Бережной Алексей Андреевич |
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Бережной Алексей Андреевич |
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Родился 15 апреля 1972 года в городе Воронеже. В 1988/89 учебном году учился в ФМШ-18 г. Москвы. С 1989 по 1995 год учился на химическом факультете МГУ им. М.В. Ломоносова, закончил кафедру физической химии. В 1995 году поступил в аспирантуру ГАИШ МГУ (отдел исследований Луны и планет). В 1999 г. закончил аспирантуру, защитив кандидатскую диссертацию "Физико-химические процессы при столкновениях комет с телами Солнечной системы".
Научные интересы связаны с исследованием проблемы химической эволюции тел Солнечной системы. В частности, химическая модификация небесных тел происходит при их столкновениях друг с другом. Особое внимание уделяю проблеме столкновения комет с планетами и их спутниками (наиболее впечатляющий пример - столкновение кометы Шумейкеров-Леви 9 с Юпитером). Занимаюсь исследованием происхождения летучих соединений в полярных областях Луны.
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.
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.
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 - 87KB.
RadioMoon.pdf - 100KB.
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 KB
aref.pdf - 157 KB.
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
Berezhnoi A.A., Klumov B.A.
p. 175-178, ESTEC, Noordwijk, The Netherlands, 10-14 July 2000
ILEWG4.pdf - 58KB
You can see fist two articles on JETP Letters Online.
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 - 207KB
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 - 161KB
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 - 253KB
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 - 218KB
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 - 218KB
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 - 448KB
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 - 1321KB
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
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 - 709KB
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 - 277KB
Увлечения-природа, фотография, книги.
Играю в футбол и настольный теннис.
Занимаюсь исследованием истории Черноземья в 17 - 19 веках.
В выходные дни часто совершаю вылазки на природу.
Больше всего нравятся холмистые равнины в лесостепи, в горах - диапазон высот
1-2.5 км (Крым, Карпаты).
Занимаюсь
художественной фотографией ( фотоохота
за птицами, млекопитающимися, насекомыми; пейзажная и архитектурная съемка).
Поставьте оценку моей страничке на сайте Astro Top 100 - Народный рейтинг!
Astrophysical Data Service http://adsabs.harvard.edu/abstract_service.html
Lunar Prospector Home Page http://lunar.arc.nasa.gov
ФК Факел http://ic.vrn.ru/~andr
International Meteor Organisation http://www.imo.net
Astronomical Meetings http://cadcwww.dao.nrc.ca/meetings/meetings.html
Путеводитель астронома по Интернету http://www.chat.ru/~samod/astro.htm
European Space Agency, Solar System Divison http://solarsystem.estec.esa.nl/
Всероссийское генеалогическое древо http://www.people.adicom.ru/people.htm
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