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;
- evolution of solid bodies in the solar system.
More information about my publications and their reading and citation you can find on ResearchGate.
Publications
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.
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
Characteristic Features in the Spectra of Europa, Ganymede, and Callisto
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).
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
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 and spectral-frequency methods of investigating atmosphereless bodies of the Solar system
V V Busarev, V V Prokof'eva-Mikhailovskaya, V V Bochkov
Where Some Asteroid Parent Bodies
V.V.Busarev
35th Lunar and Planetary Science Conference, 2004, Houston, Texas, Abstract
1026.
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
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.
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
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.
FORMATION OF HYDRATED SILICATES IN EDGEWORTH-KUIPER BELT OBJECTS.
A. B. Makalkin, Institute of Earth Physics, RAS,
Moscow, RF (e-mail: makalkin@uipe-ras.scgis.ru); Dorofeeva, V. A. Vernadsky
Institute of Geochemisry, (RAS), Moscow, RF (e-mail: dorofeeva@geokhi.ru);
V. V. Busarev, Sternberg State Astronomical Institute,
Moscow University, RF; (e-mail:
busarev@sai.msu.ru).
Brown University - Vernadsky Institute Microsymposium 38,
October 27-29, 2003, Moscow, Russia
SOME OBSERVATIONAL INDICATIONS OF THE HISTORY AND SRUCTURE OF OUR PLANETARY SYSTEM.
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
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.
Photograph album
My trip to the conference “Near-Earth Astronomy -2003”, Terskol.