Vladimir V. Busarev
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.
Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119992
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: email@example.com ;
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
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: firstname.lastname@example.org; 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
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
—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: email@example.com;
2 Research Institute Crimean Astrophysical Observatory, p/o Nauchnyi, Crimea 334413, Ukraine, e-mail: firstname.lastname@example.org
V.V. Busarev, Sternberg Astronomical Institute (SAI), Moscow University,
Universitetskij pr., 13, Moscow, 119992
V. V. BUSAREV, Sternberg State Astronomical Institute, Moscow University,
Russian Federation (RF) (E-mail: email@example.com);
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.
A. B. Makalkin, Institute of Earth Physics, RAS,
Moscow, RF (e-mail: firstname.lastname@example.org); Dorofeeva, V. A. Vernadsky
Institute of Geochemisry, (RAS), Moscow, RF (e-mail: email@example.com);
V. V. Busarev, Sternberg State Astronomical Institute,
Moscow University, RF; (e-mail:
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: firstname.lastname@example.org.
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.
- 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.