Публикации сотрудников отдела.


Бережной А.А.

Impacts as sourcess of the exosphere on Mercury.

Alexey A. Berezhnoy a,b,c, 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.

Abstract
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.

IcarusCorrectedProof.pdf - 709 KB


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.

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

09_Berezhnoy_etal.pdf - 207 KB


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.

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

28_Hasebe_etal.pdf - 161 KB


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.

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

88_Yamashita et_al.pdf - 253 KB


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.

Abstract
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.

7305CorrectedProof.pdf - 218 KB


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.

Abstract
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.

NathazardsEarthSystSci2004.pdf - 448 KB


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.

Abstract
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.

PSS_1833.pdf - 1321 KB


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).

Abstract
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.

PASJ2449modified.pdf - 277 KB


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.

Abstract
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.

EarthMoonPlanets2002.pdf - 218 KB


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.

p. 179-181, ESTEC, Noordwijk, The Netherlands, 10-14 July 2000.

LP-Moon.pdf - 26KB


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

Berezhnoi A.A., Klumov B.A.

p. 175-178, ESTEC, Noordwijk, The Netherlands, 10-14 July 2000.

ILEWG4.pdf - 58 KB


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".

aref.doc - 50 КБ
aref.pdf - 157 КБ


Тепловой режим холодных ловушек на Луне.

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

Резюме
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.

RadioMoon.doc - 87 КБ
RadioMoon.pdf - 100 КБ


Лунный лед: можно ли определить его происхождение?

Бережной А.А., Клумов Б.А.

Письма в ЖЭТФ, Т. 68, N2, с. 150-154, 1998.

Эту статью можно найти на сервере журнала Письма в ЖЭТФ.


Столкновение кометы с Юпитером: определение глубины проникновения осколков по молекулярным спектрам.

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

Письма в ЖЭТФ, Т. 63, N6, с. 387-391, 1996.

Эту статью можно найти на сервере журнала Письма в ЖЭТФ.


Бусарев В.В.

Оценка состава вещества и обнаружение сублимационной активности астероидов 145 Адеоны, 704 Интерамнии, 779 Нины и 1474 Бейры.

Бусарев В.В., Барабанов С.И., Пузин В.Б.

Астрон. вестн., 2016, т. 50, №4, с. 300-312.

Спектрофотометрические наблюдения в диапазоне 0.35–0.92 мкм 145 Адеоны, 704 Интерамнии, 779 Нины и 1474 Бейры, астероидов близких примитивных типов, позволили нам обнаружить в их спектрах отражения похожие минералогические полосы поглощения с центрами у 0.38, 0.44 и 0.67– 0.71 мкм. На этих же астероидах мы впервые зарегистрировали спектральные признаки одновременной сублимационной активности (наличие максимумов в спектрах отражения у ~0.35–0.60 мкм у Адеоны, Интерамнии и Нины и вблизи ~0.55–0.75 мкм – у Бейры), которую мы связываем с их малыми гелиоцентрическими расстояниями и, соответственно, с высокой инсоляцией поверхности.

АВ-16-2.pdf - 586 КБ


Новые спектры отражения 40 астероидов: сравнение с предшествующими результатами и интерпретация.

Бусарев В.В.

Астрон. вестн., 2016, т. 50, №1, с. 15-26.

В статье представлены и обсуждаются избранные спектры отражения 40 астероидов Главного пояса, полученные автором в Крымской лаборатории ГАИШ МГУ в 2003–2009 гг. Целью работы является поиск новых спектральных особенностей астероидов, характеризующих состав их вещества. При сравнении полученных результатов с более ранними данными сделан вывод о значительных неоднородностях в распределении химико-минералогического состава поверхностного вещества у ряда малых планет (10 Гигии, 13 Эгерии, 14 Ирены, 21 Лютеции, 45 Евгении, 51 Немаузы, 55 Пандоры, 64 Ангелины, 69 Гесперии, 80 Сафо, 83 Беатрисы, 92 Ундины, 129 Антигоны, 135 Герты и 785 Зветаны), проявляющихся при разных фазах вращения.

AВ-16-1.pdf - 329 КБ


New reflectance spectra of 40 asteroids: A comparison with previous results and interpretation.

Busarev V.V.

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.

SSR_Busarev16.pdf - 386 KB


Spectrophotometry of (32) Pomona, (145) Adeona, (704) Interamnia, (779) Nina, (330825) 2008 ХЕ3, and 2012 QG42 and laboratory study of possible analog samples.

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.

Icarus(Busarev_etal15)_Printed.pdf - 2483 KB


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

В. В. Бусарев.

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

AB-15-1_Bus.pdf - 1576 KБ


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").

Chelyabinskiy_bolid.doc - 7496KБ


Докторская диссертация на тему:

"ИЗУЧЕНИЕ ПРИРОДЫ АСТЕРОИДОВ МЕТОДАМИ СПЕКТРОФОТОМЕТРИИ".

Бусарев В.В.

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

Abstract.pdf- 454 KБ


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

© 2011 г. В. В. Бусарев.

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

АВ-11(Бусарев).pdf - 220 KБ


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

В. В. Бусарев, © 2010 г.

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

АВ-10(Бусарев).pdf - 251 KБ


Астрофизические методы исследования Луны и малых небесных тел.

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

Astrofiz methods.pdf - 570 КБ


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.

V-B- 2008(Bus_etal).doc - 169 KB


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.

УФН-07(Бус-Прок-Боч).pdf - 293 KБ


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.

АВ-05(Прок-Боч-Бус).doc - 173 KБ


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

V V Busarev, V V Prokof'eva-Mikhailovskaya, V V Bochkov.

UFN2007(Bus_etal)(engl).PDF - 225 KB


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.

Abstract
—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.

SSR-05(Prok-Boch-Bus).pdf - 208 KB


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

Бусарев В. В., ГАИШ МГУ, E-mail: busarev@sai.msu.ru

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.

OZA2007(Busarev).pdf - 701 KБ


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.

Abstract.
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.

EM&P2003(Bus-Dor-Mak).pdf - 105 KB


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.

ACM08(Bus).pdf - 120 KB


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

m44_14_busarev_etal.pdf - 93 KB


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.

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

15_Busarev_etal.pdf - 276 KB


Where Some Asteroid Parent Bodies.

V.V.Busarev.

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

LPSC2004a.pdf - 79 KB


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.

ms063.pdf - 242 KB


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

V.V. Busarev

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.

MS058.pdf - 567 KB


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

V. V. Busarev

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

LPSC2001a.pdf - 56 KБ


Где могут быть скрыты  родительские тела астероидов?

Бусарев В.В.

Terskol.pdf - 365 KБ


Горячев М.В.

Экспериментальные исследования.
Изучение небесных тел при помощи телевидения.
Поляриметр "Таймыр".
ПЗС-камера "Вега-202"


Лазарев Е.Н.

ГИПСОМЕТРИЧЕСКАЯ КАРТА ВЕНЕРЫ: МЕТОДЫ СОЗДАНИЯ И ИСПОЛЬЗОВАНИЯ.

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

1_Гипсометрическая карта Венеры - методы создания и использования.pdf - 709 КБ


ГЕНЕРАЛИЗАЦИЯ ТОЧЕЧНЫХ МАССИВОВ ДАННЫХ ПОСРЕДСТВОМ ИСПОЛЬЗОВАНИЯ ДОПОЛНИТЕЛЬНЫХ ВОЗМОЖНОСТЕЙ ГЕОИНФОРМАЦИОННЫХ СИСТЕМ.

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

2_ГЕНЕРАЛИЗАЦИЯ ТОЧЕЧНЫХ МАССИВОВ ДАННЫХ ПОСРЕДСТВОМ ИСПОЛЬЗОВАНИЯ ДОПОЛНИТЕЛЬНЫХ ВОЗМОЖНОСТЕЙ ГЕОИНФОРМАЦИОННЫХ СИСТЕМ.pdf - 498 КБ


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 г.

Автореферат.pdf - 599 КБ


История картографирования Марса.

Лазарев Евгений Николаевич.

3_История картографирования Марса.pdf - 1598 КБ


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.

Abstract
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.

4_RASTER VENUS AND LUNAR MAPS AS A SOURCE FOR OBTAINING VECTOR TOPOGRAPHIC DATA.pdf - 1393 KB


THE LUNAR SUBPOLAR RELIEF MAP: THE WAYS AND TECHNIQUES OF COMPILING AND USINGю

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.ruю

5_THE LUNAR SUBPOLAR RELIEF MAP THE WAYS AND TECHNIQUES OF COM.pdf - 612 KB


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.ruю

6_Automatic creation of the hypsometric map of Venus.pdf - 116 KB


Гипсометрическая карта Венеры.

6_Automatic creation of the hypsometric map of Venus_MAP.pdf - 2928 КБ


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.

7_Automated creation of the lunar hypsometric map techniques of compiling.pdf - 325 KB


Карта рельефа Венеры.

Лазарев Е.Н., Родионова Ж.Ф., Шевченко В.В.

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.

Лазарев Е. Н., Родионова Ж. Ф., Шевченко В. В.

RELIEF MAP OF VENUS3.doc - 979 КБ


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

М.С.Лазарева1, Е.Н.Лазарев1,2, Ж.Ф. Родионова2.

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

lazareva_et_al_2013.pdf - 6724 КБ

 


Майкл Грегори Гордон

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.

m42_50.pdf - 102 KB


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.

81_Ushkin_Michael.pdf - 234 KB


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.

ms019.pdf - 130 KB


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.

ms067.pdf - 636 KB


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.

ms068.pdf - 138 KB


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.

ms090.pdf - 387 KB


Пугачева С.Г.

Каталог названий рельефа поверхности Меркурия.
 (Изд. 2-е, испр. и доп., 2016 г.)

С.Г. Пугачева, Ж.Ф. Родионова, Т.П. Скобелева, В.В. Шевченко.

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.


Каталог названий рельефа поверхности Меркурия.

Пугачева С.Г., Скобелева Т.П., Шевченко В.В.

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.

Pugacheva LPS 41.pdf - 208 KВ


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/].

Nomenclature of lunar names.doc - 2758 КБ
Nomenclature of lunar names.pdf - 2322 КБ


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

Abstract
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.

SSR447.pdf - 1612KB


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.

m44_70_pugacheva.pdf - 204KB


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

m42_60.pdf - 43KB


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

ms080.pdf - 533KB


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

MS058.pdf - 567KB


Имена астрономов в названиях лунных образований

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

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

nomen.doc - 187 КБ
nomen.pdf - 117 КБ


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

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

Резюме
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.

ir_luna.doc - 458 КБ
ir_luna.pdf - 351 КБ


"Проекты и основные направления научных исследований".

С.Г.Пугачева


Родионова Ж.Ф.

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

rodionova_et_al_2013.pdf - 4733 КБ


Новая карта спутников Марса.

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

ГАИШ МГУ

Zeml_Vsel_6_Shubanova_ 3-18---1.pdf - 1833 КБ


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.

Rodionova ICC2013.pdf - 234 КB


История картографирования Луны.

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

Mapping the history of the moon.pdf - 8186 КБ


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

78_Sitnikov_etal.pdf - 852 КB


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

56_Lasarev_Radionova.pdf - 230 КB


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

21_Dolitsky_etal.pdf - 683 КB


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

ms035.pdf - 2609 КB


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

ms015.pdf - 202 КB


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

MS060.pdf - 166 КB


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

MS059.pdf - 575 KB


Morphological Catalogue Of The Craters Of Mars.

J. F. Rodionova, K. I. Dekchtyareva, A. A. Khramchikhin, G. G. Michael, S. V. Ajukov, S. G. Pugacheva, V. V. Shevchenko.
Editors: V.V. Shevchenko, A.F. Chicarro. 2000.


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.

maps_r.doc - 697 КБ

maps_r.pdf - 398 КБ


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.


Научно-популярные обзоры

Меркурий

Карты Меркурия

Венера

Карты Венеры

Луна

Легко ли достать Луну с неба?

Карты Луны

Марс

Карты Марса

Юпитер

Сатурн

Уран

Нептун

Плутон


Санович А.Н.

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

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

m44_56_leikin_sanovich.pdf - 73 KB


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

G.A. Leikin, A.N. 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.

m42_46.pdf - 10 KB


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.

58_Leikin_Sanovich.pdf - 76 KB


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.

ms059.pdf - 155 KB


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.

MS047.pdf - 68 KB


Феоктистова Е.А.

Origin and stability of lunar polar volatiles

Berezhnoy A.A., Kozlova E.A., Sinitsyn M.P., Shangaraev A.A., Shevchenko V.V.

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

ASR Origin and Stability.pdf - 395 KB


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

EPSC abstract
Vol. 7 EPSC2012-52 2012
European Planetary Congress 2012

EPSC2012-52.pdf - 125 KB


Stability of Volatile Species at the Poles of the Moon

Berezhnoy A.A., Kozlova E.A., Shevchenko V.V.

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

LPSC 2012 1396.pdf - 215 KB


The Cold Traps Near the South Pole of the Moon

Berezhnoy A.A., Kozlova E.A., Shevchenko V.V.

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

Houston2005(1).pdf - 143 KB


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

50_Kozlova_Shevchenko.pdf - 212KB


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

AstVest5_04KozlovaLO.pdf - 851КБ


Чикмачев В.И.

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.

m42_12.pdf - 442 KB


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.

17_Chikmachev_etal.pdf - 356 KB


Гигантский кратер на обратной стороне Луны.

В.И.Чикмачев.

ЗВЕЗДОЧЕТ №2 2002, с.14-15.


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.

MS015.pdf - 398 KB


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.

Резюме
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".

basin.doc - 262 КБ
basin.pdf - 344 КБ


Шевченко В.В.

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

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

Lipskiy_100.pdf - 3265 КБ


Новые результаты, полученные лунным спутником «ЛРО», и участие в проекте сотрудников ГАИШ.

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

New results.pdf - 1781 КБ


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.

ms082.pdf - 338 KB


MERCURY: LOCAL VARIATIONS OF THE PHOTOMETRIC RELIEF.

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.

ms083.pdf - 346 KB


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.

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.

ms084.pdf - 315 KB


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.

ms085.pdf - 280 KB


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.

MS064.pdf - 78 KB


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.

MS065.pdf - 316 KB


VARIABLE RADIO EMISSION OF THE MOON AT 25 MM DURING THE LEONID 2000 METEOR SHOWER.

A.A. Berezhnoi (1), E. Bervalds (2), O.B. Khavroshkin (3), G. Ozolins (2), V.V. Shevchenko (1), V.V. Tsyplakov (3)
(1) SAI, Moscow, Russia; (2) VIRAC, Riga, Latvia; (3) UIEP, Moscow, Russia
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.

Berezhnoi, A.A. (1), Klumov B.A.(2), Shevchenko V.V.(1)
(1) Sternberg Astronomical Institute, Moscow, Russia, (2) Institute of Dynamics of Geospheres, Moscow, Russia
Geophysical Research Abstracts Volumi 3, 2001.

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).

S.G. Pugacheva and V.V. Shevchenko
Sternberg State Astronomical Institute, Universitetskiy pr.13, Moscow, 119899, Russia pugach@sai.msu.ru Fax: 007-095-932-88-41
Geophysical Research Abstracts Volumi 3, 2001.

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".

J.Rodionova and E.Kozlova Sternberg State Astronomical Institute
Geophysical Research Abstracts Volumi 3, 2001.

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.

V.V.Shevchenko
Sternberg State Astronomical Institute, Moscow University, Moscow, Russia shev@sai.msu.ru
Geophysical Research Abstracts Volumi 3, 2001.

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..


Взгляды мирового сообщества на проблему внеземных ресурсов.

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

Резюме
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.

resource.doc - 56 КБ
resource.pdf - 113 КБ


Юрий Наумович Липский.

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

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

lipsk-j.doc - 257 КБ
lipsk-j.pdf - 572 КБ


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.

m44_75_shevchenko_etal.pdf - 188 KB


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.

m44_76_sinitsin_shevchenko.pdf - 164 KB


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