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.
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.
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.
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
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
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
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
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.
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.
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
Berezhnoi A.A., Klumov B.A.
p. 175-178, ESTEC, Noordwijk, The Netherlands, 10-14 July 2000
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.
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
Busarev V. V.
Solar System Research, 2014, v. 48, No. 1, p. 48-61
Abstract
The results of ground-based spectrophotometry of the icy Galilean satellites of
Jupiter — Europa, Ganymede, and Callisto — are discussed. The observations
were carried out in the 0.39–0.92 μm range with the use of the CCD spectrometer
mounted on the 1.25-m telescope of the Crimean laboratory of the Sternberg
Astronomical Institute in March 2004. It is noted that the calculated
reflectance spectra of the satellites mainly agree with the analogous data of
the earlier ground_based observations and investigations in the Voyager and
Galileo space missions. The present study was aimed at identifying new weak
absorption bands (with the relative intensity of ~3–5%) in the reflectance
spectra of these bodies with laboratory measurements (Landau et al., 1962;
Ramaprasad et al., 1978; Burns, 1993; Busarev et al., 2008). It has been
ascertained that the spectra of all of the considered objects contain weak
absorption bands of molecular oxygen adsorbed into water ice, which is
apparently caused by the radiative implantation of O+ ions into the surface
material of the satellites in the magnetosphere of Jupiter. At the same time,
spectral features of iron of different valence (Fe2+ and Fe3+) values typical of
hydrated silicates were detected on Ganymede and Callisto, while probable
indications of methane of presumably endogenous origin, adsorbed into water ice,
were found on Europa. The reflectance spectra of the icy Galilean satellites
were compared to the reflectance spectra of the asteroids 51 Nemausa (C-class)
and 92 Undina (X-class).
V. V. Busarev
Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119992
Russia
Received December 21, 2009
V. V. Busarev
Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119992 Russia
Received December 21, 2009
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 V Busarev, V V Prokof'eva-Mikhailovskaya, V V Bochkov
V.V.Busarev
35th Lunar and Planetary Science Conference, 2004, Houston, Texas, Abstract
1026.
V. V. Busarev1, M. N. Taran2, V. I. Fel’dman3 and V. S. Rusakov41 Lunar and
Planetary Department, Sternberg State Astronomical Institute, Moscow State
University, 119992 Moscow, Universitetskij pr., 13, Russian Federation (RF);
e-mail: busarev@sai.msu.ru; 2 Department of Spectroscopic Methods, Institute of
Geochemistry, Mineralogy and Ore Formation, Academy of Sciences of Ukraine,
03142 Kiev, Palladina pr., 34, Ukraine; 3 Division of Petrology, Geological
Department of Moscow State University, 119992 Moscow, RF; 4 Division of
Mossbauer Spectroscopy, Physical Department of Moscow State University, 119992
Moscow, RF.
Brown University - Vernadsky Institute Microsymposium 40,
2004, Moscow, Russia
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.
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
V.V. Busarev, Sternberg Astronomical Institute (SAI), Moscow University,
Universitetskij pr., 13, Moscow, 119992
Russia, busarev@sai.msu.ru.
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.
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
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
V. V. Busarev
32nd Lunar and Planetary Science Conference, March 12-16, 2001, Houston, Texas,
Abstract 1927.
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
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
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
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
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
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)
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
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
E. A. Kozlova1, V. V. Shevchenko1 . Sternberg State Astronomical Institute,
119899, Moscow, Russia
Brown University - Vernadsky Institute Microsymposium 40,
2004, Moscow, Russia
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.
Automated creation of the lunar hypsometric map techniques of compiling.pdf
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.
RASTER VENUS AND LUNAR MAPS AS A SOURCE FOR OBTAINING VECTOR TOPOGRAPHIC DATA.pdf
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
THE LUNAR SUBPOLAR RELIEF MAP THE WAYS AND TECHNIQUES OF COM.pdf
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.
Automatic creation of the hypsometric map of Venus.pdf
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
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
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
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
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
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
Rodionova Zh.F.1, Shevchenko V.V.1, Grishakina E.A.2, Slyuta E.N.2
1 - Sternberg Astronomical Institute, Moscow State University (SAI MSU)
2 - Vernadsky Institute of Geochemistry and Analytical Chemistry RAS (GEOKHI RAS)
Abstract. Our knowledge of lunar topography has significantly improved over the last two decades owing to laser altimetry and images from orbiting spacecraft. Lunar terrain is detailed in the Survey Map of the Moon, which has a scale of 1:13 000 000. The map is based on the digital terrain model built using the data from the laser altimeter installed on the US spacecraft Lunar Reconnaissance Orbiter (LRO) with the resolution of 64 pixels per degree (0.5 km per pixel). In addition to the terrain relief shaded using the wash-drawing technique, the map provides Latin names of major lunar terrain features adopted by the International Astronomical Union (IAU), and their names in Russian. There are symbols on the map, which indicate the landing sites of all the spacecraft and manned space vehicles. The paper describes the major results of lunar surface studies conducted on the basis of data from orbital spacecraft and lunar landers.
29-44.pdf (in Russian)
I.Karachevtseva a, A. Kokhanov a, J. Rodionova a,b, A. Konopikhin a, A. Zubarev a,
I. Nadezhdina a, L. Mitrokhina a, V. Patratiy a, J. Oberst a,c,d
a-Moscow State University of Geodesy and Cartography (MIIGAiK), MIIGAiK Extraterrestrial Laboratory(MExLab),
Gorokhovsky per., 4, 105064, Moscow, Russia.
b-Sternberg Astronomical Institute Moscow State University, University pr., 13,119992, Moscow, Russia.
c-German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany.
d-Technical University Berlin, Institute for Geodesy and Geoinformation Sciences, Berlin, Germany.
Planetary and Space Science 2015, 108, pp. 24-30
Abstract. A new Phobos Atlas has been prepared, which includes a variety of thematic maps at various projections and scales, emphasizing dynamic topography, surface multispectral properties, geomorphology, as well as grooves-and crater statistics. The atlas benefits from innovative mapping techniques and recent results from Mars Express image processing: new derived control point networks, shape models and gravity field working models. A structure of the atlas is presented and some examples of the maps are shown. The Phobos Atlas can be useful for the future mission planning to the Martian satellite.
3863_PSS_Phobos Atlas_Final.pdf
Renato Dicati¹, Zhanna Rodionova²
1-USFI (Unione Stampa Filatelica Italiana) Milan, Italy, e-mail:
renato.dicati@gmail.com
2-Sternberg State Astronomical Institute 119992 Universitetskiy pr.13 e-mail:
marss8@mail.ru
THE NINTH MOSCOW SOLAR SYSTEM SYMPOSIUM 2018 MS-PS-84
Abstract. Although the spatial philately was born after the launch of the first artificial satellite, Sputnik 1, the first its stamps is included in a set dedicated to Soviet Union scientists, issued in August 15, 1951, that depicts Konstantin Tsiolkovsky, the father of astronautics and the first image of a cosmic rocket. A few days after the launch of Sputnik, on October 7, 1957, two stamps were issued: the first belonging to the set dedicated to the International Geophysical Year, contains the text ‘research with rockets’ and an image in which a rocket is drawn on the background of a starry sky. The second stamp, dedicated to the birth’s centenary of Tsiolkovsky, shows the portrait of the scientist and, in the background, a rocket and the planet Saturn. On this stamp November 28, 1957, a black overprint was imprinted with the words “4 October 1957 the first Earth’s artificial satellite”. This was the first real astrophilatelitic issue. There are tables with the names of lunar spacecrafts and images of stamps devoted them in the poster.
Dicati _Rodionova_Abstract _9MS3.pdf
A.A. Kokhanova,*, I.P. Karachevtsevaa, A.E. Zubareva, V. Patratya,
Zh.F. Rodionovab, J. Oberstc,d
a MIIGAiK Extraterrestrial Laboratory (MExLab), Moscow State University of Geodesy and Cartography (MIIGAiK), Moscow, Russia
b Sternberg State Astronomical Institute Lomonosov Moscow University, Moscow, Russia
c Technical University of Berlin, Berlin, Germany
d German Aerospace Center (DLR), Berlin, Germany
Planetary and Space Science 162 (2018) 179-189
Abstract. We apply cartographic methods on remote sensing data obtained by Lunar Reconnaissance Orbiter (LRO) and Kaguya (SELENE) to characterize potential landing sites for the “Luna-25” mission, previously selected. To identify presumable hazards (steep slopes, high ruggedness, cratered terrain) we developed special algorithms and GIS-tools. Sets of hazard maps for 3 high-priority potential landing sites were created.
Mapping-of-landing-sites_final.pdf
I.P. Karachevtsevaa, A.A. Kokhanova, J.F. Rodionovaa,b,
A.Yu. Zharkovaa,, M.S. Lazarevaa
a-Moscow State University of Geodesy and Cartography (MIIGAiK), MIIGAiK Extraterrestrial laboratory (MExLab),
105064. Gorokhovsky per., Moscow, Russia, i_karachevtseva@miigaik.ru
b-Sternberg State Astronomical Institute, 1198993, Moscow, Russia
Commission IV, WG IV/8
Abstract. New estimation of fundamental geodetic parameters and global and local topography of planets and satellites provide basic coordinate systems for mapping as well as opportunities for studies of processes on their surfaces. The main targets of our study are Europa, Ganymede, Calisto and Io (satellites of Jupiter), Enceladus (a satellite of Saturn), terrestrial planetary bodies, including Mercury, the Moon and Phobos, one of the Martian satellites. In particular, based on new global shape models derived from three-dimensional control point networks and processing of high-resolution stereo images, we have carried out studies of topography and morphology. As a visual representation of the results, various planetary maps with different scale and thematic direction were created. For example, for Phobos we have produced a new atlas with 43 maps, as well as various wall maps (different from the maps in the atlas by their format and design): basemap, topography and geomorphological maps. In addition, we compiled geomorphologic maps of Ganymede on local level, and a global hypsometric Enceladus map. Mercury’s topography was represented as a hypsometric globe for the first time. Mapping of the Moon was carried out using new images with super resolution (0.5-1 m/pixel) for activity regions of the first Soviet planetary rovers (Lunokhod-1 and -2). New results of planetary mapping have been demonstrated to the scientific community at planetary map exhibitions (Planetary Maps Exhibitions, 2015), organized by MExLab team in frame of the International Map Year, which is celebrated in 2015-2016. Cartographic products have multipurpose applications: for example, the Mercury globe is popular for teaching and public outreach, the maps like those for the Moon and Phobos provide cartographic support for Solar system exploration.
isprs-archives-XLI-B4-411-2016.pdf
I.P. Karachevtseva¹, A. A. Kokhanov¹ and Zh. Rodionova²
1-Moscow State University of Geodesy and Cartography
2-Sternberg Astronomical Institute of Lomonosov Moscow University
In the book Planetary Cartography and GIS. ed. Henrik Hargitai,Springer Nature Switzerland AG 2019, pp 235-251
Abstract. We present a general procedure of the Phobos Atlas creation. Main principles of mapping, mathematical, and geographical basics are described and justified. Data sources for mapping are listed. Approaches in the development of legends and design are considered, and some examples of the maps are shown.
P. Karachevtseva¹, A. A. Kokhanov¹, N. A. Kozlova¹ and Zh. F. Rodionova²
1-Moscow State University of Geodesy and Cartography
2-Sternberg Astronomical Institute of Lomonosov Moscow University
In the book Planetary Cartography and GIS. ed. Henrik Hargitai,Springer Nature Switzerland AG 2019, pp 263-278
Abstract. Soviet missions Luna-17 (1971) and Luna-21 (1973) deployed the roving robotic vehicles Lunokhod-1 and Lunokhod-2 on the lunar surface. The Lunokhods (Moonwalkers) were the first extraterrestrial rovers that were operated remotely from Earth. Using Lunar Reconnaissance Orbiter (LRO) narrowangle camera (NAC) (Robinson et al. 2010), the Lunokhods’ routes have been reconstructed (Karachevtseva et al. 2013; 2017). Following the rover tracks that are visible on high-resolution LROC NAC images, we identified the exact rover traverses and compared them with data from archive topographic maps created during Soviet lunar missions. Derived LRO data (DEMs and orthomosaics) allowed us to analyze the topography of the Moon area at the local level and to map the Lunokhods’ routes with more details.
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.
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
E.N. Lasarev 1, 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.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
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
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
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
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
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.
Zh. F. Rodionova and E. A. Kozlova
J.F. Rodionova, A.A. Karlov, T.P.Skobeleva, E.V. Konotopskaya, V.V. Shevchenko, K.E. Kozubskiy, K.I.Dekhtyareva, T.F. Smolyakova, L.I. Tishik, E.A. Fedorova
Coordinates, diameters and morphological features of 14 923 craters of the Moon in diameters 10 km and more are available in the catalogue.
S. G. Pugacheva and V. V. Shevchenko, Sternberg State Astronomical Institute, Moscow University, 13 Universitetsky pr., 119992 Moscow, Russia, pugach@sai.msu.ru.
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.
S.G. Pugacheva. Sternberg State Astronomical Institute, Moscow
University, 13 Universitetsky pr., 119992 Moscow, Russia,
pugach@sai.msu.ru.
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
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
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
G. A Leikin, A. N. Sanovich. Sternberg Astronomical Institute, Moscow 119899, Russia.
Brown University - Vernadsky Institute Microsymposium 34,
October 8-9, 2001, Moscow, Russia
G. A
Leikin, A. N. Sanovich. Sternberg Astronomical Institute, Moscow 119899, Russia.
Brown University - Vernadsky Institute Microsymposium 34,
October 8-9, 2001, Moscow, Russia
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
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
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
G. A. Leikin and A. N. Sanovich,
Sternberg State Astronomical Institute, Universitetsky Prosp. 13, Moscow 119892,
Russia, E-mail:san@sai.msu.ru
Rodionova Zh.F.1, Shevchenko V.V.1, Grishakina E.A.2, Slyuta E.N.2
1 - Sternberg Astronomical Institute, Moscow State University (SAI MSU)
2 - Vernadsky Institute of Geochemistry and Analytical Chemistry RAS (GEOKHI RAS)
Abstract. Our knowledge of lunar topography has significantly improved over the last two decades owing to laser altimetry and images from orbiting spacecraft. Lunar terrain is detailed in the Survey Map of the Moon, which has a scale of 1:13 000 000. The map is based on the digital terrain model built using the data from the laser altimeter installed on the US spacecraft Lunar Reconnaissance Orbiter (LRO) with the resolution of 64 pixels per degree (0.5 km per pixel). In addition to the terrain relief shaded using the wash-drawing technique, the map provides Latin names of major lunar terrain features adopted by the International Astronomical Union (IAU), and their names in Russian. There are symbols on the map, which indicate the landing sites of all the spacecraft and manned space vehicles. The paper describes the major results of lunar surface studies conducted on the basis of data from orbital spacecraft and lunar landers.
29-44.pdf (in Russian)
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
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
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
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
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
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
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
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
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.
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.
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.
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.
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..
A.A. Berezhnoi, Sternberg Astronomical Institute, Moscow, Russia
Resume. If the regoliths mean temperature at 1-2 cm depth is the same as the surface one, the cold-trap H2O, SO2, CO2 ices are stable. If the regolith in the upper 1-2 cm layer does not contain water ice then the mean temperature at 20-30 cm depths is 50-60 K higher than on the surface and SO2, CO2 ices are unstable in these conditions. Our results can be checked during the observations of the thermal emission of polar lunar regolith at 0.1 mm - 10 cm. If the mean radio temperature of the polar regolith does not increase with increasing wavelength, this fact can be considered indirect evidence for the existence of water ice on the Moon.
James D. Burke,
Jet Propulsion Laboratory, California Institute of Technology
Resume. This paper summarizes the starting phase of American robotic lunar programs. It includes comments on the then-prevailing political situation within the United States, and it also touches on the effects of competition between the US and the USSR in the immediate aftermath of Sputnik. It is appropriate now to look back at those times, especially as some of the relevant data in both countries, previously secret, have now been declassified and released for public use. Though the early lunar missions yielded only limited scientific information, they did set both nations' programs on a path toward later great advances in our understanding of the Moon.
V.I. Chikmachev and V.V. Shevchenko,
Sternberg State Astronomical Institute, Universitetskii pr. 13, Moscow, Russia
Resume. The history of discovery of the giant basin in the southern region of the Moon named on the first images of the lunar far-side Mare Ingenii by IAU Task Group for Lunar Nomenclature (IAU General Assemblu, Berkley, USA,1961) is given.
V.Gromov,
VNIITRANSMASH, St. Petersburg, Russia
Resume. The purpose of this paper is to systematise and review the series of investigation concerning the physical and mechanical properties of the soil on the Moon. The results of these investigations permit a deeper understanding of the soil-forming processes of the uppermost layers on the Moon and on the other planets. They are also needed to clarify general trends and to provide basic data and engineering models in order to develop new techniques for planetary exploration. This seems to be of vital importance nowadays, because we are on the eve of a new stage in the development of missions to the Moon and the investigation of other planets.
Peter Eckart, Assistant Professor,
Division of Astronautics, Technische Universität München, 85747 Garching, Germany
Alexander Gusev, Natasha Petrova, Naufal Rizvanov,
Kazan state university & Engelgrdt's astronomical observatory, Dpt. of Astron. & Gravit., Russia.
Philip R. Harris, Ph.D., Management/Space Psychologist & Author,
HARRIS INTERNATIONAL, LTD., LaJolla, California 92037, U.S.A.
Millennium Challenges.doc
Millennium Challenges.pdf
G.G.Kochemasov,
IGEM of the Russian Academy of Sciences, Moscow, Russia
Resume. Summary: The pioneering works of Yu. N. Lipskiy and Zh. F. Rodionova on regularities in lunar tectonics (1972-1975) were later used in developing a general planetary wave tectonics conception. It shows a regular character of tectonic dichotomy, sectoring, granularity of celestial bodies, including stars. It connects widespread variability of stellar atmospheres with their wave induced structures.
H.H.Koelle,
Aerospace Institute Technical University Berlin, Germany
Resume. Spaceflight can be considered as a natural, an essential and a logical step of the evolution of the human species. Exploring space, learning to live and work in space, and using its natural resources, will improve the quality of life on Earth and last-not-least enhance the survival chances of our civilization!
P.C.Pinet1, V.V.Shevchenko2, S.Chevrel1,
Y.Daydou1, T.P.Skobeleva2, O.I.Kvaratskhelia3,
C.Rosemberg1,
1UMR 5562 "Dynamique Terrestre et Planetaire"/CNRS/UPS, Observatoire Midi-Pyrenees, 14 Av.E.Belin, Toulouse, 31400 France; 2Sternberg Astronomical Institute, Moscow University, Moscow, 119899, Russia, 3Abastumany Astrophysical Observatory, Georgian Academy of Sciences, Georgia
Resume. A detailed remote sensing survey of ten lunar regions of mare and highland types has been carried out by means of Clementine spectro-imaging data with the purpose of establishing the regional distribution of the maturity state and weight percent of iron content in the lunar soils. The data are used to obtain a scale of conformity between spectral index of maturity r, spectropolarization index, and maturity index Is/FeO.
S.G. Pugacheva,
Sternberg State Astronomical Institute, Moscow, Russia
Resume. In the present paper, the implementation of the method for calibrating IR images is considered by example of calibrating three IR lunar-surface images transmitted by the first Russian geostationary meteorological satellite (GOMS). The Moon's image, scanned simultaneously with the Earth's image, is used for image calibrating as a steady-state source of visible and IR radiation. The photographs were obtained in IR (10.5-12.5 mkm) and visible (0.4-0.7 mkm) spectral ranges. The formulas of the analytical model of the Moon's thermal emission and drawings of the thermal indicatrix in the vector form are presented.
S.G.Pugacheva, V.V.Shevchenko,
Sternberg State Astronomical Institute, Moscow University, Moscow, Russia
Resume. The results of the statistic selection of the lunar craters, which were called by names of the famous astronomers, are presented.
N.G.Rizvanov, L.I.Rakhimov,
Engelhardt Astronomical Observatory, Kazan, Russia
Resume. The brief history of development of heliometric and positional observations of the Moon in Kazan university and Engelhardt Astronomical Observatory from the end of the last century till now days is given. All aspects of research of a figure, rotation and gravitational field of the Moon are considered as well as other close to them questions.
J.F.Rodionova,
Sternberg State Astronomical Institute Moscow University, Moscow, Russia
Resume. A brief description of the mapping of the Moon carried out with the participation of the scientific workers of SAI and with the guidance of Y.N.Lipsky is taken.
V.V.Shevchenko,
Sternberg State Astronomical Institute, Moscow University, Moscow, Russia
Resume. The nature of diffuse albedo anomalies on the lunar
surface that look like swirls is one of most interesting mystery in current
lunar studies. There are two main classes of hypothesises of the swirl origin:
formation of the swirls in the regions antipodal to large impact basins (1), and
formation of the swirls in result of cometary impacts (2).
A.G.Sizentsev1, V.V.Shevchenko2, V.F.Semenov3, G.M.Baidal1,
1Korolev Energia Rocket and Space Corparation, Korolev, Russia,
2Sternberg State Astronomical Institute, Moscow University, Moscow, Russia,
3Keldysh Research Center, Moscow, Russia
Resume. The discussed concept presents a phase in the industrial development of the base, when it becomes capable of building first experimental space power stations using solar energy to supply power to Earth. At that phase the permanent lunar base turns into a settlement with a population of up to 200.
B.I. Sotnikov, G.M.Baidal, G.A. Sizentsev,
S.P.Korolev, RSC Energia
Philip J. Stooke,
Department of Geography, University of Western Ontario, London, Ontario, Canada N6A 5C2
Resume. The exploration of the Moon by spacecraft began in 1959 with the impact of Luna 2 and the first photography of the far side by Luna 3. On the fortieth anniversary of these pioneering flights it is appropriate to look back at the history of lunar exploration. What dreams were fulfilled, and what others never came to fruition? I propose the creation of an International Atlas of Lunar Exploration to tell this story in cartographic form. It would provide a detailed record of the subject, capable of serving as a foundation for future scholarship in the planetary sciences and in the history of space exploration.
G.G. Kochemasov, IGEM of the Russian Academy of Sciences, Moscow, Russia
Philip J. Stooke, Department of Geography, University of Western Ontario.