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. Bibcode: 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 > 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 cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/660/A16 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. Bibcode: 2022yCat..36600016S Altcode: We have constructed an improved version of the LQAC5 catalogue (Souchay et al., 2019A&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>10 mas/yr, {chi}μ>5, π/σπ<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. Bibcode: 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 (>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 >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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 & Laskar 2004). The second scenario includes friction at the core-mantle boundary, which increases the probabilities of capture during one crossing (Peale & Boss 1977, Correia & 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 >= 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 < 1 milliarcsecond (mas) position, < 1 mas/year proper motion, and < 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 2002A&A...392.1069K Altcode: With Tycho-2 BT and VT photometry of Hipparcos stars with π > 8.0 mas, σπ/π < 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 2001yCat.1275....0U Altcode: The AC 2000.2 is a revised version of the 1997 release of the AC 2000 (Cat. <I/247>). 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. Bibcode: 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. Bibcode: 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. Bibcode: 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) - < L-1(t) > 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 < q(N) - q(S), W(N)-W(S) > and < W(t), q (t,r) > 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1990IAUS..138..281M Altcode: No abstract at ADS Title: Geological Geomorphological Study of Modern Tectonic Movements Authors: Trifonov, V. G.; Makarov, V. I. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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| > 30°. The velocity of the migration is greater in the zone |φ| > 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1986BSolD...4...63M Altcode: No abstract at ADS Title: Solar observatories of France. Authors: Gnevyshev, M. N.; Makarov, V. I. Bibcode: 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. Bibcode: 1986BSolD1986R..63M Altcode: An analysis of the distribution of background magnetic fields in the 20th solar cycle using H&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&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. Bibcode: 1986KodOB...7.....M Altcode: No abstract at ADS Title: Longitudinal Distribution of Neutral Magnetic Lines - Part Two Authors: Makarov, V. I.; Tavastsherna, K. S. Bibcode: 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. Bibcode: 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. Bibcode: 1986BSolD...9...64M Altcode: No abstract at ADS Title: On the Forecast of SOLAR-CYCLE-22 Authors: Makarov, V. I. Bibcode: 1986BSolD...8...57M Altcode: No abstract at ADS Title: On the forecast of solar cycle 22. Authors: Makarov, V. I. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1984BSolD...4...84M Altcode: No abstract at ADS Title: On the Structure of Polar Faculae Authors: Makarov, V. I.; Makarova, V. V. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1983BSolD...5...93M Altcode: No abstract at ADS Title: Latitude Zones of Background Magnetic Fields in the 19TH Solar Cycle Authors: Makarov, V. I. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1983BSolD1983R..93M Altcode: Mean latitudes of background magnetic fields (1955 - 1962) have been calculated and analysed from H&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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 > 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1982BSolD..11...94M Altcode: No abstract at ADS Title: On the dynamics of filament bands. Authors: Makarov, V. I.; Fat'yanov, M. P. Bibcode: 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. Bibcode: 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. Bibcode: 1980ATsir1130....1M Altcode: No abstract at ADS Title: On the Evolution of Filament Bands Authors: Makarov, V. I.; Fatimov, M. P. Bibcode: 1980BSolD..10...96M Altcode: No abstract at ADS Title: The solar flare of 1973, September 7. Authors: Makarov, V. I.; Molodenskij, M. M. Bibcode: 1979BSolD1978...91M Altcode: No abstract at ADS Title: On large-scale motions in the solar atmosphere. Authors: Makarov, V. I.; Stoyanova, M. N. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1978SvA....22..382D 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. Bibcode: 1978AZh....55..666D 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1971SvA....15..279M 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. Bibcode: 1971AZh....48..360M Altcode: No abstract at ADS Title: Continuous spectra of umbrae and penumbrae of sunspots. Authors: Makarov, V. I. Bibcode: 1969BSolD1969...85M Altcode: No abstract at ADS Title: On the law of limb darkening of umbra and penumbra of sunspots. Authors: Makarov, V. I. Bibcode: 1969BSolD1969...72M Altcode: No abstract at ADS Title: Razmery i forma solnechnykh piaten v nekotorykh uchastkakh nepreryvnogo spektra Authors: Makarov, V. I. Bibcode: 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. Bibcode: 1966BAICz..17..234K Altcode: No abstract at ADS Title: Nekotorye voprosy teorii solnechnykh piaten Authors: Makarov, V. I. Bibcode: 1964IzPul..23...40M Altcode: No abstract at ADS Title: Zavisimost temperatury iader solnechnykh piaten ot ikh ploshchadi Authors: Makarov, V. I. Bibcode: 1963IzPul..23...47M Altcode: No abstract at ADS