Работы и публикации сотрудников отдела.

Бережной А.А., Клумов Б.А., Фортов В.Е., Шевченко В.В.

Эту статью можно найти на сервере журнала Письма в ЖЭТФ.

Лунный лед: можно ли определить его происхождение?

Эту статью можно найти на сервере журнала Письма в ЖЭТФ.

Тепловой режим холодных ловушек на Луне.

А.А.Бережной, Государственный Астрономический Институт им. Штернберга, 1999.

Проведено моделирование теплового режима грунта холодных ловушек на Луне на глубине до нескольких метров. Показано, что если температура в холодных ловушках на глубине 1-2 см практически не отличается от температуры поверхности, то в состав полярных льдов входят H2O, SO2, CO2. Если же в холодных ловушках образуется теплоизоляционный слой, как в экваториальных районах, то температура на глубине 1-2 м на 50-60 K выше, чем на поверхности, и включение в состав полярных отложений SO2 и CO2 вряд ли возможно. Результаты расчетов средней температуры грунта холодных ловушек можно проверить при проведении наблюдений теплового излучения грунта холодных ловушек в области длин волн 0.1 мм - 10 см. Если будет обнаружено, что средняя яркостная температура полярных лунных районов практически не увеличивается с длиной волны, то этот факт можно рассматривать как косвенное доказательство наличия водяного льда.

Автореферат кандидатской диссертации Бережного А.А.

Более подробное описание моих научных исследований и научное сообщение о моей работе за 2000 год содержится на сайте информационной системы "Наука и инновации"

Radio Emission of the Moon before and after the Lunar Prospector impact, Proceedings of the Fourth International Conference on Exploration and Utilisation of the Moon.

Berezhnoi A.A., Gusev S.G., Khavroshkin O.B., Poperechenko B.A., Shevchenko V.V., Tzyplakov V.A.

Photochemical Model of Impact-Produced Lunar Atmosphere, Proceedings of the Fourth International Conference on Exploration and Utilisation of the Moon.

IDENTIFICATION OF LUNAR ROCK TYPES.

A. A. Berezhnoy1,2, N. Hasebe1, M. Kobayashi1, G. Michael3 and N. Yamashita1 1Advanced Research Institute for Science and Engineering, Waseda University, Tokyo, Japan 2Sternberg Astronomical Institute, Moscow, Russia 3German Aerospace Center, Institute for planetary research, Berlin, Germany

HIGH PURITY GE GAMMA-RAY SPECTROMETER ON JAPANESE LUNAR POLAR ORBITER SELENE.

N. Hasebe1, M.-N. Kobayashi1, T. Miyachi1, O. Okudaira1, Y. Yamashita1, E. Shibamura2, T. Takashima3, A.A.Brezhnoy1, 1Advanced Research Institute for Science and Engineering, Waseda University (Tokyo 169-8555, Japan), 2Saitama Prefectural University (Koshigaya, Saitama 343-8540, Japan), 3Institute of Space and Astronautical Science, JAXA (Sagamihara, Kanagawa 229-8510, Japan), 4Sternberg Astronomical Institute, Moscow State Univ.

GAMMA RAYS FROM MAJOR ELEMENTS BY THERMAL NEUTRON CAPTURE REACTIONS:
EXPERIMENT AND SIMULATION FOR PLANETARY GAMMA-RAY SPECTROSCOPY.

N. Yamashita1, N. Hasebe1, M. -N. Kobayashi1, T. Miyachi1, O. Okudaira1, E. Shibamura2, A. A. Berezhnoy1,3, 1Advanced Research Institute for Science and Engineering, Waseda Univ., 3-4-1, Okubo, Shinjuku, Tokyo 169-8555 Japan (nao.yamashita@toki.waseda.jp), 2Saitama Prefectural University, 3Sternberg Astronomical Institute.

Petrologic mapping of the Moon using Fe, Mg, and Al abundances

A.A. Berezhnoy a,*, N. Hasebe a, M. Kobayashi a, G. Michael b, N. Yamashita a
a Advanced Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku-ku, 169-8555 Tokyo, Japan
b German Aerospace Centre, Institute for Planetary Research, Rutherfordstr. 2, 12489 Berlin-Adlershof, Germany
Received 16 August 2004; received in revised form 27 January 2005; accepted 1 March 2005

A comparison between the abundances of major elements on the Moon determined by Lunar Prospector gamma ray spectrometer and those in returned lunar samples is performed. Lunar Prospector shows higher Mg and Al content and lower Si content in western maria in comparison with the lunar sample collection. Lunar Prospector overestimated the Mg content by about 20%. There are no elemental anomalies at the lunar poles: this is additional evidence for the presence of polar lunar hydrogen. Using Mg, Fe, and Al abundances, petrologic maps containing information about the abundances of ferroan anorthosites, mare basalts, and Mgrich rocks are derived. This approach is useful for searching for cryptomaria and Mg-rich rocks deposits on the lunar surface. A search is implemented for rare rock types (dunites and pyroclastic deposits). Ca-rich, Al-low small-area anomalies are detected in the far side highlands.

Optical spectroscopy of comet C/2000 WM1 (LINEAR) at the Guillermo Harro Astrophysical Observatory in Mexico

Klim I.Churyumov1, Igor V.Luk'yanyk1, Alexei A.Berezhnoi2,3, Vahram H.Chavushyan2, Leo Sandoval4 and Alejandro A.Palma2,4

1Astronomical Observatory, Kyiv National Shevchenko University, Kyiv, Ukraine;
2Instituto Nacional de Astrofisica, Optica y Electronica, Tonantzintla, Puebla, Mexico;
3Sternberg Astronomical Institute, Moscow, Russia;
4Benemerita Universidad Autonoma de Puebla, Puebla, Mexico
March 24, 2002

Preliminary analysis of middle resolution optical spectra of comet C/2000 WM1 (LINEAR) obtained on November 22, 2001 is given. The emission lines of the molecules C2, C3, CN, NH2, H2O+ and presumably CO (Asundi and triplet bands), C−2 were identified in these spectra. By analyzing the brightness distributions of the C2, C3, CN emission lines along the spectrograph slit we determined some physical parameters of these neutral molecules - the velocity of expansion of molecules within the coma and their lifetimes. The Franck-Condon factors for the CO Asundi bands and C−2 bands were calculated by using a Morse potential model.

Interpretation of the microwave non-thermal radiation of the Moon during impact events

V. Grimalsky1, A. Berezhnoy2, 3, A. Kotsarenko4, N. Makarets5, S. Koshevaya6, and R. P´erez Enr´ıquez4

1Instituto Nacional de Astrofisica, Optica y Electronica (INAOE), Puebla, Mexico
2Advanced Research Institute for Science and Engineering, Waseda University, Tokyo, Japan
3Now at: Sternberg Astronomical Institute, Moscow University, Moscow, Russia
4Centro de Geociencias, Juriquilla, UNAM, Quer´etaro, Mexico
5Kyiv National Shevchenko University, Faculty of Physics, Kyiv, Ukraine
6Universidad Autonoma del Estado de Morelos (UAEM), CIICAp, Cuernavaca, Mexico
Received: 30 June 2004 - Revised: 23 November 2004 - Accepted: 24 November 2004 - Published: 30 November 2004

The results of recent observations of the nonthermal electromagnetic (EM) emission at wavelengths of 2.5 cm, 13 cm, and 21 cm are summarized. After strong impacts of meteorites or spacecrafts (Lunar Prospector) with the Moon's surface, the radio emissions in various frequency ranges were recorded. The most distinctive phenomenon is the appearance of quasi-periodic oscillations with amplitudes of 3-10K during several hours. The mechanism concerning the EM emission from a propagating crack within a piezoactive dielectric medium is considered. The impact may cause the global acoustic oscillations of the Moon. These oscillations lead to the crackening of the Moon's surface. The propagation of a crack within a piezoactive medium is accompanied by the excitation of an alternative current source. It is revealed that the source of the EM emission is the effective transient magnetization that appears in the case of a moving crack in piezoelectrics. The moving crack creates additional non-stationary local mechanical stresses around the apex of the crack, which generate the non-stationary electromagnetic field. For the cracks with a length of 0.1-1μm, the maximum of the EM emission may be in the 1-10GHz range.

A three end-member model for petrologic analysis of lunar prospector gamma-ray spectrometer data

A.A. Berezhnoya,1, N. Hasebea, M. Kobayashia, G.G. Michaelb,_, O. Okudairaa, N. Yamashitaa
aAdvanced Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku-ku, 169-8555 Tokyo, Japan
bGerman Aerospace Centre, Institute for Planetary Research, Rutherfordstr. 2, 12489 Berlin-Adlershof, Germany
Received 24 March 2004; received in revised form 10 February 2005; accepted 20 February 2005

We analyze preliminary Lunar Prospector gamma-ray spectrometer data. Al-Mg and Fe-Mg petrologic maps of the Moon show that Mg-rich rocks are located in Mare Frigoris, the South Pole Aitken basin, and in some cryptomaria. Analysis of distances of Lunar Prospector pixels from three end-member plane in Mg-Al-Fe space reveals existence of Ca-rich, Al-low small-area anomalies in the farside highlands. An Mg-Th-Fe petrologic technique can be used for estimation of abundances of ferroan anorthosites, mare basalts, KREEP basalts, and Mg-rich rocks.

Impacts as sources of the exosphere on Mercury

Alexey A. Berezhnoy a,b,∗, Boris A. Klumov c
a Sternberg Astronomical Institute, Moscow State University, Universitetskij pr., 13, 119991 Moscow, Russia
b Rutgers University, Department of Chemistry and Chemical Biology, 610 Taylor Road, Piscataway, NJ 08854-8087, USA
c Max-Planck-Institut für Extraterrestrische Physik, D-85740 Garching, Germany
Received 29 August 2007; revised 13 January 2008

Chemical processes associated with meteoroid bombardment of Mercury are considered. Meteoroid impacts lead to production of metal atoms as well as metal oxides and hydroxides in the planetary exosphere. By using quenching theory, the abundances of the main Na-, K-, Ca-, Fe-, Al-, Mg-, Si-, and Ti-containing species delivered to the exosphere during meteoroid impacts were estimated. Based on a correlation between the solar photo rates and the molecular constants of atmospheric diatomic molecules, photolysis lifetimes of metal oxides and SiO are estimated. Meteoroid impacts lead to the formation of hot metal atoms (0.2-0.4 eV) produced directly during impacts and of very hot metal atoms (1-2 eV) produced by the subsequent photolysis of oxides and hydroxides in the exosphere of Mercury. The concentrations of impact-produced atoms of the main elements in the exosphere are estimated relative to the observed concentrations of Ca, assumed to be produced mostly by ion sputtering. Condensation of dust grains can significantly reduce the concentrations of impact-produced atoms in the exosphere. Na, K, and Fe atoms are delivered to the exosphere directly by impacts while Ca, Al, Mg, Si, and Ti atoms are produced by the photolysis of their oxides and hydroxides. The chemistry of volatile elements such as H, S, C, and N during meteoroid bombardment is also considered. Our conclusions about the temperature and the concentrations of impact-produced atoms in the exosphere of Mercury may be checked by the Messenger spacecraft in the near future and by BepiColombo spacecraft some years later.

Possibility of the presence of S, SO2, and CO2 at the poles of the Moon

Alexey A. Berezhnoy*, Nobuyuki Hasebe, Takuji Hiramoto
Advanced Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku-ku，Tokyo 169-0071
* Also at Sternberg Astronomical Institute, Moscow State University, Moscow, Russia
Email (AB) iac02074@kurenai.waseda.jp and Boris A. Klumov Institute of Dynamics of Geospheres, Moscow, Russia
(Received 2003 March 4)

The presence of volatiles near lunar poles is studied. The chemical composition of a lunar atmosphere temporarily produced by comet impact is studied during day and night. C-rich and long-period comets are insufficient sources of water ice on the Moon. O-rich short-period comets deliver significant amounts of H2O, CO2, SO2, and S to the Moon. An observable amount of polar hydrogen can be delivered to the Moon by single impact of O-rich short-period comet with diameter of 5 km in the form of water ice. The areas where CO2 and SO2 ices are stable against the thermal sublimation are estimated as 300 and 1500 km2, respectively. If water ice exists in the 2 cm top regolith layer CO2 and SO2 ices can be stable in the coldest parts of permanently shaded craters. The delivery rate of elemental sulfur near the poles is estimated as 106 g/year. The sulfur content is estimated to be as high as 1 wt % in polar regions. The SELENE gamma-ray spectrometer can detect sulfur polar caps on the Moon if the sulfur content is higher than 1 wt %. This instrument can check the presence of hydrogen and minerals with unusual chemical composition at the lunar poles.

Бусарев В.В.

НОВЫЕ СПЕКТРЫ ОТРАЖЕНИЯ 40 АСТЕРОИДОВ: СРАВНЕНИЕ С ПРЕДШЕСТВУЮЩИМИ РЕЗУЛЬТАТАМИ И ИНТЕРПРЕТАЦИЯ

Московский гос. университет им. М. В. Ломоносова, Гос. астрономический институт им. П. К.Штернберга (ГАИШ МГУ), (полная версия статьи) ї 2015 г.Москва

Аннотация
В статье представлены и обсуждаются спектры отражения 40 астероидов Главного пояса, полученные автором в Крымской лаборатории ГАИШ МГУ в 2003-2009 годах.

Научно-популярный обзор:

ЧЕЛЯБИНСКИЙ БОЛИД КАК НАПОМИНАНИЕ О ГЛАВНОМ ПРОЦЕССЕ СОЛНЕЧНОЙ СИСТЕМЫ

В.В. Бусарев (ГАИШ МГУ, Москва)
(предварительный вариант статьи, опубликованной в ?2(50) 2013 г. журнала "Наука из первых рук")

Докторская диссертация на тему:

"ИЗУЧЕНИЕ ПРИРОДЫ АСТЕРОИДОВ МЕТОДАМИ СПЕКТРОФОТОМЕТРИИ"

АВТОРЕФЕРАТ
диссертации на соискание ученой степени доктора
физико-математических наук.

О НЕОДНОРОДНОСТИ ВЕЩЕСТВА АСТЕРОИДОВ 10 ГИГИИ, 135 ГЕРТЫ И 196 ФИЛОМЕЛЫ ПО СПЕКТРАМ ОТРАЖЕНИЯ

Государственный астрономический институт им. П.К. Штернберга МГУ, Москва
Поступила в редакцию 21.12.2009 г.

СПЕКТРАЛЬНЫЕ ИССЛЕДОВАНИЯ АСТЕРОИДОВ 21 ЛЮТЕЦИЯ И 4 ВЕСТА КАК ОБЪЕКТОВ КОСМИЧЕСКИХ МИССИЙ

Государственный астрономический институт им. П.К. Штернберга МГУ, Москва
Поступила в редакцию 21.12.2009 г.

Астрофизические методы исследования Луны и малых небесных тел

В.В.Бусарев, Государственный астрономический институт им.П.К.Штернберга, 2009.

RESULTS OF REFLECTANCE SPECTRAL, MÖSSBAUER, X-REY AND ELECTRON MICROPROBE INVESTIGATIONS OF TERRESTRIAL SERPENTINE SAMPLES.

V. V. Busarev1, M. V. Volovetskij2, M. N. Taran3, V. I. Fel'dman4, T. Hiroi5 and G. K. Krivokoneva6
1Sternberg State Astronomical Institute, Moscow University, 119992 Moscow, Russia Federation (RF), e-mail: busarev@sai.msu.ru ;
2Division of Mossbauer Spectroscopy, Physical Department of Moscow State University, 119992 Moscow, RF
3 Institute of Geochemistry, Mineralogy and Ore Formation, Academy of Sciences of Ukraine, 03142 Kiev, Ukraine;
4Division of Petrology, Geological Department of Moscow State University, 119992 Moscow, RF;
5Department of Geological Sciences, Brown University, Providence, Rhode Island 02912;
6All-Russia Research Institute of Mineral Resources (VIMS), 119017 Moscow, RF.
48th Vernadsky-Brown Microsymposium on Comparative Planetology, October 20-22, 2008, Moscow, abstract No. 6.

Научно-популярный обзор

Астероиды

Научно-популярный обзор

Кометы

Научно-популярный обзор

Метеоры и метеориты

Спектральный и спектрально-частотный методы исследования безатмосферных тел Солнечной системы

В.В.Бусарев, В.В.Прокофьева-Михайловская, В.В.Бочков.
УСПЕХИ ФИЗИЧЕСКИХ НАУК, Том 177, ?6, Июнь 2007г.

ИССЛЕДОВАНИЕ СТРУКТУРЫ ПОВЕРХНОСТИ М-АСТЕРОИДА 21 ЛЮТЕЦИЯ СПЕКТРАЛЬНЫМ И ЧАСТОТНЫМ МЕТОДАМИ

В. В. Прокофьева*, В. В. Бочков*, В. В. Бусарев**
*Научно-исследовательский институт Крымская астрофизическая обсерватория, Украина; e-mail: prok@crao.crimea.ua
**Государственный астрономический институт им. П.К. Штернберга, Москва, Россия.
'Астрономический вестник', т. 39, ?5, с. 457-468, 2005

Spectral and spectral-frequency methods of investigating atmosphereless bodies of the Solar system

The Surface Structure of the M-Type Asteroid 21 Lutetia:Spectral and Frequency Analysis

V. V. Prokof'eva*, V. V. Bochkov*, and V. V. Busarev**
*Research Institute, Crimean Astrophysical Observatory, National Academy of Sciences of Ukraine, p/o Nauchnyi, Crimea, 334413 Ukraine
**Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119899 Russia
Received November 25, 2004

-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.

Астероиды неоднозначных спектральных типов: 11 Партенопа, 198 Ампелла, 201 Пенелопа и 21 Лютеция

Выполненные нами в разные годы спектральные исследования показывают, что S-астероиды 11 Партенопа и 198 Ампелла, M-астероиды 201 Пенелопа и 21 Лютеция имеют особенности состава вещества, не согласующиеся с их спектральными типами.

HYDRATED SILICATES ON EDGEWORTH-KUIPER OBJECTS - PROBABLEWAYS OF FORMATION

V. V. BUSAREV, Sternberg State Astronomical Institute, Moscow University, Russian Federation (RF) (E-mail: busarev@sai.msu.ru);
V. A. DOROFEEVA, Vernadsky Institute of Geochemistry, Russian Academy of Sciences (RAS), Moscow, RF;
A. B. MAKALKIN, Institute of Earth Physics, RAS, Moscow, RF

Visible-range absorption bands at 600-750 nm were recently detected on two Edgeworth-Kuiper Belt (EKB) objects (Boehnhardt et al., 2002). Most probably the spectral features may be attributed to hydrated silicates originated in the bodies. We consider possibilities for silicate dressing and silicate aqueous alteration within them. According to present models of the protoplanetary disk, the temperatures and pressures at the EKB distances (30-50 AU) at the time of formation of the EKB
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.
Decay of the short-lived 26Al in the bodies at the early stage of their evolution and their mutual collisions (at velocities ≥1.5 km s−1) at the subsequent stage were probably two main sources of their heating, sufficient for melting of water ice. Because of the former process, large EKB bodies (R ≥ 100 km) could contain a large amount of liquid water in their interiors for the period of a few 106 yr. Freezing of the internal ocean might have begun at ≈ 5 × 106 yr after formation of the solar nebula (and CAIs). As a result, aqueous alteration of silicates in the bodies could occur.
A probable mechanism of silicate dressing was sedimentation of silicates with refractory organics, resulting in accumulation of large silicate-rich cores. Crushing and removing icy covers under collisions and exposing EKB bodies' interiors with increased silicate content could facilitate detection of phyllosilicate spectral features.

SPECTRAL SIGNS OF CARBONACEOUS CHONDRITIC MATERIAL ON (21) LUTETIA

V.V. Busarev, Sternberg Astronomical Institute (SAI), Moscow University, Universitetskij pr., 13, Moscow, 119992
Russia, busarev@sai.msu.ru.

A COMBINED SPECTRAL-FREQUENCY METHOD OF INVESTIGATIONS OF SMALL OR DISTANT PLANETS.

V. V. Busarev1, V. V. Prokof'eva2, and V. V. Bochkov2
1 Sternberg State Astronomical Institute, Moscow University, Universitetskij pr., 13, Moscow 119992, Russian Federation, e-mail: busarev@sai.msu.ru;
2 Research Institute Crimean Astrophysical Observatory, p/o Nauchnyi, Crimea 334413, Ukraine, e-mail: prok@crao.crimea.ua

POSSIBLE SPECTRAL SIGNS OF SERPENTINES AND CHLORITES IN REFLECTANCE SPECTRA OF CELESTIAL SOLID BODIES

V. V. Busarev1, M. N. Taran2, V. I. Fel'dman3 and V. S. Rusakov4
1 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.

FORMATION OF HYDRATED SILICATES IN EDGEWORTH-KUIPER BELT OBJECTS.

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).

Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

SOME OBSERVATIONAL INDICATIONS OF THE HISTORY AND SRUCTURE OF OUR PLANETARY SYSTEM.

Sternberg State Astronomical Institute, Moscow University, Moscow, Russian Federation; e-mail: busarev@sai.msu.ru.

Brown University - Vernadsky Institute Microsymposium 34, October 8-9, 2001, Moscow, Russia

Where Some Asteroid Parent Bodies

35th Lunar and Planetary Science Conference, 2004, Houston, Texas, Abstract 1026.

OXIDIZED AND HYDRATED SILICATES ON M- AND S- ASTEROIDS: SPECTRAL INDICATIONS.

32nd Lunar and Planetary Science Conference, March 12-16, 2001, Houston, Texas, Abstract 1927.

Где могут быть скрыты родительские тела астероидов?

Горячев М.В.

Лазарев Е.Н.

ГИПСОМЕТРИЧЕСКАЯ КАРТА ВЕНЕРЫ: МЕТОДЫ СОЗДАНИЯ И ИСПОЛЬЗОВАНИЯ

Аспирант Е.Н. Лазарев
Московский Государственный Университет Геодезии и Картографии

ГЕНЕРАЛИЗАЦИЯ ТОЧЕЧНЫХ МАССИВОВ ДАННЫХ ПОСРЕДСТВОМ ИСПОЛЬЗОВАНИЯ ДОПОЛНИТЕЛЬНЫХ ВОЗМОЖНОСТЕЙ ГЕОИНФОРМАЦИОННЫХ СИСТЕМ

РАЗРАБОТКА МЕТОДИКИ И ГИС-ТЕХНОЛОГИИ СОЗДАНИЯ ГИПСОМЕТРИЧЕСКИХ КАРТ ЛУНЫ ПО ДАННЫМ КОСМИЧЕСКИХ СЪЕМОК

Лазарев Евгений Николаевич
АВТОРЕФЕРАТ
диссертации на соискание ученой степени кандидата технических наук
Москва - 2008

История картографирования Марса

RASTER VENUS AND LUNAR MAPS AS A SOURCE FOR OBTAINING VECTOR TOPOGRAPHIC DATA

Evgeniy Lazarev, Janna Rodionova
Evgeniy Lazarev; Moscow State University of Geodesy and Cartography (MIIGAiK);
121614, Osenniy bulvar, Moscow, Russia;
+7(495)412-6176, zhecka@inbox.ru
Dr. Janna Rodionova; Sternberg State Astronomical Institute;
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 -60њ to -90њ) 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

Evgeniy Lazarev1,2, Zhanna Rodionova2
1Moscow State University of Geodesy and Cartography (MIIGAiK) 105064, Gorokhovskiy pereulok, 4, Moscow, Russia zhecka@inbox.ru
2Sternberg State Astronomical Institute 119991, Universitetskiy prospect, 13, Moscow, Russia jeanna@sai.msu.ru

AUTOMATIC CREATION OF THE HYPSOMETRIC MAP OF VENUS.

E. N. Lazarev1, 2, J. F. Rodionova2.
1Moscow State University of Geodesy and Cartography, 4 Gorokhovskiy per., Moscow 105064, Russia, e-mail: zhecka@inbox.ru,
2Sternberg State Astronomical Institute, 13 Universitetskiy pr., Moscow 119892, Russia, e-mail: jeanna@sai.msu.ru

Гипсометрическая карта Венеры

AUTOMATED CREATION OF THE LUNAR HYPSOMETRIC MAP: TECHNIQUES OF COMPILING.

1Shevchenko V.V., 2Shingareva K.B., 1,2Lazarev E.N , 1Rodionova J.F.
1Sternberg State Astronomical Institute (MSU) 119899, 13, Universitetskiy prospect, Moscow, Russia,
2Moscow State University for Geodesy & Cartography (MIIGAiK), 105064, 4, Gorokhovskiy pereulok, Moscow, Russia, zhecka@inbox.ru.

Карта рельефа Венеры

Издана новая Карта рельефа Венеры в масштабе 1:45 000 000, составленная в ГАИШ МГУ при участии кафедры картографии и геоинформатики на основе данных КА 'Магеллан' о высотах более 6 000 000 точек поверхности.

КАРТА РЕЛЬЕФА ВЕНЕРЫ

Составление сравнительно-планетологического тематического атласа "Рельеф планет Земной группы и их спутников".

1 Географический факультет МГУ им. М.В.Ломоносова
2 Государственный астрономический институт им. П.К. Штернберга МГУ им. М.В.Ломоносова

Майкл Грегори Гордон

ESA SMART-1 MISSION TO THE MOON

B.H. Foing1, G. Michael1, G.R. Racca2, A. Marini2, M. Grande, J. Huovelin, J.-L. Josset, H.U. Keller, A. Nathues, D. Koschny, A. Malkki (SMART-1 Science and Technology Working Team)
1ESA Research and Scientific Support Dept., ESTEC/SCI-S
2ESA Science Projects Dept., ESTEC/SCI-PD Bernard.Foing@esa.int
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

SURVEY OF MARS CRATER TOPOGRAPHY FROM MOLA DATA.

Michael G. G., European Space Agency, Research and Scientific Support Department, ESA/ESTEC, Noordwijk, The Netherlands, greg.michael@esa.int
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

BEAGLE-2 LANDING SITE ATLAS.

Michael G. G.1, Chicarro A. F.1, Rodionova J. F.2, Shevchenko V. V.2, Iluhina J.2, Kozlova E. A.2
1European Space Agency, Research and Scientific Support Department, ESA/ESTEC, Noordwijk, The Netherlands
2Sternberg Astronomical Institute, Moscow, greg.michael@esa.int
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

THE MORPHOMETRIC ANALISYS OF THE FEATURES OF MARTIAN CRATERS.

I.A. Ushkin1, G. G. Michael2, E.A. Kozlova3 .
1. Moscow State University, Vorobjovy Gory, 119899, Moscow, Russia, gray_pigeon@mail.ru .
2. ESA, Noordwijk, the Netherlands. greg.michael@rssd.esa.int
3. Sternberg State Astronomical Institute, 119899, Moscow, Russia.
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

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.
Brown University - Vernadsky Institute Microsymposium 40, 2004, Moscow, Russia

COPRATES CHASMA NORTH WALL INTERIOR LAYERED DEPOSIT: LAYER MEASUREMENTS AND COMPARISON WITH JUVENTAE CHASMA ILDS USING MARS EXPRESS HIGH RESOLUTION STEREO CAMERA (HRSC) DERIVED TOPOGRAPHY

G. Michael 1, E. Hauber1, K. Gwinner1, R. Stesky2, F. Fueten3, D. Reiss1, H. Hoffmann1, R. Jaumann1, G. Neukum4, T. Zegers5, and the HRSC Co-Investigator Team
1Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany
2Pangaea Scientific, Brockville, Ontario, Canada
3Department of Earth Sciences, Brock University, St. Catharines, Ontario, Canada
4Remote Sensing of the Earth and Planets, Freie Universitaet, Berlin, Germany
5ESTEC, ESA, Noordwijk, The Netherlands
Brown University - Vernadsky Institute Microsymposium 42, October 10-12, 2005, Moscow, Russia

Пугачева С.Г.

Каталог названий рельефа поверхности Меркурия.

В каталоге приведены названия морфологических типов рельефа Меркурия на русском и латинском языках, даны координаты объектов в гермесографической системе координат, а также исторические и библиографические сведения о происхождении названий.

THE CHEMICAL COMPOSITION OF REGOLITH AT THE MOON'S SOUTH POLE, ACCORDING TO DATA OF LUNAR PROSPECTOR AND LUNAR RECONNAISSANCE ORBITER MISSIONS.

S. G. Pugacheva and V. V. Shevchenko, Sternberg State Astronomical Institute, Moscow University, 13 Universitetsky pr., 119992 Moscow, Russia, pugach@sai.msu.ru.

НОМЕНКЛАТУРНЫЙ РЯД НАЗВАНИЙ ЛУННОГО РЕЛЬЕФА

С. Г. Пугачева, Ж. Ф. Родионова, В. В. Шевченко, Т. П. Скобелева, К. И. Дехтярева, А. П. Попов.
Государственный Астрономический институт им. П.К. Штернберга, МГУ

Каталог лунной номенклатуры содержит список названий деталей лунного рельефа. Для обозначения форм рельефа поверхности Луны установлена единая система номенклатурных терминов, которые утверждены Генеральной ассамблеей Международного астрономического Союза (МАС).
В каталоге 'Номенклатурный ряд названий лунного рельефа' приведены 1933 названия деталей рельефа Луны на русском и латинском языках. Каталог построен на основе справочника именованных лунных объектов, утвержденного Международным Астрономическим Союзом (IAO/WGPSN). Список номенклатурного ряда названий расположен в интернете на сайте Геологической службы США (USGS) [http://planetarynames.wr.usgs.gov/].

Structure of the South Pole-Aitken Lunar Basin

V. V. Shevchenko, V. I. Chikmachev, and S. G. Pugacheva
Sternberg State Astronomical Institute, Lomonosov Moscow State University, Universitetskii pr. 13, Moscow, 119899 Russia
Received April 10, 2007

The hypsometric map and the basin height profiles, for the first time relying upon a spherical daturence surface, have been constructed based on the generalization of the heights measured within the hemisphere including the ring structure of the South Pole-Aitken basin. The distribution of the major chemical elements (Fe and Th), depending upon the structure height levels, has been obtained. The relationship between these lunar rock indicators and the height levels of the rock preferential distribution has been revealed. The outer basin ring has been distinguished and the ring structure of the central basin depression has been revealed against a combined hypsometric and geochemical background. A total basin diameter of about 3500 km has been reliably determined for the first time. A unique feature of the basin structure consists in that the arrangement of the basin inner rings does not show a central circular symmetry, which can indicate that a hypothetical impactor moved along the trajectory (or orbit) oriented almost normally to the ecliptic plane. In combination with the revealed very small depth-diameter ratio in the initial basin structure, this circumstance makes it possible to put forward the hypothesis that a comet impact produced the South Pole-Aitken basin.

THE PHOTOMETRIC RESEARCHS OF THE MERCURY'S SURFACE BY MEANS OF DIGITAL MODELS.

S.G. Pugacheva. Sternberg State Astronomical Institute, Moscow
University, 13 Universitetsky pr., 119992 Moscow, Russia, pugach@sai.msu.ru.

THE PARAMETERS INVOLVED IN HAPKE'S MODEL FOR ESTIMATION OF THE COMPOSITION OF THE EJECTA LUNAR TERRAINS.

S.G. Pugacheva, V.V.
Shevchenko. Sternberg State Astronomical Institute, Moscow University, 13 Universitetsky pr., 119992 Moscow, Russia, pugach@sai.msu.ru.
Brown University - Vernadsky Institute Microsymposium 42, October 10-12, 2005, Moscow, Russia

PHYSICAL AND MINERALOGY CHARACTERISTICS OF THE LUNAR REGOLITH IN THE AREAS OF THE THERMAL ANOMALIES.

S. G. Pugacheva, V.V. Shevchenko. Sternberg State Astronomical Institute, Moscow University, Russia, pugach@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

ANOMALIES OF THE MOON'S THERMAL EMISSION IN THE IR SPECTRAL RANGE (10.5 - 12.5 micron).

S. G. Pugacheva. Sternberg State Astronomical Institute, Moscow, 119899, Russia, pugach@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 34, October 8-9, 2001, Moscow, Russia

Имена астрономов в названиях лунных образований

С.Г. Пугачева, В.В. Шевченко, Государственный астрономический институт им. П.К.Штернберга,
Московский университет, Москва, Россия, 1999.

Приводятся статистические данные по выборке имен лунных кратеров, названных в честь выдающихся астрономов.

Тепловое излучение лунной поверхности в ИК диапазоне спектра (10-12 мкм)

С.Г.Пугачева, Государственный астрономический институт им. П.К. Штернберга, Москва, Россия, 1999.

В настоящей работе рассматриваются вопросы реализации метода калибровки трех ИК-снимков поверхности Луны, переданных из космоса первым российским геостационарным искусственным спутником Земли "ГОМС". Изображение Луны сканируется одновременно с изображением Земли для калибровки изображений как стационарный источник видимого и ИК-излучения. Спектральный диапазон снимков в ИК-области составляет 10.5-12.5 мкм, в видимой области - 0.4-0.7 мкм. Приведена фазовая функция радиационной температуры лунной поверхности и графики пространственной индикатрисы теплового излучения.

"Проекты и основные направления научных исследований".

Родионова Ж.Ф.

Морфологический каталог кратеров Луны.

Ж.Ф. Родионова, А.А.Карлов, Т.П. Скобелева и др. Под общей редакцией В.В.Шевченко.
М.: Изд-во МГУ, 1987.- 173 с.

Приведены координаты, диаметры и морфологические признаки 14 923 кратеров Луны, диаметром более 10 км. Морфологические признаки даны на основе анализа космических снимков и современных фотографических атласов.
Для широкого круга исследователей, занимающихся изучением поверхности Луны и сравнительной планетологией.

Morphological Analysis of the Cratering of the South Pole-Aitken Basin on the Moon

Zh. F. Rodionova and E. A. Kozlova
Государственный астрономический институт им. П.К.Штернберга, 1999.
Карты и глобусы Луны, созданные при участии отдела исследований Луны и планет

Приведено краткое описание картографирования Луны, выполненного при участии сотрудников ГАИШ под научным руководством Ю.Н.Липского.

Morphological Catalogue Of The Craters Of Mars.

A HIPSOMETRICAL FEATURES OF THE LUNAR SURFACE FROM THE CLEMENTINE MISSION.

J. F. Rodionova1, O. V. Elkina2, E. A. Kozlova1, V. V. Shevchenko1, P.V. Litvin2.
1. Sternberg State Astronomical Institute, 119899, Moscow, Russia; jeanna@sai.msu ru.
2. Moscow State University, Vorobjovy Gory, 119899, Moscow, Russia.
Brown University - Vernadsky Institute Microsymposium 34, October 8-9, 2001, Moscow, Russia

AN ANALYSIS OF THE DATA OF MARS ORBITER LASER ALTIMETER.

Rodionova J1., Iluhina J2., Michael G1,
1Sternberg State Astronomical Institute, jeanna@sai.msu.ru,
2Moscow University,
Brown University - Vernadsky Institute Microsymposium 34, October 8-9, 2001, Moscow, Russia

MARS: MOVEMENT OF GEOGRAPHICAL POLES AND DEFORMATION OF ITS SURFACE.

A.V. Dolitsky 1, J. F. Rodionova 2, R M. Kochetkov 3, A. F. Ainetdinova 2
1 - United Institute of Physics of the Earth of Russian Academy of Sciences .Moscow, ab4870@mail.sitek.ru
2 - Sternberg State Astronomical Institute, Moscow. jeanna@sai.msu.ru.
3 - Moscow Technical University of communication and information, krmkrm@rol.ru
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

SOME FEATURES OF THE CRATERING OF ISIDIS BASIN.

J.A.Iluhina, A.V.Lagutkina, J.F.Rodionova.
Sternberg State Astronomical Institute, Moscow University, jeanna@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

THE NEW DATA ON THE EARLY STAGE OF DEVELOPMENT OF THE EARTH, MARS, THE MOON AND MERCURY.

A.V.Dolitsky1, R.M.Kochetkov2, E.A. Kozlova3, J.F.Rodionova3,
1 - United Institute of Physics of the Earth RAS, Moscow, av13868@comtv.ru,
2 - Moscow Technical University of communication and information, Moscow, krmkrm@rol.ru.
3 - Sternberg State Astronomical Institute, Moscow, jeanna@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 40, 2004, Moscow, Russia

AUTOMATIC COMPILING OF HYPSOMETRIC MAP OF A PART OF THE VENUSIAN SURFACE.

E.N.Lasarev1, J. F. Rodionova 2,
1- Geographical faculty M.V. Lomonosov Moscow State University,
2- Sternbrg Sate Astronomical Institute, Universitetskij prospect 13, Moscow 119992, jeanna@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 40, 2004, Moscow, Russia

A TREATMENT OF DATA BANK OF MORPHOLOGIC CATALOGUE OF MERCURIAN CRATERS.

B. D. Sitnikov., E.A. Kozlova, J.F. Rodionova.
Sternberg State Astronomical Institute, Moscow, jeanna@sai.msu.ru.
Brown University - Vernadsky Institute Microsymposium 40, 2004, Moscow, Russia

История картографирования Луны

Ж.Ф.Родионова, Государственный астрономический институт им.П.К.Штернберга, 2009.

Hypsometric Globe of Mars - 3D Model of the Planet

Zh. F. Rodionova 1, J. A. Brekhovskikh2
1 Sternberg State Astronomical Institute Lomonosov Moscow University, Russia; marss8@mail.ru
2 Space Research Institute, Moscow, Russia; julia_br@iki.rssi.ru

Abstract. The new Hypsometric Globe of Mars is based on laser altimeter data of Mars Global Surveyor spacecraft. The diameter of the globe is 21 cm. Coordinates and the heights of 64 800 points on the surface of Mars were used for creating a 3-D Model of the surface of Mars.. A digital model of the relief was constructed with ArcGIS software. Contour lines were added together with hill-shading on the globe. The names of the main features - lands, plateaus, mountains, lowlands - plains and also some large craters are labeled. The places of landing sites of the spacecrafts are shown.

Новая карта спутников Марса

М.С. ШИБАНОВА, Е.Н. ЛАЗАРЕВ, кандидат технических наук
Ж.Ф. РОДИОНОВА, кандидат физико-математических наук
ГАИШ МГУ

КАРТОГРАФИРОВАНИЕ МАРСА.

Ж.Ф.РОДИОНОВА1, Ю.А.БРЕХОВСКИХ2, Е.Н.ЛАЗАРЕВ1,3, М.С. ЛАЗАРЕВА3, В.В.ШЕВЧЕНКО1

1- Государственный астрономический институт им. П.К.Штернберга МГУ им. М.В.Ломоносова
2- Институт космических исследований РАН
3 -Географический факультет МГУ им. М.В.Ломоносова

Научно-популярные обзоры:

Санович А.Н.

SOME PROBLEMS OF THE EVOLUTION OF ASTEROIDS – RUBBLE PILE.

G. A Leikin, A. N. Sanovich. Sternberg Astronomical Institute, Moscow 119899, Russia.
Brown University - Vernadsky Institute Microsymposium 34, October 8-9, 2001, Moscow, Russia

SOME PROBLEMS OF THE EVOLUTION OF ASTEROID – RUBBLE PILE

G. A. Leikin and A. N. Sanovich, Sternberg State Astronomical Institute, Moscow State University,
119992,Moscow,Universitetskij Prosp. 13, Russia , E-mail:san@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

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.
Sternberg State Astronomical Institute, Moscow, State University, 119992, Moscow, Universitetskij prosp. 13, Russia, E-mail: san@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 40, 2004, Moscow, Russia

A TIME ESTIMATE FOR CONSOLIDATION AND DISINTEGRATION OF AN ASTEROID – RUBBLE PILE.
THE SIMPLEST MODEL. A PRELIMINARY ANALYSIS.

G.A. Leikin, A.N. and Sanovich,
Sternberg, State Astronomical Institute Universitetsky Prosp. 13, Moscow 119992, Russia E-mail: san@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 42, October 10-12, 2005, Moscow, Russia

ASTEROIDAL DAMAGE TO THE EARTH: IMPLICATIONS BY ASTEROIDS - RUBBLE PILES.

G. A. Leikin and A. N. Sanovich,
Sternberg State Astronomical Institute, Universitetsky Prosp. 13, Moscow 119892, Russia, E-mail:san@sai.msu.ru

Феоктистова Е.А.

THE CRATERS SHOEMAKER AND FAUSTINI AS COLD TRAPS FOR VOLATILES

E. A. Kozlova1, V. V. Shevchenko1 . Sternberg State Astronomical Institute, 119899, Moscow, Russia
Brown University - Vernadsky Institute Microsymposium 40, 2004, Moscow, Russia

О ПРИРОДЕ АНОМАЛЬНЫХ ОБРАЗОВАНИЙ В ПОЛЯРНЫХ ОБЛАСТЯХ МЕРКУРИЯ И ЛУНЫ

Е.А.Козлова
Государственный астрономический институт им. П.К.Штернберга
Московского государственного университета им.М.В.Ломоносова, Россия
Поступила в редакцию 27.01.2004 г.
АСТРОНОМИЧЕСКИЙ ВЕСТНИК, 2004, том 38, ?5, с. 1-13

Properties of the impact-produced lunar exosphere during Perseid 2009 meteor shower

A.A. Berezhnoy (1), O.R. Baransky (2), K.I. Churyumov (2), V.V. Kleshchenok (2), E.A. Kozlova (1), V. Mangano (3), V.O. Ponomarenko (2), Yu.V. Pakhomov (4), V.V. Shevchenko (1), yu. I. Velikodsky (5)
(1) Sternberg Astronomical Institute, Universitetskij pr., 13, Moscow, 19991, Russia.
(2) Shevchenko National University, Kiev, Ukraine
(3) Institute Astrophysics and Planetology from Space, INAF, Rome, Italy
(4) Institute of Astronomy, Russian Academy of Science, Pyatnitskaya Street 48, Moscow, 119017 Russia
(5) Institute of Astronomy, Kharkiv National University, 35 Sumskaya Street

The Cold Traps Near the South Pole of the Moon

в сборнике 36th Annual Lunar and Planetary Science Conference, серия Lunar and Planetary Institute Science Conference Abstracts, том 36, с. 1061 тезисы

Origin and stability of lunar polar volatiles

в журнале Advances in Space Research, том 50, с. 1581-1712 DOI
издательство Pergamon Press Ltd. (United Kingdom)

Properties of the impact-produced lunar exosphere during Perseid 2009 meteor shower

Stability of Volatile Species at the Poles of the Moon

в сборнике Lunar and Planetary Institute Science Conference Abstracts, серия Lunar and Planetary Institute Science Conference Abstracts, том 43, с. 1396 тезисы

Чикмачев В.И.

Гигантский кратер на обратной стороне Луны

TO THE DISCOVERY OF THE "SOUTH POLE - AITKEN " BASIN.

V. I. Chikmachev and V.V. Shevchenko,
Sternberg State Astronomical Institute, Moscow University, Universitetsky 13, Moscow, 119899 , Russia,
MICROSYMPOSIUM 34, Topics in Comparative Planetology October 8-9, 2001, Moscow, Russia

Бассейн "Южный полюс - Эйткен" на первых снимках обратной стороны Луны

В.И.Чикмачев, В.В.Шевченко, Государственный астрономический институт имени П.К.Штернберга,
г. Москва, Россия, 1999.

Рассматривается история обнаружения гигантского бассейна в южной полярной области Луны, который по первым снимкам обратной стороны Луны был назван и утвержден МАС как "Море Мечты".

GENERALIZED TOPOGRAPHY OF THE LUNAR SOUTH POLE - AITKEN BASIN.

V.I.Chikmachev, S.G.Pugacheva and V.V.Shevchenko, Sternberg State Astronomical Institute, Moscow University, Moscow, chik@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 40, 2004, Moscow, Russia

AN ORIGIN FOR THE SOUTH POLE-AITKEN BASIN THORIUM. V.I.

Chikmachev, S.G.Pugacheva, Sternberg State Astronomical institute. Moscow University, Moscow. chik@sai.msu.ru.
Brown University - Vernadsky Institute Microsymposium 42, October 10-12, 2005, Moscow, Russia

Шевченко В.В.

Geophysical Research Abstracts Volumi 3, 2001

Взгляды мирового сообщества на проблему внеземных ресурсов

В.В.Шевченко, Государственный астрономический институт им. П.К.Штернберга, Московский университет, Москва, Россия, 1999.

Тезисы доклада на пленарном совместном заседании Комиссии Государственной Думы РФ по законодательному обеспечению проблем устойчивого развития и научного Экспертно-консультативного Совета при Комиссии по теме: О возможности применения ракетно-ядерного потенциала в интересах устойчивого развития России и мира , 28 июня 1999 года.

Юрий Наумович Липский

В.В.Шевченко, Ж.Ф.Родионова, Государственный астрономический институт им.П.К.Штернберга, 1999.

Приводятся биографические данные Ю.Н.Липского, результаты его научной деятельности и краткая история образования отдела исследований Луны и планет.

MERCURY: SURFACE LAYER STRUCTURE FROM OPTICAL PROPERTIES.

V.V.Shevchenko, Sternberg State Astronomical Institute, Moscow University, Universitetsky 13, Moscow 119899, Russia, shev@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 34, October 8-9, 2001, Moscow, Russia

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.
Brown University - Vernadsky Institute Microsymposium 34, October 8-9, 2001, Moscow, Russia

EVALUATING THE STRUCTURE OF THE SURFACE LAYER OF MERCURY.

V.V.Shevchenko, Sternberg State Astronomical Institute, Moscow University, Moscow 119992, Russia, shev@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

MERCURY: LOCAL VARIATIONS OF THE PHOTOMETRIC RELIEF.

REMOTE METHOD OF IDENTIFICATION OF THE EJECTA LUNAR TERRAINS AND THEIR COMPOSITION FITURES.

1 Sternberg State Astronomical Institute, Moscow University, 13 Universitetsky pr., 119992 Moscow, Russia;
2 UMR 5562/CNES/Observatory Midi-Pyrenees, Toulouse University, 14 avenue E. Belin, 31400 Toulouse, France. shev@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

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.
1UMR 5562 'Dynamique Terrestre et Planetaire'/CNRS/UPS, Observatoire Midi-Pyrenees, Toulouse, 31400 France;
2Sternberg Astronomical Institute, Moscow University, Moscow, 119992, Russia,
3Abastumany Astrophysical Observatory, Georgian Academy of Sciences, Georgia. shev@sai.msu.ru
Brown University - Vernadsky Institute Microsymposium 38, October 27-29, 2003, Moscow, Russia

Творческий путь в астрономии и космических исследованиях Ю.Н. Липского

В.В.Шевченко, Государственный астрономический институт им.П.К.Штернберга, 2009.

Новые результаты, полученные лунным спутником 'ЛРО', и участие в проекте сотрудников ГАИШ

В.В.Шевченко, Государственный астрономический институт им.П.К.Штернберга, 2009.

SPECTRAL FEATURES OF THE AVALANCHE DEPOSITS IN LUNAR CRATER REINER.

V.V.Shevchenko1,2, P.C.Pinet1, S.Chevrel1, Y.Daydou1, T.P.Skobeleva2, O.I.Kvaratskhelia3,
C.Rosemberg1. 1UMR 5562 'Dynamique Terrestre et Planetaire'/CNRS/UPS, Observatoire Midi-
Pyrenees, Toulouse, 31400 France; 2Sternberg Astronomical Institute, Moscow University, Moscow,
119992, Russia, 3Abastumany Astrophysical Observatory, Georgian Academy of Sciences, Georgia.
shev@sai.msu.ru

FEATURES OF THE HYDROGEN DISTRIBUTION AROUND LUNAR CRATERS PROCLUS

AND KEPLER. M.P. Sinitsin, V.V. Shevchenko, Sternberg Astronomical Institute, Moscow University,
Moscow, 119992, Russia shev@sai.msu.ru

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