authors: Makarov, V. I.
2002joso.book...93M Altcode:
Solar physics research in Russia is carried out at the several
observatories and universities. We show the most important solar
physics events during 2000-2001.

---------------------------------------------------------
Title: Full-sky Astrometric Mapping Explorer (FAME) Rescope Activities
Authors: Johnston, K.; Dorland, B.; Gaume, R.; Hajian, A.; Harris, F.;
Harris, H.; Hennessy, G.; Kaplan, G.; Levine, S.; Monet, D.; Munn, J.;
Murison, M.; Pier, J.; Urban, S.; Zacharias, N.; Seidelmann, P. K.;
Lee, J.; Makarov, V.; Olling, R.; Codella, T.; Geary, J.; Latham,
D.; Phillips, J.; Johnson, M.; Vassar, R.; Horner, S.
2001AAS...199.4504J Altcode: 2001BAAS...33.1367J
The Full-sky Astrometric Mapping Explorer (FAME) will measure the
positions, proper motions, parallaxes, and photometry for 40 million
stars between 5 and 15 magnitude, with accuracies of 50 microarcseconds
at 9th magnitude and degraded accuracy for fainter stars as faint
as 15 magnitude. The mission is planned for an October 2004 launch
and a five-year duration. The FAME mission has progressed in its
development. Due to budget, weight, and power limitations, the FAME
architecture has been rescoped so that it will satisfy the budget
limitations and retain the basic science objectives of the mission. The
new design and characteristics, the status of developments and tests,
and the scientific baseline and minimum mission requirements are
presented.

---------------------------------------------------------
Title: The increase in the magnetic flux from the polar regions of
the Sun over the last 120 years
Authors: Makarov, V. I.; Obridko, V. N.; Tlatov, A. G.
2001ARep...45..746M Altcode:
The latitudes of the zonal boundaries of the global magnetic field of
the Sun are determined from the magnetic neutral lines on synoptic Hα
maps obtained during 1878 1999. The area of the polar zone occupied
by magnetic field of a single polarity at solar minima has doubled
over the last 120 years. This provides an explanation for the secular
increase in heliospheric characteristics, which differs from the
two-fold increase of the magnetic field strength predicted for this
period. The temporal variations of the magnetic flux from the polar
regions and their role in global changes of the Earth’s climate are
discussed in connection with secular variations in the structure of
the internal magnetic field of the Sun.

---------------------------------------------------------
Title: Does the Poleward Migration Rate of the Magnetic Fields Depend
on the Strength of the Solar Cycle?
Authors: Makarov, V. I.; Tlatov, A. G.; Sivaraman, K. R.
2001SoPh..202...11M Altcode:
We present the pattern of the polar magnetic reversal for cycle 23
derived from Hα synoptic charts and have also included the reversals
of the earlier cycles 18-22 for comparison. At the beginning of a
new cycle (i.e., soon after the polar reversal) the zonal boundaries
of unipolar magnetic regions of opposite polarities (seen as filament
bands on the synoptic charts) appear close to and on either side of the
equator continuing through the years of minimum indicating the onset
of the cancellation of flux at these low latitudes. The cycle thus
starts with cancellation of flux close to the equator and ends with the
polar reversal or flux cancellation near the poles. The filament bands
just below the polemost ones migrate and reach latitudes 35°-45° by
the time of polar reversal and become the polemost, once the polar
reversal has taken place. During the years of minimum that follow,
these filament bands remain more or less stagnant at the latitudes
35°-45° except for occasional slow migration towards the equator. The
migration to the poles starts at a low speed of 3 m s−1
only when the spot activity has risen to a significant level and then it
accelerates to 30 m s−1 at the peak of the activity. It
takes 3-4 years for the polemost bands to reach the poles moving
at these high speeds. We quantify this possible cause and effect
phenomenon by introducing the concept of the `strength of the solar
cycle' and represent this by either of a set of three parameters. We
show that the velocity of poleward migration is a linear function of
the `strength of the solar cycle'.

---------------------------------------------------------
Title: VizieR Online Data Catalog: The AC 2000.2 Catalogue (Urban+
2001)
Authors: Urban, S. E.; Corbin, T. E.; Wycoff, G. L.; Hoeg, E.;
Fabricius, C.; Makarov; v. v.
2001yCat.1275....0U Altcode:
The AC 2000.2 is a revised version of the 1997 release of the AC 2000
(Cat. &lt;I/247&gt;). It was decided that the availability of an
improved reference catalogue and the inclusion of photometry from the
Tycho-2 catalogue would be sufficient to warrant a complete re-reduction
of the data and a new distribution of the catalogue. The AC 2000.2
catalog contains positions of 4,621,751 stars at the average epoch of
plate exposures for each star (average 1907). (17 data files).

---------------------------------------------------------
Title: Millimeter-radio, SOHO/EIT 171 Å features and the polar
faculae in the polar zones of the Sun
Authors: Riehokainen, A.; Urpo, S.; Valtaoja, E.; Makarov, V. I.;
Makarova, L. V.; Tlatov, A. G.
2001A&A...366..676R Altcode:
In this work we study different manifestations of activity in the polar
zones of the Sun in order to gain understanding on the phenomenon of
enhanced radio temperature regions (ETR) at high solar latitudes. We
have obtained simultaneous radio and optical data during 9 days in
1997. The radio data from the Metsähovi radio telescope, Finland,
consisted of 37 GHz and 87 GHz solar maps. White light observations at
the Kislovodsk solar mountain station in Russia were used to measure the
coordinates of polar faculae groups and diffuse bright structures. We
also compared our data with the 171 Å EUV SOHO/EIT images for the
same time periods. We find the ETRs in general coincide with the
relatively dark areas seen in the SOHO/EIT images. Bright structures
in the SOHO/EIT maps are, in general, encircled by the polar faculae
groups and diffuse bright structures visible in white light. Some of the
EUV bright structures appear to be bases of solar plumes. Connections
between ETRs and polar faculae are complicated; sometimes polar faculae
groups and diffuse bright structures are situated around the ETR
maxima or at their borders, sometimes we see the polar faculae groups
distributed over the whole ETR area. Some faint ETRs appear to have no
associated polar faculae. However, in general there is a correlation
between the ETRs, the polar faculae groups, and the bright structures
(bases of the plumes and some other features), indicating that they
are different manifestations of the same underlying activity. It is
possible that magnetic loops in the active areas, traced by the polar
faculae, are responsible for the observed radio enhancements.

---------------------------------------------------------
Title: Large-Scale Magnetic Field and Sunspot Cycles
Authors: Makarov, V. I.; Tlatov, A. G.; Callebaut, D. K.; Obridko,
V. N.; Shelting, B. D.
2001SoPh..198..409M Altcode:
Hα magnetic synoptic charts of the Sun are processed for 1915-1999 and
the spherical harmonics are calculated. It is shown that the polarity
distribution of the magnetic field on Hα charts is similar to the
polarity distribution of the Stanford magnetic field observations
during 1975-1999. The index of activity of the large-scale magnetic
field A(t), representing the sum of the intensities of dipole and
octupole components, is introduced. It is shown that the cycle of
the large-scale magnetic field of the Sun precedes on the average by
5.5 years the sunspot activity cycle, W(t). This means that the weak
large-scale magnetic fields of the Sun do not result from decay and
diffusion of strong fields from active regions as it is supposed in
all modern theories of the solar cycle. On the basis of the new data
the intensity of the current solar cycle 23 is predicted and some
aspects of the theory of the solar cycle are discussed.

---------------------------------------------------------
Title: The neutral lines of the large-scale magnetic field and
sunspot cycle
Authors: Makarov, V. I.; Tlatov, A. G.
2001ESASP.464..111M Altcode: 2001soho...10..111M
H-alpha magnetic charts describe real structures of the solar magnetic
fields with their topological properties. There are a few morphological
characteristics to describe this topology, among them are the length of
the magnetic neutral lines, l(φ,θ). The total length of the neutral
lines on the H-alpha charts, L = Σ02πl(φ,θ)
as a new index of solar activity was calculated for 1915-1999. It was
shown that L(t) reaches maximum in a top of cycle and it has minimum
in absence of sunspots. The value L(t) was increased by 1.3 since 1915
up to 1999. It was found that the index K(t) = L-1(t) - &lt;
L-1(t) &gt; in the minimum of the cycle seems to be in good
agreement with the sunspot areas of the next sunspot cycle. It was shown
that the index K(t) and Wolf numbers, W(t), are in antiphase and the
maximum of K(t) precedes to one of W(t) with shift-time 5.5 yrs. It
means that the large-scale magnetic fields are primary regarding the
sunspot magnetic fields and they do not result from the dispersal and
transport of old active region magnetic fluxes. New index of solar
activity, K(t), may be used in the periods of absence of sunspots, as
a deepest minimum of K(t) was observed before the highest sunspot cycle.

---------------------------------------------------------
Title: Poleward migration rate of the magnetic fields and the power
of the solar cycle
Authors: Makarov, V. I.; Tlatov, A. G.; Callebaut, D. K.; Sivaraman,
K. R.
2001ESASP.464..115M Altcode: 2001soho...10..115M
We show that the velocity of poleward migration of the magnetic fields
is a linear function of the "strength of the solar cycle". We introduce
a new index "the strength of the solar cycle" and represent this
quantitatively by the two parameters: Σminrev
Ssp - summation of all the annual means of sunspot areas
Ssp of the cycle for the N and S hemispheres separately
starting from the lowest value of the annual mean in Ssp in
the minimum phase all the way to the year of the polarity reversal and
Σminrev W - summation of the Wolf numbers as done
for Σminrev Ssp but over the entire
visible hemisphere. Each of these parameters according to us represents
the "strength of the solar cycle" although they are not independent
of each other. We also discuss some questions regarding the role of
the meridional circulation in transporting the fields towards the poles.

---------------------------------------------------------
Title: The Large-Scale Solar Magnetic Field and 11-Year Activity
Cycles
Authors: Makarov, V. I.; Tlatov, A. G.
2000ARep...44..759M Altcode:
Magnetic Hα synoptic maps of the Sun for 1915 1999 are analyzed
and the intensities of spherical harmonics of the large-scale solar
magnetic field computed. The possibility of using these Hα maps
as a database for investigations of long-term variations of solar
activity is demonstrated. As an example, the magnetic-field polarity
distribution for the Hα maps and the analogous polarity distribution
for the magnetographic maps of the Stanford observatory for 1975 1999
are compared. An activity index A(t) is introduced for the large-scale
magnetic field, which is the sum of the magnetic-moment intensities
for the dipole and octupole components. The 11-year cycle of the
large-scale solar magnetic field leads the 11-year sunspot cycle
by, on average, 5.5 years. It is concluded that the observed weak
large-scale solar magnetic field is not the product of the decay of
strong active-region fields. Based on the new data, the level of the
current (23rd) solar-activity cycle and some aspects of solar-cycle
theory are discussed.

---------------------------------------------------------
Title: The Large-scale Magnetic Field and Sunspot Cycles
Authors: Makarov, V. I.; Tlatov, A. G.
2000JApA...21..161M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Polar Magnetic Field Reversals of the Sun in Maunder Minimum
Authors: Makarov, V. I.; Tlatov, A. G.
2000JApA...21..193M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Gravitational Energy of Solar Oscillations and Climatic Changes
Authors: Callebaut, D. K.; Callebaut, D. K.; Makarov, V. I.; Tlatov,
A. G.
2000ESASP.463..297C Altcode: 2000sctc.proc..297C
No abstract at ADS

---------------------------------------------------------
Title: Polar Activity and Magnetic Field Reversal in Current Solar
Cycle 23
Authors: Makarov, V. I.; Makarova, V. V.; Tlatov, A. G.; Callebaut,
D. K.; Sivaraman, K. R.
2000ESASP.463..367M Altcode: 2000sctc.proc..367M
No abstract at ADS

---------------------------------------------------------
Title: Modern Understanding of the Solar Activity Cycle as a Global
Process from Optical and Radio Observations
Authors: Gelfreikh, G. B.; Makarov, V. I.; Tlatov, A. G.
2000PCEC...25..437G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On Polar Magnetic Field Reversals of the Sun including the
Maunder Minimum
Authors: Makarov, V. I.; Callebaut, D. K.
1999ESASP.448..117M Altcode: 1999mfsp.conf..117M; 1999ESPM....9..117M
No abstract at ADS

---------------------------------------------------------
Title: On the Large-Scale Magnetic Field and Sunspot Cycles
Authors: Makarov, V. I.; Tlatov, A. G.
1999ESASP.448..125M Altcode: 1999mfsp.conf..125M; 1999ESPM....9..125M
No abstract at ADS

---------------------------------------------------------
Title: Polar Activity of the Sun in the New Global Solar Cycle 23
Authors: Makarov, V. I.; Makarova, V. V.
1999ESASP.448..121M Altcode: 1999mfsp.conf..121M; 1999ESPM....9..121M
No abstract at ADS

---------------------------------------------------------
Title: Solar torsional oscillations and the grand activity cycle
Authors: Kitchatinov, L. L.; Pipin, V. V.; Makarov, V. I.; Tlatov,
A. G.
1999SoPh..189..227K Altcode:
Some consequences of a nonlinear coupling between magnetic field and
rotation are studied within a solar type 2D dynamo model for a spherical
convective shell. The magnetic feedback on the rotation law produces
two main effects. First, the torsional oscillations are excited. Second,
a long-term amplitude modulation of the dynamo cycles is produced. The
latter may be identified with the grand cycle of solar activity. The
dynamo model seems to be in accord with the phase relations between
the torsional and magnetic activity oscillations observed in the
11-year cycle as well as in the 55-year grand cycle. It, however,
fails to reproduce the observationally suggested global decreasing
trend in the equatorial rotation rate.

---------------------------------------------------------
Title: Polar Magnetic Field Depth as Derived from SoHO EIT Polar
Plumes Observations
Authors: Makarov, V. I.; Callebaut, D. K.; Cugnon, P.
1999ASPC..184..334M Altcode:
The polar corona of the Sun was analysed using the SoHO EIT images at
17.1 nm during June 1, 1997 - June 24, 1998 and the solar eclipses
during 1871 - 1997. The depth of the "solar magnet" (SM) or q(t,r)
as the distance from the center of the Sun to the intersection of the
tangents to the polar coronal plumes at their base at the limb was
found. According to the eclipse observations q(t,r) is about (0.45 +/-
0.05) R_sun in the solar maximum and (0.65 +/- 0.05) R_sun in the solar
minimum. According to the SoHO observations q(N) = (0.67 +/- 0.02)
R_sun and q(S) = (0.71 +/- 0.02) R_sun during the minimum activity
for 1996, March - October (N for North, S for South). With increase
of the solar activity in 1997-1998 the value of q(N,t,r) decreases to
(0.52 +/- 0.02) R_sun in the Northern hemisphere and to (0.40 +/- 0.02)
R_sun in the Southern hemisphere whereas the Wolf number increases from
12 to 70.0. A North-South asymmetry Q(t,r) = q(N) - q(S) = - 0.06 (solar
radius as unit) has been negative during June 1, 1997 - February 10,
1998 and then it gradually increased and attained a maximum Q(t,r) =
0.17 in mid of May, 1998. An anticorrelation between &lt; q(N) - q(S),
W(N)-W(S) &gt; and &lt; W(t), q (t,r) &gt; was found. The relationship
between the depth of the "solar magnet" and polar ring - filaments
is discussed.

---------------------------------------------------------
Title: Fields and currents in solar ring filaments.
Authors: Callebaut, D. K.; Makarov, V. I.
1999joso.proc..158C Altcode:
Some ring filaments encircle the whole Sun and shrink to encircle
a polar cap. The use of conservation laws and of the equations of
Maxwell allows to construct an approximate model which is nearly
fully consistent. The observations show that the height of a filament
encircling a polar cap and approaching the pole, lowers somewhat. The
authors' theoretical model agrees with this observation when taking
energy losses (due to eruptions) into account. However the observations
show that essentially the (small) poloidal component of the magnetic
field is drastically reduced after an eruption, which requires a
further, more detailed modelling of the discontinuous dissipation
process. Moreover it is suggested that these ring filaments when
encircling a polar cap are connected with the polar plumes in coronal
holes. This entails that these ring filaments are related to the
so-called solar magnet.

---------------------------------------------------------
Title: Fine structure of polar faculae.
Authors: Makarov, V. I.; Okunev, O. V.; Pravdjuk, L. M.; Kneer, F.
1999joso.proc..151M Altcode:
Using photoheliograms with high spatial resolution (SSSO) it was found
that polar faculae consists of a few fine structure elements with the
sizes ranging from 200 km to 400 km (the telescopic resolution limit
is about 180 km). Presumably, polar faculae are caused by magnetic
flux concentrations and their shape reminds of the set of flux tubes.

---------------------------------------------------------
Title: Oscillatory motions in the corona.
Authors: Callebaut, D. K.; Makarov, V. I.
1999joso.proc..120C Altcode:
Intensity observations of the green line Fe XIV 530.3 nm in the solar
corona were combined from various observatories to yield a continuous
set of data from pole to pole during the period 1940 to 1993. 5 pairs of
bands in each hemisphere evolving from the poles towards the equator
were obtained. The authors' preliminary interpretation that this
corresponds to torsional oscillations moving from the poles to the
equator turned out to be difficult to combine with their own previous
work on the poleward motion of filaments and global polarity regions
(Callebaut and Makarov, 1992). Hence the authors rather interpret the
observations as representing the variation of the activating elements
like magnetic fields in and around the solar surface, instead of real
motions of the corona itself.

---------------------------------------------------------
Title: A sophisticated lander for scientific exploration of Mars:
scientific objectives and implementation of the Mars-96 Small Station
Authors: Linkin, V.; Harri, A. -M.; Lipatov, A.; Belostotskaja, K.;
Derbunovich, B.; Ekonomov, A.; Khloustova, L.; Kremnev, R.; Makarov,
V.; Martinov, B.; Nenarokov, D.; Prostov, M.; Pustovalov, A.; Shustko,
G.; Järvinen, I.; Kivilinna, H.; Korpela, S.; Kumpulainen, K.; Lehto,
A.; Pellinen, R.; Pirjola, R.; Riihelä, P.; Salminen, A.; Schmidt,
W.; Siili, T.; Blamont, J.; Carpentier, T.; Debus, A.; Hua, C. T.;
Karczewski, J. -F.; Laplace, H.; Levacher, P.; Lognonné, Ph.; Malique,
C.; Menvielle, M.; Mouli, G.; Pommereau, J. -P.; Quotb, K.; Runavot,
J.; Vienne, D.; Grunthaner, F.; Kuhnke, F.; Musmann, G.; Rieder, R.;
Wänke, H.; Economou, T.; Herring, M.; Lane, A.; McKay, C. P.
1998P&SS...46..717L Altcode:
A mission to Mars including two Small Stations, two Penetrators
and an Orbiter was launched at Baikonur, Kazakhstan, on 16 November
1996. This was called the Mars-96 mission. The Small Stations were
expected to land in September 1997 (L s approximately
178°), nominally to Amazonis-Arcadia region on locations (33 N, 169.4
W) and (37.6 N, 161.9W). The fourth stage of the Mars-96 launcher
malfunctioned and hence the mission was lost. However, the state of
the art concept of the Small Station can be applied to future Martian
lander missions. Also, from the manufacturing and performance point
of view, the Mars-96 Small Station could be built as such at low
cost, and be fairly easily accommodated on almost any forthcoming
Martian mission. This is primarily due to the very simple interface
between the Small Station and the spacecraft. The Small Station is a
sophisticated piece of equipment. With the total available power of
approximately 400 mW the Station successfully supports an ambitious
scientific program. The Station accommodates a panoramic camera,
an alpha-proton-x-ray spectrometer, a seismometer, a magnetometer,
an oxidant instrument, equipment for meteorological observations,
and sensors for atmospheric measurement during the descent phase,
including images taken by a descent phase camera. The total mass of
the Small Station with payload on the Martian surface, including
the airbags, is only 32 kg. Lander observations on the surface of
Mars combined with data from Orbiter instruments will shed light on
the contemporary Mars and its evolution. As in the Mars-96 mission,
specific science goals could be exploration of the interior and surface
of Mars, investigation of the structure and dynamics of the atmosphere,
the role of water and other materials containing volatiles and in situ
studies of the atmospheric boundary layer processes. To achieve the
scientific goals of the mission the lander should carry a versatile set
of instruments. The Small Station accommodates devices for atmospheric
measurements, geophysical and geochemical studies of the Martian surface
and interior, and cameras for descent phase and panoramic views. These
instruments would be able to contribute remarkably to the process of
solving some of the scientific puzzles of Mars.

---------------------------------------------------------
Title: Meteorological observations on Martian surface : met-packages
of Mars-96 Small Stations and Penetrators
Authors: Harri, A. -M.; Linkin, V.; Polkko, J.; Marov, M.; Pommereau,
J. -P.; Lipatov, A.; Siili, T.; Manuilov, K.; Lebedev, V.; Lehto, A.;
Pellinen, R.; Pirjola, R.; Carpentier, T.; Malique, C.; Makarov, V.;
Khloustova, L.; Esposito, L.; Maki, J.; Lawrence, G.; Lystsev, V.
1998P&SS...46..779H Altcode:
The scientific objectives of a meterological experiment on the
Martian surface are defined, and the meteorological equipment
of the landing elements of the Mars-96 mission are described
with emphasis on the applicability for re-use in forthcoming Mars
missions. The general strategy for atmospheric surface observations
is discussed. Meteorological surface observations are of utmost value
in studying the Martian atmosphere. The climatological cycles and
atmospheric circulations, as well as the boundary layer phenomena can
be understood thoroughly only, if the contribution of in situ surface
measurements are amalgamated with the remote observations. The Mars-96
mission had an ambitious goal of deploying four versatile payloads
at four Northern hemispheric sites. The observations of pressure,
temperature, wind, atmospheric optical thickness and humidity, as
well as pressure and temperature measurements during the atmospheric
descent were included in the meteorology experiment. Even though the
Mars-96 mission was unsuccessful, the objectives and implementation of
the meteorology experiment are applicable to any forthcoming landing
mission to Mars. This applies both to a mission having a number of
observation sites spread all over the surface of Mars, and to a single
lander or rover. The main operational objective of this meteorological
experiment is to provide a regular time series of the meteorological
parameters with accelerated measurement campaigns during dawn and
dusk. Such a data set would substantially improve our understanding
of the atmospheric structure, dynamics, climatological cycles, and the
atmosphere-surface interactions. The implementation of the meteorology
instrument features advanced sensor technology and flexible system
design. The application on the Mars-96 landing elements was, however,
severely constrained by the limited power supply. The usefulness of
the system can be substantially enhanced by modest additional resources
and with few or no design modifications.

---------------------------------------------------------
Title: Polar Activity of the Coming Global Solar Cycle 23
Authors: Makarov, V. I.; Makarova, V. V.
1998ASPC..140..347M Altcode: 1998ssp..conf..347M
No abstract at ADS

---------------------------------------------------------
Title: On the Inner Magnetic Field of the Sun in the Global Magnetic
Cycle
Authors: Makarov, V. I.
1998ASPC..140...83M Altcode: 1998ssp..conf...83M
No abstract at ADS

---------------------------------------------------------
Title: Large-Scale Patterns of Prominences in the Global Solar Cycles
During 1880-1995
Authors: Callebaut, D. K.; Makarov, V. I.; Tavastsherna, K. S.
1998ASPC..150..442C Altcode: 1998IAUCo.167..442C; 1998npsp.conf..442C
No abstract at ADS

---------------------------------------------------------
Title: On The Relationship Between Current and Magnetic Field in
Ring-Filaments
Authors: Callebaut, D. K.; Makarov, V. I.
1998ASPC..150..111C Altcode: 1998IAUCo.167..111C; 1998npsp.conf..111C
No abstract at ADS

---------------------------------------------------------
Title: Torsional Oscillation Pattern in the Large - Scale Magnetic
Field (1910 - 1993) and in the Solar Corona (1940 - 1993)
Authors: Makarov, V. I.; Tlatov, A. G.; Callebaut, D. K.
1998ASPC..140...65M Altcode: 1998ssp..conf...65M
No abstract at ADS

---------------------------------------------------------
Title: Spectro-Polarimetry of Polar Faculae
Authors: Homann, T.; Kneer, F.; Makarov, V. I.
1997SoPh..175...81H Altcode:
This contribution deals with the properties of small-scale
magnetic elements at the polar caps of the Sun. Spectro-polarimetric
observations, obtained with high spatial resolution with the Gregory
Coudé Telescope at the Observatorio del Teide on Tenerife, were
analysed. We find, though with limited data sets, that polar faculae
differ in two aspects from faculae of the network in non-active
regions near the equator (equatorial faculae): (1) Polar faculae
appear to have the same magnetic polarity as the general polar magnetic
field. Presumably, the latter is rooted in the small-scale faculae. The
equatorial faculae show both magnetic polarities. (2) Polar faculae,
with a size of 3.5” ± 1.3”, are larger than equatorial faculae with
2.1” ± 0.4”. Yet as for equatorial faculae, polar faculae possess
kilogauss magnetic fields.

---------------------------------------------------------
Title: Torsional oscillations in the solar corona
Authors: Makarov, V. I.; Tlatov, A. G.
1997AZh....74..615M Altcode:
The dependence of the differential rotation of the solar corona on
latitude and time is investigated using observations in the Fe XIV 5303
A line from 1940 to 1992. Five bands of fast and slow rotation relative
to the average value are distinguished. The bands of slow rotation
arise after the reversal of the polar magnetic field of the sun and
migrate toward the equator over the course of eight to 15 years along
the 'butterfly' patterns of polar faculae and of the sunspots of the
following cycle. The bands of fast rotation arise 5-6 years later,
and also migrate toward the equator parallel to the bands of slow
rotation. The fastest latitude drift of the bands was observed from
1945 to 1955 and preceded the maximum of the 19th solar activity cycle
(1955-1965). The amplitude of the azimuthal component of the coronal
rotation relative to the mean rotation varied within +/- 30 m/s. The
equatorial drift velocity varied from 3 to 5 m/s. The latitude-time
distribution of the zones with slow coronal rotation is associated
with the appearance of high-latitude and middle-latitude coronal holes
after the reversal of the solar polar magnetic field and during the
solar activity maximum of the next sunspot cycle. The origin of the
zones of anomalous rotation in the corona and their dynamics in the
global activity cycle are discussed.

---------------------------------------------------------
Title: Torsional oscillations in the solar corona
Authors: Makarov, V. I.; Tlatov, A. G.
1997ARep...41..543M Altcode:
The dependence of the differential rotation of the solar corona on
latitude and time is investigated using observations in the Fe XIV
5303 Angstrom line from 1940 to 1992. Five bands of fast and slow
rotation relative to the average value are distinguished. The bands
of slow rotation arise after the reversal of the polar magnetic field
of the Sun and migrate toward the equator over the course of 8 to
15 years along the `butterfly' patterns of polar faculae and of the
sunspots of the following cycle. The bands of fast rotation arise
5-6 years later and also migrate toward the equator parallel to the
bands of slow rotation. The fastest latitude drift of the bands was
observed from 1945 to 1955, and preceded the maximum of the 19th solar
activity cycle (1955-1965). The amplitude of the azimuthal component
of the coronal rotation relative to the mean rotation varied within
30 m/s. The equatorial drift velocity varied from 3 to 5 m/s. The
latitude-time distribution of the zones with slow coronal rotation is
associated with the appearance of high-latitude and middle-latitude
coronal holes after the reversal of the solar polar magnetic field
and during the solar activity maximum of the next sunspot cycle. The
origin of the zones of anomalous rotation in the corona and their
dynamics in the global activity cycle are discussed.

---------------------------------------------------------
Title: Torsional oscillations of the sun during 1915-1990
Authors: Makarov, V. I.; Tlatov, A. G.
1997AZh....74..474M Altcode:
The differential rotation of the large-scale magnetic field of the sun
is investigated using H-alpha synoptic charts for latitudes from +45 to
-45 deg for the period from 1915 to 1990. Walsh function expansions are
used in the analysis. The latitude dependence of the mean differential
rotational velocity is determined. Between 1915 and 1990, seven zones
of rapid rotation and seven zones of slow rotation relative to the
mean value are distinguished. These zones of anomalous rotation drift
toward the equator from a latitude of 45 deg on a timescale of 2.5 to
8 years; the drift velocity varies cyclically from 2 to 6 m/s. A zone
remains at a given latitude for between 4 and 6.5 years. The maximum
equatorial-drift velocity was observed in 1935-1955, and preceded the
solar magnetic activity maximum. More recently, from 1960 to 1990,
the drift velocity did not exceed 3 m/s. The properties of torsional
oscillations and their relation to the solar activity cycle are
investigated.

---------------------------------------------------------
Title: Torsional oscillations of the Sun from 1915 to 1990
Authors: Makarov, V. I.; Tlatov, A. G.
1997ARep...41..416M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Long-Term Variations of the Torsional Oscillations of the Sun
Authors: Makarov, Valentine I.; Tlatov, Andrey G.; Callebaut, Dirk K.
1997SoPh..170..373M Altcode:
We investigated long-term variations of the differential rotation
of the solar large-scale magnetic field on 1024 Hα charts in the
latitude zones from +45° to -45° in the period 1915-1990. We used the
expansion in terms of Walsh functions. It turns out that the rotation
of the Sun becomes more rigid than average during the cycle maximum
and the rotation is more differential during minimum. From 1915 to
1990, 7 bands of faster- and 7 bands of slower-than-average rotation
are revealed showing an 11-year period. These bands drift towards the
equator: 45° in 2.5 to 8 years. The time span of the bands varies from
4 to 6.8 years and is in anti-phase with long-term solar activity. The
latitude span of the bands of torsional oscillations varies from 0.5
R⊙ to 1.3 R⊙ and shows a long-term variation
of about 55 years. The poloidal component of velocity, Vθ
varies from 2 ms -1 to 6 ms -1. The maximum rate
of the equatorial drift occurs in the period between 1935 and 1955 and
it develops prior to the highest maximum activity. At the modern epoch
from 1965 to 1985, Vθ does not exceed 3 ms -1,
but now it has a tendency to increase. The bands of slower-than-average
rotation correspond to the evolution of the magnetic activity towards
the equator in the butterfly diagram.

---------------------------------------------------------
Title: Influence of Light Scattering and Finite Size of Shower
Particle Disk on Space-Temporal Structure of Cherenkov Radiation
Emitted in Water by High Energy Electromagnetic Cascade
Authors: Plyasheshnikov, A. V.; Lagutin, A.; Makarov, V.; Misaki, A.
1997ICRC....7..137P Altcode: 1997ICRC...25g.137P
No abstract at ADS

---------------------------------------------------------
Title: Report on observations during total solar eclipse of October
24, 1995.
Authors: Makarov, V. I.; Erchov, V. N.
1997KodOB..13..107M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: 3D Modeling of the solar corona in different stages of the
solar magnetic cycle over the period 1870 to 1991
Authors: Makarov, V. I.; Tlatov, A. G.; Fatianov, M. P.
1996R&QE...39..849M Altcode:
Three-dimensional (3D) modeling of the solar corona has been carried
out on the basis of the magnetic field distribution on H-alpha charts
for the epochs of solar eclipses that occur near the epoch of the
polar magnetic field reversal. Analysis of the 3D modeling shows
that: 1. Besides the global neutral sheet, two high-latitude
coronal neutral sheets are also observed during the epoch of the polar
magnetic field reversal. 2. The observed structure of the
coronal streamers is due to a projection of the folds of corrugated
neutral sheets on the picture plane rather than due to the peculiar
configuration of the magnetic field lines.

---------------------------------------------------------
Title: The Mars 96 Small Station - Implementation and Scientific
Objectives
Authors: Linkin, V.; Lipatov, A.; Makarov, V.; Khloustova, L.;
Ekonomov, A.; Kremnev, R.; Martinov, B.; Harri, A. -M.; Pirjola, R.;
Siili, T.; Pellinen, R.; Kumpulainen, K.; Runavot, J.; Vienne, D.;
Laplace, H.; Mouli, G.; Pommereau, J. -P.; Malique, C.; Carpentier,
T.; Rieder, R.; Economou, T.; Lognonne, Ph.; Menvielle, M.; Karczewski,
J. -F.; Herring, M.; Levachier, P.
1996DPS....28.0317L Altcode: 1996BAAS...28.1068L
The Mars-96 mission, including two Small Stations, two Penetrators and
an Orbiter, will be launched at Baikonur, Kazakhstan, on 16 November,
1996. The launcher will be Proton, a Russian launcher with an excellent
launch record. The two Small Stations will be separated from the
spacecraft 4 to 5 days before insertion to the intermediate orbit
around Mars. The Stations are expected to land in September 1997 ({(
Ls)} (approx) (178^{\circ})), nominally to Amazonis-Arcadia
region on locations (33( circ)N, 169.4(^{\circ})W) and
(37.6(circ)N, 161.9( circ \)W). The Small Station
observations combined with the data from the Orbiter instruments are
expected to shed light on the contemporary Mars and its evolution, by
providing data on the atmosphere, surface and the interior. Specific
science goals are exploration of the structure and dynamics of the
atmosphere, the role of water and other materials containing volatiles
and in situ studies of boundary layer processes. New information of
the puzzle of an intrinsic magnetic field will be gained. An extensive
effort will be taken to enhance our understanding of the interior of
Mars by recording seismic activity. To achieve the scientific goals of
the mission the Small Station will carry a following instrumentation :
camera for descent phase (DESCAM) and for panoramic views (PANCAM),
meteopackage (MET), optical sensor (ODS), soil oxidization instrument
(MOX), alpha-proton-neutron-Xray instrument (APX), seismometer and
magnetometer (Optimism).

---------------------------------------------------------
Title: Polar Faculae and Sunspot Cycles
Authors: Makarov, V. I.; Makarova, V. V.
1996SoPh..163..267M Altcode:
The monthly number of polar faculae of the Sun were determined from
white-light images at spectral band λ(eff) = (4100 ± 200) Å obtained
at the Kislovodsk Solar Station during 1960-1994. Corrected monthly
numbers were obtained with the help of the visibility function. The
level of polar activity larger than 1σ above the monthly running mean
was calculated, and the relation between the polar faculae and sunspot
cycle was studied. We confirmed earlier results (Makarov and Makarova,
1987) that the monthly number of polar faculae, NPFm(t)
correlates with the monthly sunspot area Am(Sp)(t + T)
with a time shift T ≈ 6 yr. The new polar faculae cycle began in
the middle of 1991. Peculiarities of the first part of sunspot cycle
23 are discussed.

---------------------------------------------------------
Title: On the 22-Year Oscillations, I
Authors: Vasilyev, Oleg B.; Makarov, Valentine I.
1996SoPh..163..249V Altcode:
Observational data of the solar diameter in Italy during 1876-1937 and
in Greenwich during 1851-1937 were analyzed. The Whittaker operator
with different smoothing coefficients was used. The average data sets
for the analysis of the possible oscillations of the solar diameter
during 1876-1937 were obtained. Average values of the solar radius
R(t) and absolute values of its time derivative ¦dR(t)/dt¦ were
compared with the Wolf number, W(t), and with the integral A(t) =
∫0tW(t)dt + constant. A good correlation r(R',
W) = «¦dR(t)/dt¦, W(t)» and r(R, A) = «R(t), A(t)» was found. It
was shown that the frequency spectra of R(t) and A(t) are similar. It
was found that during odd 11-yr cycles, the solar diameter decreases,
whereas during even cycles it increases. A hysteresis-like behavior
in the variation of R(t) during the 22-yr solar magnetic cycle was
demonstrated.

---------------------------------------------------------
Title: Torsional mode in the solar-corona intensity variations in
the Fe XIV 5303 A line between 1957 and 1991
Authors: Makarov, V. I.; Tlatov, A. G.
1995AZh....72..749M Altcode:
We reduced a series of the solar-corona observations in the Fe XIV 5303
A line, obtained at the Kislovodsk Station in 1957.5-1991.0. Half-year
coronal intensities were least-square-fitted with m-th power polynomials
in latitude. Latitude zones with zero second derivative of the coronal
intensity were determined. It is shown that these zones appear at
latitudes close to 80 deg after the reversal of the polar magnetic
field at maxima of the 11-year cycle and then slowly drift toward the
equator during the 22-year magnetic cycle at a mean velocity of about 2
m/s. The data obtained are compared with the solar torsional-oscillation
pattern obtained from the observed velocity field. Possible causes
for the 22-year pole-equator wave in the coronal brightness variations
are considered.

---------------------------------------------------------
Title: A torsional mode in intensity variations of the solar corona
in the Fe XIV 5303 Å line from 1957-1991
Authors: Makarov, V. I.; Tlatov, A. G.
1995ARep...39..668M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: a Study of Atmospheric Turbulence Processes Over the Terrain
with Obstacle by Using LIDAR and Transport Model
Authors: Pershin, S.; Makarov, V.; Bukharin, A.; Butusov, O.
1994BAAS...26.1553P Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Coronal loops and prominences as observed with RATAN 600
Authors: Korzhavin, A. N.; Bogod, V. M.; Borovik, V. N.; Gelfreikh,
G. B.; Makarov, V. I.
1994SSRv...70..193K Altcode:
This paper presents a short summary of observations of coronal
structures at microwaves using an instrument with high spatial
resolution and good wavelength coverage. The comparison of the RATAN-600
data with optical observations of coronal loops in the green line
and with the Very Large Array maps at 21 cm has shown that the loops
represent only a small part of coronal matter, although their role may
be of great importance in the physics of the solar corona. Prominence
(filament) associated sources, especially ”peculiar” ones, are
also reviewed.

---------------------------------------------------------
Title: Global Magnetic Activity in 22-YEAR-SOLAR-CYCLES
Authors: Makarov, Valentine I.
1994SoPh..150..359M Altcode:
Properties of even and odd 11-year solar cycles as part of the 22-year
magnetic cycle have been studied on the basis of the data on the zonal
structure of the large-scale magnetic field, of polar faculae activity
cycles, duration of 11-year cycles, high-latitude prominence areas,
inclinations of the coronal streamers, velocity of magnetic neutral line
migration, and peculiarities of the polar magnetic field reversal. It
is shown that the properties of the odd cycle depend on those of the
preceding even cycle. The 22-year magnetic cycle, consisting of an even
and odd cycle, is a unified dynamic process. The new data obtained show
that the poloidal magnetic fieldB(p) of `+' and `−' polarity for the
new 22-year magnetic cycle is formed simultaneously, possibly in deep
layers of the Sun in the form of a certain magnetic configuration,
containing alternating `+' and `−' polarities of the field.

---------------------------------------------------------
Title: Data Analysis and Expected Results of the TYCHO Mission
Authors: Wicenec, A. J.; Bastian, U.; Schweckendiek, P.; Egret, D.;
Halbwachs, J.; Hog, E.; Makarov, V.
1994ASPC...61..147W Altcode: 1994adass...3..147W
The Tycho Data Reduction Consortium (TDAC) data analysis scheme
is presented and the central parts in the reduction chain are
described. Figures are shown to verify the photometric stability of
the instrument and the rigidity of the astrometrical parameters derived
from several month of data of the nominal mission. The expected number
of output stars and the expected photometric and astrometric accuracy
is presented.

---------------------------------------------------------
Title: Coronal Large-Scale Structure in Odd and Even 11-Year Cycles
Authors: Makarov, V. I.; Mikhailutsa, V. P.; Fatianov, M. P.;
Stepanova, T. V.
1994scs..confQ..96M Altcode: 1994IAUCo.144Q..96M
No abstract at ADS

---------------------------------------------------------
Title: General Magnetic Field Reversal in the Solar Cycle 22 Period:
1986-1992
Authors: Makarov, V. I.
1994A&AT....5..333M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On 22-Year Pole To Equator Variation of the Corona Intensity
Authors: Makarov, V. I.; Tlatov, A. C.
1994scs..confR..96M Altcode: 1994IAUCo.144R..96M
No abstract at ADS

---------------------------------------------------------
Title: Obituary - Gnevyshev, M.N. - 1914-1992
Authors: Abalakin, V.; Makarov, V.; Kim, I.
1993SoPh..146....1A Altcode:
No abstract at ADS

---------------------------------------------------------
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: Variations of prominence heights in high latitude global
magnetic neutral lines.
Authors: Makarov, V. I.; Tavastsherna, K. S.; Davydova, E. I.;
Sivaraman, K. R.
1992BSolD...3...90M Altcode:
An analysis of the heights of prominences referring to the high latitude
global magnetic neutral line has been made. The analysis shows that
the mean height of the high-latitude ring of prominences decreases
by 12 per year (900 km/year) as they approach the pole with a single
reversal of the magnetic field. In the case of a 3-fold reversal the
mean heights of polar prominences do not practically change. It is
shown that the variations of height allow to judge on the inhomogeneity
in longitudinal distribution of magnetic fields. A dependence of the
variation of prominence height on the latitude of the polar filament
ring has been obtained.

---------------------------------------------------------
Title: Sign reversal of the high-latitude solar magnetic field
Authors: Benevolenskaja, E. E.; Makarov, V. I.
1992SvAL...18..108B Altcode: 1992PAZh...18..266B
It is assumed that the existence of threefold magnetic field
reversals in one of the solar hemispheres is the result of two types
of variations in the background magnetic field. The first type is the
Hale 22-yr cycle; the second is a quasi-biannual cycle. In the first
approximation, the background magnetic field evolution can be described
by a diffusion equation corrected for meridional circulation and with
a periodically changing source. Numerical modeling shows that, in the
case of multiplicity of the frequencies and under a certain relationship
between the amplitudes of these periods, zones of polarity reversals
may form during maxima of even 11-yr (Zurich numbering) cycles.

---------------------------------------------------------
Title: An estimation of parameters of dimension of the Sun's
background magnetic fields on the basis of H-alpha charts. The years
1914 - 1984.
Authors: Ajmanova, G. K.; Makarenko, N. G.; Makarov, V. I.;
Tavastsherna, K. S.
1992BSolD...3...97A Altcode:
On the basis of H-alpha synoptic charts (1914 - 1984) an index has
been used, that characterizes the predominance of the area, taken by
the background field of certain polarity in 10° latitude bands. This
index has been used for estimation of the number of independent degree
of freedom for different latitude zones of the Sun. It is found that for
the 50° - 90° latitudes the number of degrees of freedom is equal to
two and in the zone of sunspots this number is three. On the basis of
the data obtained a conclusion is made on the existence of two possibly
independent dynamic systems on the Sun: 1) a system generating the
global background magnetic field on the entire disk with two degrees of
freedom and 2) a system, responsible for generation of active regions.

---------------------------------------------------------
Title: Global solar cycle in the distribution of the green coronal
emission period: 1940 1989
Authors: Bortsov, V. V.; Makarov, V. I.; Mikhailutsa, V. P.
1992SoPh..137..395B Altcode:
We have studied the latitude-time distribution of the green (5303 Å)
coronal line emission for 1940-1989 from observations by Waldmeier
(1957), Kislovodsk, Lomnický Štít, Norikura, and Pic-du-Midi -
Q.B.S.A. (1955-1987). We have compared these data with the distributions
of the weak magnetic field (Stenflo, 1988), of polar faculae and
sunspots, and have given our interpretation of the results. We have
found that a new cycle of coronal activity commences after the polar
field reversal in the form of two components in each hemisphere. We
identify the first component with the polar faculae that appear at
latitude 40° and migrate polewards. The second component representing
sunspots shows up at 40° latitude 5-6 years after and drifts
equatorward. Thus the global coronal activity cycle has a duration
of 16-17 years and is described by two components that reflect the
activity of polar faculae and sunspots.

---------------------------------------------------------
Title: The Latitude of Filament Bands at the Sunspot Minimum and
the Activity Level in the Two Following 11-YEAR Solar-Cycles
Authors: Makarov, V. I.; Mikhailutsa, V. P.
1992SoPh..137..385M Altcode:
The zonal structure of the distribution of filaments is considered. The
mean latitudes of two filament bands are calculated in each solar
hemisphere at the minima of the sunspot cycle in the period 1924-1986:
middle latitude φ2, m and low latitude φ1, m. It
is shown that the mean latitude of the filament band φ2, m
at the minimum -m of the cycle correlates, with ϱ = 0.94, with the
maximum - M sunspot area S(M) and maximum Wolf number W(M) in the
succeeding solar cycle M. It is shown that the mean latitude of the
low-latitude filament band φ1, m is linearly dependent on
the mean latitude filament band φ2, m + 1 at the succeeding
minimum. We found a correlation of the latitude of the low-latitude
filament band φ1, m with the maximum sunspot area in the
M + 1 cycle. This enables us to predict the power of two succeeding
11-year solar cycles on the basis of the latitude of filament bands at
the minimum of activity, 1985-1986: W(22) ∼- 205 ± 10, W(23) ∼-
210 ± 10. The importance of the relationships found for theory and
applied aspects is emphasized. An attempt is made to interpret the
relationships physically.

---------------------------------------------------------
Title: Green Coronal Emission and the Global Solar Cycle
Authors: Sivaraman, K. R.; Makarov, V. I.
1992ASPC...27..415S Altcode: 1992socy.work..415S
No abstract at ADS

---------------------------------------------------------
Title: The Large-Scale Magnetic Field at the Sunspot Minimum and
the Activity Level in the Two Following Sunspot Cycles
Authors: Makarov, V. I.; Mikhallutsa, V. P.
1992ASPC...27..404M Altcode: 1992socy.work..404M
No abstract at ADS

---------------------------------------------------------
Title: The Solar High Latitude Magnetic Field Reversal
Authors: Benevolenskaya, Elena E.; Makarov, V. I.
1992ASPC...27..532B Altcode: 1992socy.work..532B
No abstract at ADS

---------------------------------------------------------
Title: Pamir-Tien Shan GPS Project: Network, Observation Campaign
92 and Analysis Strategy
Authors: Reigber, Ch.; Klotz, J.; Angermann, D.; Trapeznikov, Yu. A.;
Tatevian, S. K.; Makarov, V. I.; Abdullabekov, K. N.; Yuldashbaev,
T. S.; Tsurkov, V. G.; Kurskeev, A. K.
1992gpe..conf...42R Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Global solar cycle in the distribution of the green and red
coronal emission. Period 1940 - 1989.
Authors: Bortzov, V. V.; Makarov, V. I.; Mikhajlutsa, V. P.
1991BSolD..11...87B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Behaviour of even and odd l-modes of the solar magnetic
field with the phase of the global solar cycle on the basis of Hα
charts. Interval: 1915 - 1985.
Authors: Makarov, V. I.; Tavastsherna, K. S.; Gokhale, M. H.;
Sivaraman, K. R.
1991BSolD...6...95M Altcode:
The properties of the latitude-time distribution of the area of
predominant polarity of a large-scale magnetic field on the Sun have
been studied in 10° latitude zones on Hα charts for 1915 - 1985. The
power spectrum of the rotating symmetric harmonic, l-mode, when m =
0 has been calculated for the entire period in question and separated
for the epoch of maxima and minima of the cycle. It is shown that
alongside with the dipole component l = 1, the mode l = 3 (octapole)
is dominant at some intervals of the minimum activity. The mode l =
5 is dominant at the maximum of activity. The intensity of even modes
is 3 - 5 times smaller than that of odd modes. Two dominant periods
are detected: 22 year and 7 year; they have the maximum intensity of
the power spectrum at l = 3 and l = 5, respectively. The dependence
of the phase φ(l)/2π on l-mode is determined. The phase displacement
between the activity of the large-scale magnetic field at the latitude
larger 40° and the zone of sunspot activity is derived.

---------------------------------------------------------
Title: Biennial cycle in dynamics of large-scale magnetic fields.
Authors: Makarov, V. I.; Tavastsherna, K. S.; Petrova, N. S.
1991BSolD...3...98M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Quasi-biennial activity variations in the Sun's polar zones.
Authors: Makarov, V. I.; Makarova, V. V.; Tlatov, A. G.
1991BSolD...2...89M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Quasi-biennial variation and latitude solar magnetic field
reversal.
Authors: Benevolenskaya, E. E.; Makarov, V. I.
1991BSolD...2...89B Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Largescale Magnetic Field in the Global Solar Cycle -
Observational Aspects
Authors: Makarov, V. I.; Sivaraman, K. R.
1991LNP...380..213M Altcode: 1991IAUCo.130..213M; 1991sacs.coll..213M
The global solar cycle is considered as an interaction of 3 types of
activity: at low-latitude (sunspots), at high-latitude (polar faculae)
and the weak magnetic field. The properties of single and 3-fold
reversals of the polar magnetic field are considered. The variation
spectrum of the large-scale magnetic field of the Sun is analyzed in
the range of 1-30 nHz. A dependence between the rate of a poleward
meridional flow and phase of the global cycle is discussed.

---------------------------------------------------------
Title: Spectrum of Solar Largescale Magnetic Field Variations in
the Frequency Range 1-MHZ to 30-MHZ in the Period 1910-1985
Authors: Makarov, V. I.; Tavastsherna, K. S.; Petrova, N. S.
1991ATsir1547...27M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Dynamics of the latitude structure of the solar large-scale
magnetic field at separate longitude intervals during 1915 - 1965.
Authors: Makarov, V. I.; Kushnir, M. V.
1990BSolD..11...76M Altcode:
Dynamics of background magnetic fields has been studied on the basis
of H-alpha synoptic charts for 1915 - 1965 at separate longitude
intervals. Peculiarities of the polarity reversal of the magnetic field
latitude migration of the zonal structures in dependence on the phase
of the cycle is analyzed.

---------------------------------------------------------
Title: A topological model of the sun's threefold magnetic field
reversals.
Authors: Benevolenskaya, E. E.; Makarov, V. I.
1990BSolD...5...75B Altcode:
It is shown that single and threefold reversals of the solar magnetic
field may be a result from interaction of two types of magnetic
fields: of a low-frequency field of the order of 22 years and of a
high-frequency field of the order of 1.5 years.

---------------------------------------------------------
Title: Global Evolution of Photospheric Magnetic Fields
Authors: Makarov, V. I.; Sivaraman, K. R.
1990IAUS..138..281M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Geological Geomorphological Study of Modern Tectonic Movements
Authors: Trifonov, V. G.; Makarov, V. I.
1990UNPSA...1...41T Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The nature of rotation rates of the sector structure of the
solar magnetic field.
Authors: Makarov, V. I.; Ruzmajkin, A. A.; Starchenko, S. V.;
Tavastsherna, K. S.
1989BSolD..11..104M Altcode:
It is shown that the observed dominant rotation periods of the sector
structure of the interplanetary magnetic field are associated with
the distribution of the generating source of the magnetic field in
the convective zone. The source is due to interaction of differential
rotation and average helicity at different layers of the convective
zone.

---------------------------------------------------------
Title: New Results Concerning the Global Solar-Cycle
Authors: Makarov, V. I.; Sivaraman, K. R.
1989SoPh..123..367M Altcode:
We derive the poleward migration trajectory diagram of the filament
bands for the years 1915-1982 from the H-alpha synoptic charts. We find
that the global solar activity commences soon after the polar field
reversal in the form of two components in each hemisphere. The first
component we identify with the polar faculae that appear at latitudes
40-70° and migrate polewards. The second and the more powerful
component representing the sunspots shows up at ∼40° latitudes
5-6 years later and drifts equatorward giving rise to the butterfly
diagram. Thus the global solar activity is described by the faculae and
the sunspots that occur at different latitude belts and displaced in
time by 5-6 years. This gives rise to the prolonged duration for the
global solar activity lasting for 16-18 years as against the 11 years
which has come about based only on the spots. The two components match
with the pattern of the coronal emission in 5303 Å line. Finally, we
show that the two components of activity also match with the pattern
of excess shear associated with the torsional oscillations on the Sun
and this provides a link between the torsional oscillations and the
magnetic activity.

---------------------------------------------------------
Title: On the relationship between current and the magnetic field
in polar regions.
Authors: Makarov, V. I.; Molodenskij, M. M.
1989BSolD...6...87M Altcode:
The results of observations of prominence magnetic fields on Hanle's
effect at the Pic-du-Midi Observatory (France) given to one of the
present authors are discussed. Leroy's result that the latitudinal
component of the magnetic field Bφ in filaments is opposite
in sign to the background component is due to the conditions of the
filament stability derived previously. The reversal of the longitudinal
component of the field Bλ for new filament band during the
polar field reversal cannot be satisfactorily explained yet. Different
possible explanations of this phenomenon are discussed.

---------------------------------------------------------
Title: Evolution of latitude zonal structure of the large-scale
magnetic field in solar cycles
Authors: Makarov, V. I.; Sivaraman, K. R.
1989SoPh..119...35M Altcode:
Properties of a latitude zonal component of the large-scale
solar magnetic field are analyzed on the basis of Hα charts for
1905-1982. Poleward migration of prominences is used to determine
the time of reversal of the polar magnetic field for 1870-1905. It is
shown that in each hemisphere the polar, middle latitude and equatorial
zones of the predominant polarity of large-scale magnetic field can be
detected by calculating the average latitude of prominence samples
referred to one boundary of the large-scale magnetic field. The
cases of a single and three-fold polar magnetic field reversal are
investigated. It is shown that prominence samples referred to one
boundary of the large-scale magnetic field do not have any regular
equatorward drift. They manifest a poleward migration with a variable
velocity up to 30 m s-1 depending on the phase of the
cycle. The direction of migration is the same for both low-latitude
and high-latitude zones. Two different time intervals of poleward
migration are found. One lasts from the beginning of the cycle to
the time of polar magnetic field reversal and the other lasts from
the time of reversal to the time of minimum activity. The velocity of
poleward migration of prominences during the first period is from 5 m
s-1 to 30 m s-1 and the second period is devoid
of regular latitude drift.

---------------------------------------------------------
Title: Do polar faculae on the sun predict a sunspot cycle?
Authors: Makarov, V. I.; Makarova, V. V.; Sivaraman, K. R.
1989SoPh..119...45M Altcode:
The paper reports the results of the analysis of the data on polar
faculae for three solar cycles (1960-1986) at the Kislovodsk Station of
the Pulkovo Observatory and on polar bright points in Ca II K line for
two solar cycles (1940-1957) at the Kodaikanal Station of the Indian
Institute of Astrophysics. We have noticed that the monthly numbers
of polar faculae and polar bright points in Ca II K line and monthly
sunspot areas in each hemisphere of the following solar cycle have a
correlation with each other. A new cycle of polar faculae and polar
bright points in the Ca II K line begins after the polar magnetic field
reversal. We find that the smaller the period between the ending of
the polar field reversal and the beginning of a new sunspot cycle is,
the more intense is the cycle itself. The intensity of the forthcoming
solar cycle (cycle 22) and the periods of strong fluctuations in
activity expected in this cycle are also discussed.

---------------------------------------------------------
Title: The Spacetime Polarity Distribution of the Largescale Solar
Magnetic Field
Authors: Obridko, V. N.; Makarov, V. I.; Tavastsherna, K. S.; Gaziev,
G. A.
1989ATsir1536...31O Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Pulkovo Observatory and Service of the Sun in the USSR.
Authors: Gnevyshev, M. N.; Makarov, V. I.
1989pulk.conf..182G Altcode:
No abstract at ADS

---------------------------------------------------------
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: On the Hale law for large-scale magnetic fields during 1925
- 1982.
Authors: Makarov, V. I.; Tavastsherna, K. S.; Vasil'Eva, V. V.
1988BSolD1987...59M Altcode:
H-alpha charts for 1925 - 1982 were processed with the aim of detection
of the polarity reversal in activity cycles of the large-scale magnetic
field of the Sun in 10° latitude intervals. It is found that the main
period of the polarity inversion of the large-scale magnetic field at
the latitudes from 30° to 90° in both the hemispheres is 280 solar
rotations or 20.7 years. The above mentioned period is either absent
or very faintly pronounced at the latitudes from 0° to 30° in the
sunspot zone.

---------------------------------------------------------
Title: Some peculiarities of a latitudinal migration of filaments
in solar cycles 18 and 19 (1944 - 1965).
Authors: Bortsov, V. V.; Makarov, V. I.
1988BSolD1987...78B Altcode:
Filament coordinates were determined from Meudon synoptic H-alpha
charts. The behaviour of the latitudinal migration of filaments
in dependence on their lifetime is studied. It is shown that the
filaments manifest a poleward migration at a velocity from 3 to 15 m
s-1 at all latitudes. The direction of the migration is the
same for the low-latitude zones |φ| ≤ 30° and high-latitude zones
|φ| &gt; 30°. The velocity of the migration is greater in the zone
|φ| &gt; 30° than that in the sunspot zone.

---------------------------------------------------------
Title: On the rotation of the sector structure of the interplanetary
magnetic field during 1926 - 1986.
Authors: Tavastsherna, K. S.; Makarov, V. I.; Petrova, N. S.
1988BSolD1988...84T Altcode:
The data of a spectral analysis of the interplanetary magnetic field
for the years 1926 - 1986 are given. Three dominating periods of the
quasi-rigid rotation of the two- and four-sector structures are found:
28.2, 27.2, 26.4 days, varying from cycle to cycle. It is shown that
the two-sector structure is practically observed at all phases of the
considered cycles. In the sunspot minimum it is associated with the
maximum Wolf number in the succeeding cycle.

---------------------------------------------------------
Title: Variation of Coronal Brightness in the 5303A Line during
the Activity Cycle and Latitudinal Zonal Structure of the Coronal
Magnetic Field - Period of 1944-1974
Authors: Makarov, V. I.; Leroy, J. L.; Noens, J. C.
1987SvA....31..560M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The variation of the coronal intensity in the 5303 A line
in the activity cycle and the latitudinal zonal structure of the
coronal magnetic field - The period 1944-1974
Authors: Makarov, V. I.; Leroy, J. L.; Noens, J. C.
1987AZh....64.1072M Altcode:
A comparison of variations of intensity of the corona using the 5303
Å line (Pic du Midi observations) with the latitude zonal structure of
the coronal magnetic field for 1944 - 1974 is made using Hα charts. It
is shown that the global process of solar activity originally is to be
seen in the polar zone after the polarity reversal and lasts for about
11 years up to the next reversal of the magnetic field of the Sun. A
second and more intense manifestation of this process takes place at
+30° to -30° in latitude and also lasts for about 11 years. This
means that the total duration of the global solar activity cycle at
all latitudes attains 17 - 18 years.

---------------------------------------------------------
Title: Magnetic waves of solar activity.
Authors: Makarov, V. I.; Ruzmaikin, A. A.; Ruzmajkin, A. A.;
Starchenko, S. V.
1987SoPh..111..267M Altcode:
An asymptotic solution of generation equations for the solar mean
magnetic field is given and studied. The variation of rotational angular
velocity with depth is taken from helioseismological data. Average
helicity is prescribed according to the mixing length theory. It is
shown that three dynamo waves of the magnetic field are excited. The
first wave is generated at the surface layer and concentrates at
latitudes of about 60°. Its activity becomes apparent in the poleward
migration of the zone of polar faculae formation. The second more
powerful wave of the field is excited in the center of the convection
zone and its activity shows up in a sunspot cycle. The third wave
which is similar to the first wave, is generated at the bottom of the
convection zone and attenuates towards the surface. Its activity may
appear as a three-fold reversal of the polar magnetic field.

---------------------------------------------------------
Title: On the relationship between polar faculae, X-ray bright points
and ephemeral active regions on the sun.
Authors: Makarov, V. I.; Makarova, V. V.
1987BSolD1987Q..62M Altcode:
A study was made on the basis of an analysis of photoheliograms of
the Kislovodsk Station of the Pulkovo Observatory (during the minima
of solar activity in 1964, 1976, 1985). Under the assumption of a
homogeneous longitudinal distribution it is found that about 900 polar
faculae are observed simultaneously over the entire solar disc. Through
a 14 day analysis of solar X-ray observations it has been discovered
that polar faculae coincide in coordinates with X-ray bright points
(XBP) in 66% of the cases. On certain days the coincidence attains
85%. A conclusion is made that polar faculae, EAR and XBP seem to be a
particular type of solar activity, differing from sunspot activity. This
difference is discussed and the importance of polar faculae studies
in understanding the global process of solar activity is stressed.

---------------------------------------------------------
Title: Magnetic neutral lines of the large-scale magnetic field and
solar activity.
Authors: Makarov, V. I.; Tavastsherna, K. S.; Sivaraman, K. R.
1987SvA....30..317M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: "Butterfly" diagram for polar faculae and sunspots during
1940 - 1985.
Authors: Makarov, V. I.; Makarova, V. V.; Sivaraman, K. R.
1987BSolD1987R..62M Altcode:
Data on the time-latitude distribution of polar faculae and sunspots
for 1940 - 1985 are given. They characterize two waves of the toroidal
component of the magnetic field of the global process of solar activity.

---------------------------------------------------------
Title: Activity waves of the solar magnetic field.
Authors: Makarov, V. I.; Ruzmajkin, A. A.; Starchenko, S. V.
1987BSolD1987Q..82M Altcode:
An asymptotic solution of generation equations for the solar magnetic
field is given. A variation in the angular velocity of rotation with
depth is assumed on the basis of helioseismic data. Mean helicity
is calculated on the basis of mixing length theory. It is shown that
three dynamo-waves of the magnetic field are excited.

---------------------------------------------------------
Title: Note on the forecast of strong fluctuations of solar activity
in solar cycle 22.
Authors: Makarov, V. I.; Makarova, V. V.
1987BSolD1987...73M Altcode:
The results of a reduction of polar faculae are given for the last three
cycles of solar activity (1960 - 1987) on the basis of observations
at the Kislovodsk Station of the Pulkovo Observatory. The results
of a comparison of monthly numbers of polar faculae with monthly
sunspot areas of the succeeding cycle for each hemisphere are given. A
significant correlation has been derived between strong fluctuations
of polar faculae and strong fluctuations of sunspot areas in the
succeeding cycle. A possibility of forecasting strong fluctuations of
sunspot activity in solar cycle 22 is discussed on the basis of polar
faculae observations during 1982 - 1987.

---------------------------------------------------------
Title: On the two types of neutral lines of the large-scale solar
magnetic field.
Authors: Makarov, V. I.; Mikhajlutsa, V. P.
1987BSolD1986...81M Altcode:
Two types of solar magnetic neutral lines have been defined on the
criterion of topology of the field above them. The lines above which
closed systems of the line-of-force loops are observed that transform
into helmet-like formations in the corona are referred to the first
type. The neutral lines with deeply open field structures identified
with cavities in the filaments and filament channels in the chromosphere
are referred to the second type. The even number of the neutral line in
the given latitudinal interval beginning with the pole, which separates
latitude zonal structures of the magnetic field and the presence of
a symmetrically scattered flocculus relative to the neutral line are
necessary and sufficient conditions for the existence of a cavity in
the chromosphere. The first type of neutral lines always bears an odd
number, the second type an even number.

---------------------------------------------------------
Title: On the epochs of polarity reversals of the polar magnetic
field of the sun during 1870-1982
Authors: Makarov, V. I.; Sivaraman, K. R.
1986BASI...14..163M Altcode:
The H-alpha synoptic charts for the 1904-1982 period and data on the
polar prominences for the 1870-1905 period are used to investigate
the polarity reversal of the polar magnetic field on the sun for 11
solar cycles. Good agreement is found between polarity reversals
obtained from the drift trajectory of the neutral line and those
from magnetograph observations. A three-fold polarity reversal of the
sun's magnetic field was found in the 12th and 14th solar cycles in
the southern hemisphere, and in the 16th, 19th and 20th solar cycles
in the northern hemisphere. It is noted that the filament bands in
the two hemispheres do not reach the respective poles simultaneously.

---------------------------------------------------------
Title: Lineaments of eastern Cuba - Geological interpretation of
aerial and space imagery
Authors: Makarov, V. I.; Trifonov, V. G.; Volchkova, G. I.; Formel,
F.; Brezhnianskii, K.
1986IssZK...4...75M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Magnetic Neutral Lines of the Largescale Magnetic Field and
Solar Activity
Authors: Makarov, V. I.; Tavastsherna, K. S.; Sivaraman, K. R.
1986SvA....30..317M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the latitude migration of polar faculae in the solar
activity cycle - Period: 1970-1978
Authors: Makarov, V. I.; Makarova, V. V.
1986JApA....7..113M Altcode:
Coordinates of polar faculae have been measured and processed
using daily photoheliograms of the Kislovodsk Station of the
Pulkovo Observatory with the final goal of studying their latitude
distribution during the solar cycles 20-21. The first polar faculae
emerge immediately after the polarity inversion of the solar magnetic
field at the latitudes from 40 deg to 70 deg with the average phi
approximately equal to 55 deg. The zone of the emergence of polar
faculae migrates poleward during the period between the neighboring
polarity inversions of the solar magnetic field. This migration is about
20 deg for 8 years, which corresponds to a velocity of 0.5 m/s. The
maximum number of polar faculae was reached at the activity minimum
(1975-1976). The last polar faculae were observed in the second half
of 1978 at the latitudes from 70 deg to 80 deg.

---------------------------------------------------------
Title: Magnetic neutral lines of the large-scale magnetic field and
solar activity
Authors: Makarov, V. I.; Tavastsherna, K. S.; Sivaraman, K. R.
1986AZh....63..534M Altcode:
On the basis of Hα synoptic charts for the period 1955 - 1981 two
components in the distribution of the scales of structures of the
large-scale magnetic field are found. It is shown that the general
magnetic field of the sun has a latitudinal zonal structure which
is formed from the elements of the 1st and 2nd distributions. The
boundaries of latitude zones of the magnetic field either oscillate
near average latitudes or have only poleward migration. Three types of
quasi-periodic oscillations are noted, their periods being different
in the S and N hemispheres. The most probable period of oscillations
is found in the southern hemisphere and it equals to about 20 solar
rotations.

---------------------------------------------------------
Title: On the latitudinal migration of polar faculae in their activity
cycle. II. Period: 1940 - 1968.
Authors: Makarov, V. I.; Sivaraman, K. R.
1986BSolD1986...64M Altcode:
Coordinates and the number of polar faculae are determined
at latitudinal higher 40° on K232-Ca+
spectroheliograms of the Kodaikanal Observatory for 2097 days for
the period 1940 - 1968. First polar faculae appear immediately after
the polarity reversal of the magnetic field as bright pairs of dots
against the chromospheric network. The polar faculae cycle is asymmetric
relative to the sunspot cycle, and the maximum of their number does not
always coincide with the sunspot minimum. The duration of the cycle of
polar faculae is equal to the interval between the neighbouring polarity
reversal of the magnetic field and lasts from 7 to 11 years. The zone
of the emergence of polar faculae migrates polewards with the mean
velocity 0.5 m/sec.

---------------------------------------------------------
Title: Latitude Structure of the Largescale Magnetic Solar Field in
Separate Longitudinal Intervals - Part One - SOLAR-CYCLE-20
Authors: Makarov, V. I.; Kushnir, M. V.
1986BSolD...4...63M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Solar observatories of France.
Authors: Gnevyshev, M. N.; Makarov, V. I.
1986ZemVs...2...48G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Latitude structure of the large-scale solar magnetic field
in separate longitudinal intervals. I Solar cycle No. 20.
Authors: Makarov, V. I.; Kushnir, M. V.
1986BSolD1986R..63M Altcode:
An analysis of the distribution of background magnetic fields in the
20th solar cycle using H&amp;alpha; charts is made. The
peculiarities of the time-latitude distribution of the field at all
the latitudes are determined predominantly by the poleward migration
of magnetic fields of active regions. On the latitude versus time
diagram only few cases are observed of equatorial fluxes of the field
at some longitudes. They are due to the latitude-longitude structure
of separate unipolar regions on H&amp;alpha; charts.

---------------------------------------------------------
Title: Atlas of H-alpha synoptic charts for solar cycle 19 (1955 -
1964). Carrington solar rotations 1355 to 1486.
Authors: Makarov, V. I.; Sivaraman, K. R.
1986KodOB...7.....M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Longitudinal Distribution of Neutral Magnetic Lines - Part Two
Authors: Makarov, V. I.; Tavastsherna, K. S.
1986BSolD...1...63M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Connection between brightness variations in a spot umbra and
wave processes in the penumbra.
Authors: Loskutnikov, V. S.; Makarov, V. I.
1986mris.conf...87L Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the Latitudinal Migration of Polar Faculae in Their Activity
Cycle - Part Two - 1940-1968
Authors: Makarov, V. I.; Sivaraman, K. R.
1986BSolD...9...64M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the Forecast of SOLAR-CYCLE-22
Authors: Makarov, V. I.
1986BSolD...8...57M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the forecast of solar cycle 22.
Authors: Makarov, V. I.
1986BSolD1986...57M Altcode:
Data are given on the epoch of reversal of the polar magnetic field of
the Sun for the period 1870 - 1982. A dependence between the interval
from the reversal of the polar magnetic field to the beginning of a new
cycle and its intensity is found. The annual Wolf number in the maximum
of solar cycle 22 may attain ≅ 85+10, and total half annual sunspot
area 31×104millionth of the solar visible hemisphere. The
obtained result is discussed in terms of two waves of the magnetic
field toroidal component in the global process of solar activity.

---------------------------------------------------------
Title: Longitudinal distribution of magnetic neutral lines. I.
Authors: Makarov, V. I.; Tavastsherna, K. S.
1986BSolD1985...51M Altcode:
Half-annual values of the number of neutral lines of the solar
large-scale magnetic field (1945 - 1974), calculated on the basis of
Hα charts, are given.

---------------------------------------------------------
Title: Longitudinal distribution of neutral magnetic lines. II.
Authors: Makarov, V. I.; Tavastsherna, K. S.
1986BSolD1986Q..63M Altcode:
On the basis of the longitudinal distribution of neutral magnetic
lines of the large-scale magnetic solar field for the period 1945 -
1974 three types of their activity are detected: isolated islands
of a unipolar field, a family of neutral magnetic lines, complexes
of neutral magnetic lines. No significant deviation from the random
distribution of neutral lines has been found.

---------------------------------------------------------
Title: The Latitudinal Migration of Polar Faculae during Their
Activity Cycle - 1970-1978
Authors: Makarov, V. I.; Makarova, V. V.
1985BSolD...9...71M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On quasi-periodic oscillations of the boundaries of latitudinal
zonesof the solar magnetic field.
Authors: Makarov, V. I.; Petrova, N. S.; Tavastsherna, K. S.
1985BSolD1985...69M Altcode:
It is shown that the variation in the latitude of the boundaries
of the magnetic field zones during 1945 - 1981 consists of poleward
migration and quasi-periodic oscillations. In the southern hemisphere
where a unifold polarity inversion was observed at that time at
all the boundaries oscillations with the period of about 18 solar
rotations (4×107sec), horizontal velocity of about 5
m/sec and amplitude of oscillations of about 5×109cm were
detected. For sunspot total areas periods of about 10 solar rotations
vaguely showed up in the same period.

---------------------------------------------------------
Title: The Behaviour of Prominence Areas in the 11-YEAR Cycle and
Their Relationship with Other Solar Events
Authors: Gnevyshev, M. N.; Makarov, V. I.
1985SoPh...95..189G Altcode:
On the basis of the data on prominence areas for 1880-1976 and positions
of the boundary background magnetic field for 1955-1982 it is shown that
the maximum development of prominences and their poleward migration,
accompanied by the magnetic field reversal, concides with the first
maximum of the 11-year solar cycle, which is characterized by an
enhancement of solar activity at all latitudes. The second maximum
is an increase of all features, including prominences but in the low
latitudes only. That prominence zone migrates poleward in the following
11-year solar cycle.

---------------------------------------------------------
Title: On the structure of polar faculae.
Authors: Makarov, V. I.; Makarova, V. V.
1985BSolD1984...88M Altcode:
Coordinates of polar faculae and charts of their spatial distribution
are given using photoheliograms for 1970 - 1978. Four types of polar
faculae are defined according to their expansion and compactness. On the
basis of identification of polar faculae with magnetic field knots it
is shown that polar faculae are classified into unipolar and bipolar
faculae using magnetic characteristics as a criterion. The polarity
of the magnetic field of bipolar faculae, originated after the general
magnetic field reversal, is opposite to that of sunspots at that period
and coincides with the polarity of the magnetic field of sunspots in
the following cycle.

---------------------------------------------------------
Title: Latitude zonal structures of the large-scale magnetic field
of the sun during 1880 - 1935.
Authors: Makarov, V. I.
1985BSolD1984...68M Altcode:
On the basis of the reduction of the latitude distribution of prominence
areas for 1880 - 1935 the existence of latitude zonal structures of
the radial component of the solar magnetic field, obtained earlier
from Hα charts for 1955 - 1982, is confirmed.

---------------------------------------------------------
Title: A Longitudinal Distribution of Magnetic Neutral Lines -
Part One
Authors: Makarov, V. I.; Tavastcherna, K. S.
1985BSolD..12...51M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Latitudinal migration of polar faculae during their activity
cycle. Period 1970 - 1978.
Authors: Makarov, V. I.; Makarova, V. V.
1985BSolD1985...71M Altcode:
Heliographic co-ordinates of polar faculae were measured on daily
photoheliograms taken at the Kislovodsk Mountain Station of the
Central Astronomical Observatory of the USSR Academy of Sciences for
the 20th and 21st cycles. The latitudinal distribution of polar faculae
was studied.

---------------------------------------------------------
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 study of the solar magnetic field using Hα-charts for 1945
- 1982.
Authors: Makarov, V. I.
1985AbaOB..60..193M Altcode:
The properties of the latitudinal zonal structure of the solar magnetic
field for 1945 - 1982 are studied on the basis of Hα-charts. In
each solar hemisphere 3 zones of the magnetic field can be detected:
equatorial, mean latitudinal and polar zones with the mean boundaries
at 0°, ±20°, ±40° after the sign reversal and in the minimum of
activity. The poleward migration of latitudinal zones of magnetic fields
lasting 13, 22 and 35 years, depending on the characteristics of the
cycle, is observed. This determined the epoch and peculiarities of the
magnetic polar field reversal. In potential approximation spherical
harmonics are given, characterizing the evolution of the latitudinal
zonal structure of the solar magnetic field.

---------------------------------------------------------
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: Correlation between tectonic events in the most recent period
of earth evolution
Authors: Kukina, N. V.; Makarov, V. I.; Trifonov, V. G.; Volchkova,
G. I.
1985MINGI.399.....K Altcode:
Methods used in correlating various neotectonic events are described,
together with a general discussion of short-lived changes in tectonic
activity. Neotectonic events in the Carpathian-Caucasus-Kopetdag segment
and in ancient folded areas (including Tien Shan and segments of Rhodope
mountains) of the Alpine-Asian orogenic belt are analyzed. Correlation
of neotectonic events of the earth's mobile belts revealed the
presence in the earth crust of segments which are characterized by the
synchronism of the most important events in tectonic activity. Common
activating phases disclosed in these areas indicate the presence
of global rhythmicity in tectogenesis. In addition, the studies
have uncovered some specificities in the neotectonic stage of the
Mesozoic-Cenozoic period of the earth evolution.

---------------------------------------------------------
Title: Do prominences migrate equatorwards?
Authors: Makarov, V. I.
1984SoPh...93..393M Altcode:
The mean latitude of prominence samples referring to one boundary
of the polarity division line of the large-scale magnetic field is
calculated on the basis of Hα charts in the period 1955-1982. It
is shown that the magnetic field in that period had a latitude zonal
structure. The boundaries of the latitude zones of the magnetic field
had no regular equatorwards migration. They either oscillated near
the mean boundaries at 0°, ±20°, ±40°, or migrated polewards.

---------------------------------------------------------
Title: Latitude Zonal Structures of the Largescale Magnetic Solar
Field during 1880-1953
Authors: Makarov, V. I.
1984BSolD..10...68M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the method of the Mountain Kislovodsk Station of the
Pulkovo Observatory for the construction of "Synoptic Charts of
Active Solar Features".
Authors: Makarov, V. I.
1984BSolD1984...59M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Latitude zones of background magnetic fields in solar cycles
No. 20 and No. 21.
Authors: Makarov, V. I.; Fat'yanov, M. P.
1984BSolD1984...84M Altcode:
Mean latitudes of background magnetic fields (1965 - 1982) have been
analysed and calculated on the basis of Hα maps. Background magnetic
fields appear to have a latitude zonal structure. The boundaries
of these zones either migrate poleward or change their location in
relation to some mean latitude. Equatorward migration of background
magnetic field zones has not been detected. Latitude zones of background
magnetic fields display a 22-year cycle. It is shown that the boundary
of the interplanetary magnetic field sectors can be multiconnected.

---------------------------------------------------------
Title: Latitudinal zonal structure of the solar coronal magnetic
field.
Authors: Makarov, V. I.
1984BSolD1984...52M Altcode:
Properties of the latitudinal zonal structure of the solar magnetic
field are studied on the basis of Hα charts for the period 1955 -
1981. It is shown that after the sign inversion of the magnetic field in
the minimum of solar activity in each solar hemisphere 3 zones of the
field exist: the equatorial, mean-latitudinal and polar zones with the
boundaries at ±20° and ±40°. Equatorial and mean-latitudinal zones
can be considered as f and p fields of active regions. The lifetime
of the zones depends on the character of the sign inversion and is
about 13.22 and 35 years. A phenomenological model of the solar cycle
is discussed.

---------------------------------------------------------
Title: Latitudinal Zonal Structure of the Solar Coronal Magnetic Field
Authors: Makarov, V. I.
1984BSolD...9...52M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Latitude Zones of Background Magnetic Fields in SOLAR-CYCLE-20
and SOLAR-CYCLE-21
Authors: Makarov, V. I.; Fatianov, M. P.
1984BSolD...4...84M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the Structure of Polar Faculae
Authors: Makarov, V. I.; Makarova, V. V.
1984BSolD..12...88M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Structure of the large-scale magnetic field of the sun from
July 28 to August 3, 1983.
Authors: Kushnir, M. V.; Makarov, V. I.; Fat'yanov, M. P.
1984BSolD1984...58K Altcode:
The large-scale solar magnetic field is analysed on the basis of daily
Hα charts.

---------------------------------------------------------
Title: The Structure of the Largescale Magnetic Field of the Sun
from 1983JUL28 to 1983AUG3
Authors: Kushnir, M. V.; Makarov, V. I.; Fatianov, M. P.
1984BSolD...8...58K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Poleward Migration of the Magnetic Neutral Line and the
Reversal of the Polar Fields on the Sun - Part One - Period 1945-1981
Authors: Makarov, V. I.; Fatianov, M. P.; Sivaraman, K. R.
1983SoPh...85..215M Altcode:
Poleward migration of the magnetic neutral line on the Sun has been
calculated for the periods 1945-1950 and 1955-1981 using synoptic
charts based on Hα observations. Epochs of sign reversal of the solar
magnetic field at latitudes 50° to 90° have been determined for
these periods. During the cycles 19 and 20 a threefold sign reversal
took place in the northern hemisphere. During all the above cycles
both the solar poles were of one polarity for a period ranging from
0.5 to 1 year. The poleward drift velocity of the magnetic neutral
line varies from 6 to 29 m s−1 and seems to depend on
the strength of the cycle.

---------------------------------------------------------
Title: Poleward Migration of the Magnetic Neutral Line and the
Reversal of the Polar Fields on the Sun - Part Two - Period 1904-1940
Authors: Makarov, V. I.; Sivaraman, K. R.
1983SoPh...85..227M Altcode:
Poleward migration of the magnetic neutral line on the Sun has been
computed for the period 1904-1940 using synoptic charts based on Hα
observations and the epochs of sign reversal of the solar magnetic
field at latitudes 50° to 90° have been determined for this
period. During the cycles 16 and 14, a threefold sign reversal took
place in the northern and southern hemispheres, respectively. During
all the cycles studied both the solar poles were of one polarity for
a period ranging from 0.6 to 1.6 years. The poleward drift velocity
of the neutral line varies from 4.2 to 8.2 m s−1. The
apparent relation between the velocity of the filament bands when
three bands are present with the bursts of solar activity is discussed.

---------------------------------------------------------
Title: On the Scale of Structures of the Largescale Background
Magnetic Field in the 20TH Solar Cycle
Authors: Makarov, V. I.; Tavastsherna, K. S.
1983BSolD...5...93M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Latitude Zones of Background Magnetic Fields in the 19TH
Solar Cycle
Authors: Makarov, V. I.
1983BSolD..10...93M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Polar Migration of the Magnetic Neutral Line and Sign Inversion
of the Solar Magnetic Field during 1890-1895
Authors: Makarov, V. I.
1983BSolD...1...86M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the variation of prominence heights in the solar cycles
from 1912 to 1974.
Authors: Makarov, V. I.
1983BSolD1983..100M Altcode:
An analysis of heights of prominences has been made using the Kodaikanal
Observatory data for the period 1912 - 1974. In each cycle their
heights increased by ≈12arcsec from minimum to maximum. Near the
minima of activity the prominence height linearly decreased with time
from 29arcsec in 1912 to 38arcsec in 1973.

---------------------------------------------------------
Title: A comparison of the distribution of background field polarity
on Hα-synoptic charts with magnetographic observations of magnetic
fields.
Authors: Makarov, V. I.; Stoyanova, M. N.
1983BSolD1982...94M Altcode:
It is shown that the distribution of the background magnetic field
polarity of the sun (at the latitude zone ± 40°) on the Hα synoptic
charts of the Kislovodsk Station coincide with that of the magnetic
field polarity observed at the Mt. Wilson Observatory by 89%. For the
entire solar surface the coincidence of the charts reaches 95%.

---------------------------------------------------------
Title: The Speed of the Polar Migration of the Magnetic Neutral Line
and the Intensity of the 11-YEAR Cycle
Authors: Makarov, V. I.
1983BSolD...2..105M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Speed of polar migration of the magnetic neutral line and
intensity of the 11-year cycle.
Authors: Makarov, V. I.
1983BSolD1983..105M Altcode:
The speed of the polar migration of the magnetic neutral line is in
best correlation with the intensity of the preceding 11-year solar
cycle for 9 solar cycles (1890-1981).

---------------------------------------------------------
Title: Latitude zones of background magnetic fields in the 19th
solar cycle.
Authors: Makarov, V. I.
1983BSolD1983R..93M Altcode:
Mean latitudes of background magnetic fields (1955 - 1962) have been
calculated and analysed from H&amp;alpha; synoptic maps. The
equatorward migration of mean boundaries of background magnetic fields
was not observed in either hemisphere. From 1955 to 1962 six zones of
background magnetic fields of opposite polarities were observed. In
1955 - 1962 four zones of background magnetic fields were observed in
the southern hemisphere.

---------------------------------------------------------
Title: Polar migration of prominences and the inversion of the
polar magnetic field of the sun in the 11th and 12th solar cycles
(1869 - 1885).
Authors: Makarov, V. I.
1983BSolD1983...87M Altcode:
The trajectories of the polar migration of prominences are calculated
on the basis of spectroscopic observations of prominences during 1869 -
1885. The epoch of the polarity inversion of the polar magnetic field
is determined. Three "waves" of migration of polar prominences were
observed in the southern hemisphere in the 12th solar cycle whose
velocities were 3.9, 7.0 and 8.3 m sec-1. In the northern
hemisphere only one "wave" of migration was observed whose velocity
was 4.0 m sec-1. The 12th solar cycle is similar to the 14th
solar cycle from the point of view of polar migration of prominences.

---------------------------------------------------------
Title: Structure and polar migration of background magnetic fields.
Authors: Makarov, V. I.; Tavastsherna, K. S.
1983BSolD1983R..84M Altcode:
Hα maps of the 20th and 21th solar cycles (1963 - 1981) were analysed
in order to detect the time sequence of quasi-circular structures
of filaments and filament channels within the limits 3° to 15° in
size. These structures are shown to be connected with the emergence
of a new magnetic flux of opposite polarity to that of the background
magnetic field.

---------------------------------------------------------
Title: Polar migration of the magnetic neutral line and sign inversion
of the solar magnetic field during 1890-1895.
Authors: Makarov, V. I.
1983BSolD1983Q..86M Altcode:
An analysis of the magnetic neutral line migration is made on the
basis of Hα charts of prominence distributions. The epoch of the sign
inversion of the magnetic field at the latitudes from 60° to 90° is
calculated. In both hemispheres the sign changed only once. The rate
of the polar migration of the neutral line was 3.8 m/sec. The 13th
solar cycle is similar to the 15th and 17th solar cycles according to
the peculiarities of the neutral line migration.

---------------------------------------------------------
Title: The Structure and Polar Migration of Background Magnetic Fields
Authors: Makarov, V. I.; Tavastsherna, K. S.
1983BSolD...6...84M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the scales of structures of the large-scale background
magnetic field in the 20th solar cycle.
Authors: Makarov, V. I.; Tavastsherna, K. S.
1983BSolD1983Q..93M Altcode:
On the basis of Hα maps two scale distributions of longitudinal
structures of the large-scale magnetic field are found at 10 - 40°
in both solar hemispheres. One of them is a gaussian distribution for
the dimensions from 3 to 15°. These are "islands" of the predominant
polarity of the magnetic field. They are outlined by filaments and
filament channels and are connected with the appearance of a new
magnetic flux. The other is a Pearson curve of type I for 15° to 60°
with maximum at 25°. At the equator and latitudes φ &gt; 40° there
are no predominant dimensions.

---------------------------------------------------------
Title: Polar Migration of Prominences and the Reversal of the Polar
Magnetic Field Polarity in the 11TH and 12TH Solar Cycles 1869-1885
Authors: Makarov, V. I.
1983BSolD...7...87M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the Variation of the Prominence Altitudes in the Solar
Cycles during 1912-1974
Authors: Makarov, V. I.
1983BSolD...4..100M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Morphology of H-alpha filaments and filament channel systems
Authors: Makarov, V. I.; Stoianova, M. N.; Sivaraman, K. R.
1982JApA....3..379M Altcode:
The results of a study of the morphology of the large-scale filament
structures of the sun and their relations with the distribution of
the large-scale magnetic field on the solar surface are reported. A
continuous filament which forms a closed circular contour has been
seen on spectroheliograms, particularly during the maximum phase of
the solar cycle. Their mean size seldom exceeds 10 degrees, while
their lifetimes occasionally span several days. In the core of the
H-alpha line, single filaments are seen connected with one another
by a regular structure of dark chromospheric elements several tens
of degrees in extent or at times by a conglomeration of absorption
grains one to three degrees in length. Occasionally, prominences can be
detected above filament channels. Some arches of the filament channel
may elongate with an associated local increase in coronal intensity.

---------------------------------------------------------
Title: On the Dynamics of the Chromosphere above Sunspots
Authors: Zhugzhda, Iu. D.; Makarov, V. I.
1982SoPh...81..245Z Altcode:
The brightness oscillations of a sunspot umbra in the Hα and
Ca+ K lines are studied. The observational results
are explained in terms of the resonance theory of slow-mode
magnetohydrodynamic waves in the sunspot chromosphere. The thickness
of the chromosphere above a sunspot varies quasi-periodically from
420 km to 1000 km.

---------------------------------------------------------
Title: The recent 21st-cycle sign reversal in the polar magnetic
field on the sun
Authors: Makarov, V. I.; Fatyuanov, M. P.
1982PAZh....8..631M Altcode:
The poleward motion of filament belts on the sun was analyzed in order
to provide an estimation of when the polar magnetic field of the sun
would reverse sign during the 21st solar cycle. It was determined that
during the 21st solar cycle the polar magnetic field became negative
at the north pole in December 1980 and positive at the south pole in
September 1981. It is suggested that the underlying polar magnetic
field on the sun may be concentrated within a thin photospheric surface
layer. The polarity-reversal process was found to be accompanied by
the development of arch prominences near the poles.

---------------------------------------------------------
Title: The Recent 21ST-CYCLE Sign Reversal in the Polar Magnetic
Field on the Sun
Authors: Makarov, V. I.; Fatyanov, M. P.
1982SvAL....8..340M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Irregularities of the Limb of the Solar Disk in White Light
Authors: Dubov, E. E.; Makarov, V. I.
1982SvA....26..113D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Irregularities of the limb of the solar disk in white light
Authors: Dubov, E. E.; Makarov, V. I.
1982AZh....59..186D Altcode:
At the very limb of the solar disk the continuous spectrum is broken
up into separate strips, which we consider as a manifestation of the
irregularity ('hilliness') of the limb of the solar disk. The distance
between the strips correspond to the sizes of supergranules. The height
of the 'hills' is on the order of 400 km.

---------------------------------------------------------
Title: The Dynamics of Filament Bands and Hale's and Sperer's Laws
Authors: Makarov, V. I.
1982BSolD...4...89M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the relation between the dynamics of filament bands and
Hale's and Spoerer's laws.
Authors: Makarov, V. I.
1982BSolD1982...89M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A Comparison of the Distribution of Background Field Polarity
on Hα Synoptic Charts with Magnetographic Magnetic Field Observation
Authors: Makarov, V. I.; Stoyanova, M. N.
1982BSolD..11...94M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the dynamics of filament bands.
Authors: Makarov, V. I.; Fat'yanov, M. P.
1981BSolD1980...96M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the Large Scale Brightness Fluctuations in the Solar
Atmosphere
Authors: Krat, V. A.; Makarov, V. I.; Tavastsherna, K. S.
1980SoPh...68..237K Altcode:
The October 1976 spectroscopic observations of the solar chromosphere
with the great coronagraph of the Kislovodsk Station of the Pulkovo
Observatory were analysed using the autocorrelation method. The
autocorrelation function and the power spectrum were calculated. It
was found that the brightness distribution in the chromosphere
is essentially bimodal and has characteristic scales of 1.2 ×
104 km and 2.4 × 104 km. The supergranulation
(3.5 × 104 km) in the brightness field was found to show
up more faintly at all heights.

---------------------------------------------------------
Title: On Sign Inversion of the Solar Polar Magnetic Field in the
21ST Solar Cycle
Authors: Makarov, V. I.; Fatianov, M. P.
1980ATsir1130....1M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the Evolution of Filament Bands
Authors: Makarov, V. I.; Fatimov, M. P.
1980BSolD..10...96M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The solar flare of 1973, September 7.
Authors: Makarov, V. I.; Molodenskij, M. M.
1979BSolD1978...91M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On large-scale motions in the solar atmosphere.
Authors: Makarov, V. I.; Stoyanova, M. N.
1979BSolD1979...89M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: prediction of the solar corona structure.
Authors: Gnevyshev, M. N.; Nikol'Skij, G. M.; Makarov, V. I.
1979BSolD1978...75G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Photometry of comet Kohoutek (1973 XII).
Authors: Gun-der, Kim; Makarov, V. I.; Nikol'Skij, G. M.
1979KomTs.256R....G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Observations of the solar emission of the transition region
from the photosphere to the chromosphere from spectra in the Hα
region
Authors: Dubov, E. E.; Makarov, V. I.
1978SvA....22..382D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Cross structural plan of the earth's crust and the problem of
the manifestation of its plutonic elements on the surface (Tyan-Shan
and Turan plate as examples)
Authors: Makarov, V. I.; Solovyeva, L. I.
1976cspe.rept....1M Altcode:
The plutonic structures of the earth's crust based on an analysis of its
surface with the aid of orbital photographs are studied. It is found
that space photography is very valuable in studying the substructure
of the earth's crust. The possibility of distinguishing genetically
diverse components of the geochemical spectrum of the earth's surface
may have far-reaching consequences in fossil fuel exploration.

---------------------------------------------------------
Title: Neotectonic transverse structures of the Tyan-Shan and their
manifestation on space photographs
Authors: Makarov, V. I.; Solovyeva, L. I.
1976ntst.rept...10M Altcode:
The structural and geomorphological analysis of the Tyan'-Shan'
relief in conjunction with the deciphering of space photographs has
shown almost identical value of closely conjugated longitudinal and
cutting directions which were similarly evident in the morphology of
fold and boulder structural forms and rupture disturbances of different
order-from planetary to local. However, in different Tyan'-Shan' areas
or within one area but in different stages of the tectonic development,
these directions were manifested in such a way that one of them was
the main direction and others were secondary and formed structural
details. But in all the combinations, often varying in time, they have
inevitably accompanied each other and are closely connected genetically.

---------------------------------------------------------
Title: The chromospheric structure before the proton flare on
September 7, 1973 according to the films taken with a birefringent
filter in the Halpha and KCa+ lines.
Authors: Makarov, V. I.; Molodenskij, M. M.
1976BSolD1976Q..93M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The results of observations of chromospheric spicules in the
H8 and 3889 Å He I lines.
Authors: Makarova, V. V.; Makarov, V. I.
1975BSolD1975..100M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The structure of the lower chromosphere in the Na and He
(D1, D2, D3) lines from observations
with the 53-cm coronograph.
Authors: Makarov, V. I.; Shilova, N. S.
1973BSolD1973...69M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Spatial localization and brightness variations of Ellerman's
bombs.
Authors: den, O. E.; Makarov, V. I.; Molodenskij, M. M.
1973BSolD1973..101D Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Strong magnetic fields in the penumbra and the bright bridge
region in the large sunspot group observed in August 1972.
Authors: Shpitalnaya, A. A.; Makarov, V. I.; den, O. E.
1973BSolD1973Q..73S Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Investigation of the He I 3888.65 Å and H8 3889.05
Å lines in the spectrum of the solar chromosphere from observations
with a large coronograph.
Authors: Makarova, V. V.; Makarov, V. I.
1972BSolD1972...99M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The D3 helium line in the solar chromosphere from
observations with the 53-cm Lyot coronograph.
Authors: Makarov, V. I.
1972BSolD1972...71M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On photographing the form of the solar corona taken in the
5302 Å line at the High-Altitude Station (near Kislovodsk).
Authors: Gnevyshev, M. N.; Ioffe, S. B.; Makarov, V. I.; Smirnova,
T. A.
1972BSolD1972..105G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A dark band near the solar limb studied with the 53-cm Lyot
coronograph.
Authors: Makarov, V. I.; Platov, Yu. V.
1972BSolD1971...72M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Profiles of the Coronal Lines λλ 5303 Å, 6374 Å Based on
Large (53 cm) Coronograph Observations.
Authors: Makarova, V. V.; Makarov, V. I.; Nikol'Skii, G. M.
1971SvA....15..279M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Continuous spectra of umbrae and penumbrae of sunspots.
Authors: Makarov, V. I.
1969BSolD1969...85M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: On the law of limb darkening of umbra and penumbra of sunspots.
Authors: Makarov, V. I.
1969BSolD1969...72M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Razmery i forma solnechnykh piaten v nekotorykh uchastkakh
nepreryvnogo spektra
Authors: Makarov, V. I.
1968IzPul.184...58M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The non-radial structure of corona 5303 Å following proton
flares
Authors: Křivský, L.; Makarov, V. I.
1966BAICz..17..234K Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Nekotorye voprosy teorii solnechnykh piaten
Authors: Makarov, V. I.
1964IzPul..23...40M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Zavisimost temperatury iader solnechnykh piaten ot ikh
ploshchadi
Authors: Makarov, V. I.
1963IzPul..23...47M Altcode:
No abstract at ADS