Vladimir V. Busarev

Scientific interests:

- spectrophotometry of the main belt asteroids and near-Earth asteroids, Centaurs, and Kuiper belt objects;

- hydrated asteroids of M-, S-, and E- types, and possible analogs of their matter, the terrestrial hydrosilicates and carbonaceous chondrites;

Publications:

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.

Where Some Asteroid Parent Bodies

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

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

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

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. 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

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

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.

HYDRATED SILICATES ON EDGEWORTH-KUIPER OBJECTS – PROBABLEWAYS OF FORMATION

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

Visible-range absorption bands at 600–750 nm were recently detected on two Edgeworth-Kuiper Belt (EKB) objects (Boehnhardt et al., 2002). Most probably the spectral features may be attributed to hydrated silicates originated in the bodies. We consider possibilities for silicate dressing and silicate aqueous alteration within them. According to present models of the protoplanetary disk, the temperatures and pressures at the EKB distances (30–50 AU) at the time of formation of the EKB
objects (106 to 108 yr) were very low (15–30 K and 10−9–10−10 bar). At these thermodynamic conditions all volatiles excluding hydrogen, helium and neon were in the solid state. An initial mass fraction of silicates (silicates/(ices + dust)) in EKB parent bodies may be estimated as 0.15–0.30.
Decay of the short-lived 26Al in the bodies at the early stage of their evolution and their mutual collisions (at velocities ≥1.5 km s−1) at the subsequent stage were probably two main sources of their heating, sufficient for melting of water ice. Because of the former process, large EKB bodies (R ≥ 100 km) could contain a large amount of liquid water in their interiors for the period of a few 106 yr. Freezing of the internal ocean might have begun at ≈ 5 × 106 yr after formation of the solar nebula (and CAIs). As a result, aqueous alteration of silicates in the bodies could occur.
A probable mechanism of silicate dressing was sedimentation of silicates with refractory organics, resulting in accumulation of large silicate-rich cores. Crushing and removing icy covers under collisions and exposing EKB bodies’ interiors with increased silicate content could facilitate detection of phyllosilicate spectral features.

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

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

—A preliminary study of the surface of the asteroid 21 Lutetia with ground-based methods is of significant importance, because this object is included into the Rosetta space mission schedule. From August 31 to November 20, 2000, about 50 spectra of Lutetia and the same number of spectra of the solar analog HD10307 (G2V) and regional standards were obtained with a resolution of 4 and 3 nm at the MTM-500 telescope television system of the Crimean astrophysical observatory. From these data, the synthetic magnitudes of the asteroid in the BRV color system have been obtained, the reflected light fluxes have been determined in absolute units, and its reflectance spectra have been calculated for a range of 370–740 nm. In addition, from the asteroid reflectance spectra obtained at different rotation phases, the values of the equivalent width of the most intensive absorption band centered at 430–440 nm and attributed to hydrosilicates of the serpentine type have been calculated. A frequency analysis of the values V (1, 0) confirmed the rotation period of Lutetia 0.d3405 (8.h172) and showed a two-humped light curve with a maximal amplitude of 0.m25. The color indices B–V and V–R showed no noticeable variations with this period. A frequency analysis of the equivalent widths of the absorption band of hydrosilicates near 430–440 nm points to the presence of many significant frequencies, mainly from 15 to 20 c/d (c/d is the number of cycles per day), which can be caused by a heterogeneous distribution of hydrated material on the surface of Lutetia. The sizes of these heterogeneities (or spots) on the asteroid surface have been estimated at 3–5 to 70 km with the most frequent value between 30 and 40 km.

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

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.

Spectral Studies of Asteroids 21 Lutetia and 4 Vesta as Objects of Space Missions V. V. Busarev

Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119992 Russia
Received December 21, 2009

Asteroids 10 Hygiea, 135 Hertha, and 196 Philomela: Heterogeneity of the Material from the Reflectance Spectra

V. V. Busarev
Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119992 Russia
Received December 21, 2009

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