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Publications of employees of a department.
Solar System Research, 2016, V. 50, No. 1, P. 13-23.
This paper presents and discusses selected reflectance spectra of 40 Main Belt asteroids. The spectra have been obtained by the author in the Crimean Laboratory of the Sternberg Astronomical Institute (2003–2009). The aim is to search for new spectral features that characterize the composition of the asteroids’ material. The results are compared with earlier findings to reveal substantial irregularities in the distribution of the chemical_mineralogical compositions of the surface material of a number of minor planets (10 Hygiea, 13 Egeria, 14 Irene, 21 Lutetia, 45 Eugenia, 51 Nemausa, 55 Pandora, 64 Angelina, 69 Hesperia, 80 Sappho, 83 Beatrix, 92 Undina, 129 Antigone, 135 Hertha, and 785 Zwetana), which are manifest at different rotation phases.
Busarev V.V., Barabanov S.I., Rusakov V.S., Puzin V.B., Kravtsov V.V.
Icarus, v. 262 (2015), p. 44-57.
Six asteroids including two NEAs, one of which is PHA, accessible for observation in September 2012 were investigated using a low-resolution (R 100) spectrophotometry in the range 0.35–0.90 lm with the aim to study features of their reflectance spectra. A high-altitude position of our Terskol Observatory (3150 m above sea level) favorable for the near-UV and visible-range observations of celestial objects allowed us to probably detect some new spectral features of the asteroids. Two subtle absorption bands centered at 0.53 and 0.74 lm were found in the reflectance spectra of S-type (32) Pomona and interpreted as signs of presence of pyroxenes in the asteroid surface matter and its different oxidation. Very similar absorption bands centered at 0.38, 0.44 and 0.67–0.71 lm have been registered in the reflectance spectra of (145) Adeona, (704) Interamnia, and (779) Nina of primitive types. We performed laboratory investigations of ground samples of known carbonaceous chondrites, Orguel (CI), Mighei (CM2), Murchison (CM2), Boriskino (CM2), and seven samples of low-iron Mg serpentines as possible analogs of the primitive asteroids. In the course of this work, we discovered an intense absorption band (up to 25%) centered at 0.44 lm in reflectance spectra of the low-Fe serpentine samples.
The results of ground-based spectrophotometry of the icy Galilean satellites of Jupiter — Europa, Ganymede, and Callisto — are discussed. The observations were carried out in the 0.39–0.92 μm range with the use of the CCD spectrometer mounted on the 1.25-m telescope of the Crimean laboratory of the Sternberg Astronomical Institute in March 2004. It is noted that the calculated reflectance spectra of the satellites mainly agree with the analogous data of the earlier ground_based observations and investigations in the Voyager and Galileo space missions. The present study was aimed at identifying new weak absorption bands (with the relative intensity of ~3–5%) in the reflectance spectra of these bodies with laboratory measurements (Landau et al., 1962; Ramaprasad et al., 1978; Burns, 1993; Busarev et al., 2008). It has been ascertained that the spectra of all of the considered objects contain weak absorption bands of molecular oxygen adsorbed into water ice, which is apparently caused by the radiative implantation of O+ ions into the surface material of the satellites in the magnetosphere of Jupiter. At the same time, spectral features of iron of different valence (Fe2+ and Fe3+) values typical of hydrated silicates were detected on Ganymede and Callisto, while probable indications of methane of presumably endogenous origin, adsorbed into water ice, were found on Europa. The reflectance spectra of the icy Galilean satellites were compared to the reflectance spectra of the asteroids 51 Nemausa (C-class) and 92 Undina (X-class).
V. V. Busarev1, M. N. Taran2, V. I. Fel’dman3 and V. S. Rusakov41 Lunar and Planetary Department, Sternberg State Astronomical Institute, Moscow State University, 119992 Moscow, Universitetskij pr., 13, Russian Federation (RF); e-mail: busarev@sai.msu.ru; 2 Department of Spectroscopic Methods, Institute of Geochemistry, Mineralogy and Ore Formation, Academy of Sciences of Ukraine, 03142 Kiev, Palladina pr., 34, Ukraine; 3 Division of Petrology, Geological Department of Moscow State University, 119992 Moscow, RF; 4 Division of Mossbauer Spectroscopy, Physical Department of Moscow State University, 119992 Moscow, RF.
—A preliminary study of the surface of the asteroid 21 Lutetia with ground-based methods is of significant importance, because this object is included into the Rosetta space mission schedule. From August 31 to November 20, 2000, about 50 spectra of Lutetia and the same number of spectra of the solar analog HD10307 (G2V) and regional standards were obtained with a resolution of 4 and 3 nm at the MTM-500 telescope television system of the Crimean astrophysical observatory. From these data, the synthetic magnitudes of the asteroid in the BRV color system have been obtained, the reflected light fluxes have been determined in absolute units, and its reflectance spectra have been calculated for a range of 370–740 nm. In addition, from the asteroid reflectance spectra obtained at different rotation phases, the values of the equivalent width of the most intensive absorption band centered at 430–440 nm and attributed to hydrosilicates of the serpentine type have been calculated. A frequency analysis of the values V (1, 0) confirmed the rotation period of Lutetia 0.d3405 (8.h172) and showed a two-humped light curve with a maximal amplitude of 0.m25. The color indices B–V and V–R showed no noticeable variations with this period. A frequency analysis of the equivalent widths of the absorption band of hydrosilicates near 430–440 nm points to the presence of many significant frequencies, mainly from 15 to 20 c/d (c/d is the number of cycles per day), which can be caused by a heterogeneous distribution of hydrated material on the surface of Lutetia. The sizes of these heterogeneities (or spots) on the asteroid surface have been estimated at 3–5 to 70 km with the most frequent value between 30 and 40 km.
objects (106 to 108 yr) were very low (15–30 K and 10−9–10−10 bar). At these thermodynamic conditions all volatiles excluding hydrogen, helium and neon were in the solid state. An initial mass fraction of silicates (silicates/(ices + dust)) in EKB parent bodies may be estimated as 0.15–0.30.
A. B. Makalkin, Institute of Earth Physics, RAS, Moscow, RF (e-mail: makalkin@uipe-ras.scgis.ru); Dorofeeva, V. A. Vernadsky Institute of Geochemisry, (RAS), Moscow, RF (e-mail: dorofeeva@geokhi.ru); V. V. Busarev, Sternberg State Astronomical Institute, Moscow University, RF; (e-mail: busarev@sai.msu.ru).
Moscow, Russian Federation; e-mail: busarev@sai.msu.ru.
Berezhnoy A.A., Kozlova E.A., Shevchenko V.V.
(1) Sternberg Astronomical Institute, Universitetskij pr., 13, Moscow, 19991, Russia.
Berezhnoy A.A., Kozlova E.A., Sinitsyn M.P., Shangaraev A.A., Shevchenko V.V.
AUTOMATED CREATION OF THE LUNAR HYPSOMETRIC MAP: TECHNIQUES OF COMPILING.
1Shevchenko V.V., 2Shingareva K.B., 1,2Lazarev E.N , 1Rodionova J.F.
2Moscow State University for Geodesy & Cartography (MIIGAiK), 105064, 4, Gorokhovskiy pereulok, Moscow, Russia, zhecka@inbox.ru.
119899, 13, Universitetskiy prospect, Moscow, Russia, jeanna@sai.msu.ru.
The new hypsometric maps of Venus and the Moon should improve and accelerate studying the surfaces of these planets and relief-forming processes. Additionally, these maps should be useful for students and scientists. The hypsometric map of Venus is produced in Lambert equal-area azimuth projection. Its height contours are obtained using the Magellan altitude data. To create Lunar Subpolar relief map the authors obtained heights from the A. Cook et.al. raster image of South Lunar Subpolar region (latitudes from -60° to -90°) being constructed in stereographic projection. [A.C. Cook, T.R. Watters, M.S. Robinson et.al. (2000) JGR, Vol.105, E5, 12023-12033]. Morphometric investigations of Venus and Lunar South Pole region surface have been fulfilled using our databases. The height profiles of some lunar craters being situated here and detailed profiles of the whole this area created by us describe the features of this region surface with the high resolution up to 100 meters.
THE LUNAR SUBPOLAR RELIEF MAP: THE WAYS AND TECHNIQUES OF COMPILING AND USING.
AUTOMATIC CREATION OF THE HYPSOMETRIC MAP OF VENUS.
E. N. Lazarev1, 2, J. F. Rodionova2.
2Sternberg State Astronomical Institute, 13 Universitetskiy pr., Moscow 119892, Russia, e-mail: jeanna@sai.msu.ru.
THE MORPHOMETRIC ANALISYS OF THE FEATURES OF MARTIAN CRATERS (10 – 20 km).
I.A. Ushkin11, G. G. Michael2.
1. Moscow State University, Vorobjovy Gory, 119899, Moscow, Russia, gray_pigeon@mail.ru .
2. ESA, Noordwijk, the Netherlands. greg.michael@rssd.esa.int.
SURVEY OF MARS CRATER TOPOGRAPHY FROM MOLA DATA.
THE MORPHOMETRIC ANALISYS OF THE FEATURES OF MARTIAN CRATERS.
I.A. Ushkin1, G. G. Michael2, E.A. Kozlova3 .
3. Sternberg State Astronomical Institute, 119899, Moscow, Russia.
Shevchenko. Sternberg State Astronomical Institute, Moscow University, 13 Universitetsky pr., 119992 Moscow, Russia, pugach@sai.msu.ru.
SOME PROBLEMS OF THE EVOLUTION OF ASTEROIDS - RUBBLE PILE.
G. A Leikin, A. N. Sanovich. Sternberg Astronomical Institute, Moscow 119899, Russia.
SOME PROBLEMS OF THE EVOLUTION OF ASTEROIDS – RUBBLE PILE.
ON A TIME SPAN OF ASTEROID – RUBBLE PILE (ARP) CONSOLIDATION AND A REASON OF LOW DENSITY OF SUCH ASTEROIDS.
G. A. Leikin and A.N. Sanovich.
A TIME ESTIMATE FOR CONSOLIDATION AND DISINTEGRATION OF AN ASTEROID – RUBBLE PILE.
THE SIMPLEST MODEL. A PRELIMINARY ANALYSIS.
ASTEROIDAL DAMAGE TO THE EARTH: IMPLICATIONS BY ASTEROIDS – RUBBLE PILES.
SPECTRAL FEATURES OF THE AVALANCHE DEPOSITS IN LUNAR CRATER REINER.
119992, Russia, 3Abastumany Astrophysical Observatory, Georgian Academy of Sciences, Georgia.
REMOTE DETERMINATION OF LUNAR SOIL MATURITY.
V.V.Shevchenko1,2, P.C.Pinet1, S.Chevrel1, Y.Daydou1, T.P.Skobeleva2, O.I.Kvaratskhelia3, C.Rosemberg1.
REMOTE METHOD OF IDENTIFICATION OF THE EJECTA LUNAR TERRAINS AND THEIR COMPOSITION FITURES.
V.V. Shevchenko1, 2, P. Pinet2, S. Chevrel2, S.G. Pugacheva1, Y. Daydou2.
MERCURY: LOCAL VARIATIONS OF THE PHOTOMETRIC RELIEF.
EVALUATING THE STRUCTURE OF THE SURFACE LAYER OF MERCURY.
PERMANENTLY SHADOWED AREAS AT THE LUNAR POLES.
V. V. Shevchenko1, E. A. Kozlova1, G. G. Michael1.
1.Sternberg State Astronomical Institute, 119899, Moscow, Russia. shev@sai.msu.ru.
MERCURY: SURFACE LAYER STRUCTURE FROM OPTICAL PROPERTIES.
VARIABLE RADIO EMISSION OF THE MOON AT 25 MM DURING THE LEONID 2000 METEOR SHOWER.
Geophysical Research Abstracts Volumi 3, 2001.
Radioseismology of the Moon and planets is based on registration and interpretation of electromagnetic radiation of seismic origin. The frequency of such electromagnetic radiation varies from some kHz to the frequency of soft X-ray radiation. The most probable two models of transformation of mechanical stress into electromagnetic radiation are: 1) the formation of new microcracks; 2) charges arising at the peaks of existing cracks drawing under the action of increasing load. We observed the Moon on November 16 - 18 with the 32 m antenna of the Ventspils International Radio Astronomy Center at 12.2 GHz. The half-power beamwidth was 3.5 arcminutes. The DSB bandwidth is 2 x 22 MHz and output time constant is 1 sec. The observable lunar region was a seismic active region (30W, 5S). We could not exactly track the antenna with the velocity of the Moon, an observable region lagged behind and during 30 minutes of observation cycle the beam draw a near 15 arcminutes long trip on the lunar surface in direction to Mare Serentatis. During the morning of November 17 we registered significant quasiperiodic oscillations of the lunar radio emission starting near 1:44 UT. Similar oscillations were registered on November 18 starting near 2:28 UT. More or less intensive oscillations (quasiperiods were equal to 1-2 minutes) were received until November 18, 9:30 UT with bottom to peak heights of some K, sometimes up to 10K. The character of these oscillations is different from atmospheric fluctuations. The time of observed oscillations does not contradicts with predictions of McNaught about the Leonid activity on the Moon. Similar oscillations were registered after the Lunar Prospector impact (July 31, 1999) during observations of the Moon at 13 and 21 cm. These results can be explained by detection of the lunar radio emission of seismic origin. The interpretation of quasiperiodic oscillations in terms of Nikolaevsky's waves is given. Implications of radioseismic method of investigations of the Moon for determination of the intensity of meteor showers on lunar orbit and for estimation of the mineral composition of lunar regolith are described.
THE CHEMICAL COMPOSITION OF LUNAR REGOLITH NEAR COLD TRAPS.
In our previous papers we have found that a significant part of cometary matter is captured by the Moon after a low-speed collision between a comet and the Moon. Now we consider the chemical composition of impact vapour formed after a such collision based on new kinetical model of chemical processes. We have found that H2O, CO2, and SO2 are main H-, C-, and S-containing species respectively in the fireball. The temperature in polar regions near cold traps is suitable for the presence of some volatile compounds (sulfur, carbon and hydrocarbons) in the regolith. We estimate an amount of sulfur- and carbon- containing species delivered to lunar polar regions due to cometary impacts. Our estimations can be checked during conduction of observations by the SMART-1 spacecraft.
THE SPACE ANGULAR FUNCTION OF THE MOON'S THERMAL EMISSION (10 -12 MICRON).
The features of the lunar surface, varying in their individual properties, have a brightness constant in time, and the dynamics of reflected and own radiation is determined in each case only by the geometry of observing conditions at any given moment. Therefore, using the known characteristics of the lunar features, we can determine the standard values of the radiation emitted or reflected by a great number of particular objects, which form a system of standards in a certain wavelength and energy-flux range. The space function of the Moon's thermal emission was constructed by results of the statistical processing of the database 1655 lunar sites in the vector form. The database contains the brightness characteristics of the emitted and reflected radiation measured in an IR (10-12 mm) and a visible (0.445 mm) range for 23 Moon's phase angles and 1954 lunar regions. The space function is based on physical regularities and statistical relationship between the intensity of thermal and reflected radiation, the geometry of observation and illumination, and the albedo and microrelief of the lunar surface. An analytic formula of the dependence of radiation temperature of the lunar surface on the incidence angular parameters make it possible to calculate the infrared temperature for any geometry of the angular parameters. The root-mean-square error in the determination of the radiation temperature is +1.5 K. The computer images were constructed in the form of contour maps of brightness and temperature, of thermal inertia and other thermal parameters, using the database of brightness and temperatures values for lunar-surface areas.
THE CRATERING FEATURES OF THE BASIN "SOUTH POLE-AITKEN".
Morphological features of craters in the South Pole-Aitken are studied. Craters in the basin are compared to craters located in highland and mare regions. In comparision studies, the following morphological features were considered: the degree of rim degradation; the presence of terraces and faults, hills, peaks and ridges, fissures and chains of small craters, lava on the crater floor; the character of the floor; and the presence of ray systems. In the basin 3.8 million sq. km in area, 1538 craters of 10 km in diameter or larger are found. Craters in the South Pole-Aitken are found to be less degraded than those in the mare region. Additionaly, terraces on the inner slopes of craters in the basin are less degraded, and more faults are observed in the craters in the highland region. The craters in the three regions studed are similar in the presence of peaks and hills, while the density of craters with fissures and chains of small craters on the floor are greater in the mare! region. No craters with ray systems are found in the basin. The South Pole Aitken Basin is assumed to have formed late in the period of heavy bombardment. The morphology of craters in the mare region is found to differ drastically from those in the basin and the highland region. A low crater density and the abundance of crater-ruins and craters with faults in the mare region are due to lava flooding of ancient depressions during the period of basaltic volcanism and the destruction of the majority of craters formed in the preceding heavy bombardment period. The mare regions differs in the densities of craters with fissures and chains of small craters, peaks and lavas on the floor. We attribute these distinctions to the difference in endogenic processes that proceeded in the considered regions. The endogenic processes should reveal themselves more often in the mare regions because the lunar crust here is much thinner than in the highland regions.
LUNAR RESOURCES FOR RESCUE OF MANKIND IN XXI CENTURY.
In results of many ecological investigations it has been found that the permissible level of the energy production inside Earth's environment is about 0.1% of solar energy received by Earth's surface. The value is about 90 TW (90 x 10 12 Watt). On the other hand, the general estimation shows that the total energy use (and production, accordingly) in the world is about 16 TW in the end of 2000. This value will increase by factor of two (about 34 TW) to the year 2050. If the tendency will be preserved the total energy production in the world will approach to 98 TW to the year 2100. It means the permissible level of the energy production inside Earth's environment will be exceeded. But it is obviously that the processes destroying Earth's environment in global scale will begin before it - after middle of century. Hence, the first result of the practical actions for rescue of the Earth's environment must be obtained not late than in 2020 - 2030. It means that general decisions must be approved now or in the beginning of the new century. The only way to resolve this problem consists in the use of extraterrestrial resources. The nearest available body - source of space resources is the Moon. The most known now space energy resource is lunar helium-3. Very likely, the lunar environment contains new resource possibilities unknown now. So, the lunar research space programs must have priority not only in fundamental planetary science, but in practical purposes too..

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