Characterizing 21 Lutetia with its Reflectance Spectra

Busarev, V. V.; Bochkov, V. V.; Прокофьева, В. В.; Taran, Michail N.

doi:10.1007/978-1-4020-2573-0_9

Cited by 10 publications

(6 citation statements)

References 4 publications

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“…In some of our spectra, we confirmed the presence of a broad feature at 0.45-0.55 μm previously reported by Lazzarin et al (2009) (Busarev et al 2004;Prokof'eva et al 2005) and in 2003 (Lazzarin et al 2004). The feature was interpreted to be indicative of aqueous alteration activity (Lazzarin et al 2004(Lazzarin et al , 2009Prokof'eva et al 2005).…”

Section: Spectral Observationssupporting

confidence: 90%

“…According to Vernazza et al (2009), they are most probable candidates to be the parent bodies of enstatite chondrites. This conclusion has difficulties in explaining 1) the observed features in the Lutetia's visible spectra which are interpreted as being indicative of aqueous alteration material (Lazzarin et al 2004(Lazzarin et al , 2009Busarev 2004); 2) the presence of a 3 μm feature associated with hydrated minerals (Rivkin et al 2000); 3) the features of 5.2-38 μm emissivity spectrum ; and 4) the particular polarization properties of Lutetia. The above-mentioned features can be more naturally explained by assuming similarity of Lutetia's surface to particular types of carbonaceous chondrites.…”

Section: Discussionmentioning

confidence: 98%

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Puzzling asteroid 21 Lutetia: our knowledge prior to the Rosetta fly-by

Belskaya

Fornasier

Krugly

et al. 2010

A&A

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Aims. A wide observational campaign was carried out in [2004][2005][2006][2007][2008][2009] that aimed to complete the ground-based investigation of Lutetia prior to the Rosetta fly-by in July 2010. Methods. We obtained BVRI photometric and V-band polarimetric measurements over a wide range of phase angles, and visible and infrared spectra in the 0.4-2.4 μm range. We analyze them with previously published data to retrieve information about Lutetia's surface properties.Results. Values of lightcurve amplitudes, absolute magnitude, opposition effect, phase coefficient, and BVRI colors of Lutetia surface seen at near pole-on aspect are determined. We define more precisely parameters of polarization phase curve and show their distinct deviation from any other moderate-albedo asteroid. An indication of possible variations in both polarization and spectral data across the asteroid surface are found. To explain features found by different techniques, we propose that (i) Lutetia has a non-convex shape, probably due to a large crater, and heterogeneous surface properties probably related to surface morphology; (ii) at least part of the surface is covered by a fine-grained regolith of particle size smaller than 20 μm; (iii) the closest meteorite analogues of Lutetia's surface composition are particular types of carbonaceous chondrites, or Lutetia has specific surface composition that is not representative among studied meteorites.

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Section: Spectral Observationssupporting

confidence: 90%

Section: Discussionmentioning

confidence: 98%

Puzzling asteroid 21 Lutetia: our knowledge prior to the Rosetta fly-by

Belskaya

Fornasier

Krugly

et al. 2010

A&A

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“…13, Moscow, 119899 Russia The spectral observations of Lutetia performed by Busarev with 1.25-m and 0.6-m telescopes at the Crimean laboratory of the Sternberg Astronomical Institute (Busarev, 2002) and by Bochkov at a 0.5-m telescope of the Crimean Astrophysical Observatory (Bochkov et al , 2003) revealed a noticeable absorption band centered at 430-440 nm in the reflectance spectra of the asteroid. A joint analysis of the reflectance spectra obtained in these studies confirmed the M spectral class of the asteroid (Busarev et al , 2004a). The rather high albedo of the asteroid (0.22) leads to the natural suggestion that its surface material mainly contains high-temperature minerals (of pyroxene and olivine types) with an admixture of metallic iron .…”

Section: The Surface Structure Of the M-type Asteroid 21 Lutetiasupporting

confidence: 60%

“…It is interesting to note that Rivkin et al (1995Rivkin et al ( , 2000 suggest considering such bodies to be an isolated class of objects, which, like asteroids of the C, P, and F types, are initially primitive and fell into the M type by mistake. One of the coauthors of the present paper suggested and developed the hypothesis that hydrosilicates could be brought to the asteroids of high-temperature types (M, S, and E) by fragments of silicate-icy bodies that arrived in the main asteroid belt (MAB) from the Jupiter Growth Zone (Busarev, 1998(Busarev, , 2000(Busarev, , 2002(Busarev, , 2003a(Busarev, , 2004Busarev et al, 2004a). This hypothesis is based on the theoretical results of Safronov (1979), Safronov and Ziglina (1991), and Ruskol and Safronov (1998), who showed that large silicate-icy bodies from the Jupiter region (Jupiter region bodies, JRBs) could be thrown away with a high velocity (up to several kilometers per second) by Jupiter's embryo when its mass reached several Earth masses.…”

Section: Hydrosilicate Spots On the Surface Of 21 Lutetia: Size Estimmentioning

confidence: 95%

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

Прокофьева

Bochkov

Busarev³

2005

Sol Syst Res

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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. d 3405 (8. h 172) and showed a two-humped light curve with a maximal amplitude of 0. m 25 . 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.

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“…Moreover the observations obtained at IRTF ) suggested a similarity with the carbonaceous chondrite spectra which characterize the C-type asteroid. Busarev et al (2004) and Lazzarin et al (2004), obtained several V spectra showing rotational phase variation with possible presence of features at 0.44 and 0.67 µm probably associated to hydrated silicates.…”

Section: Target Selection and Characterizationmentioning

confidence: 98%

Asteroid target selection for the new Rosetta mission baseline

Barucci¹,

Fulchignoni²,

Fornasier

et al. 2005

A&A

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Abstract. The new Rosetta mission baseline to the comet 67P/Churyumov-Gerasimenko includes two asteroid fly-bys. To help in target selection we studied all the candidates of all the possible scenarios. Observations have been carried out at ESO-NTT (La Silla, Chile), TNG (Canaries), and NASA-IRTF (Hawaii) telescopes, in order to determine the taxonomy of all the candidates. The asteroid targets were chosen after the spacecraft interplanetary orbit insertion manoeuvre, when the available total amount of ∆V was known. On the basis of our analysis and the available of ∆V, we recommended to the ESA Science Working Group the asteroids 21 Lutetia and 2867 Steins as targets for the Rosetta mission. The nature of Lutetia is still controversial. Lutetia's spectral properties may be consistent with a composition similar to carbonaceous chondrite meteorites. The spectral properties of Steins suggest a more extensive thermal history. Steins may have a composition similar to relatively rare enstatite chondrite/achondrite meteorites.

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Characterizing 21 Lutetia with its Reflectance Spectra

Cited by 10 publications

References 4 publications

Puzzling asteroid 21 Lutetia: our knowledge prior to the Rosetta fly-by

Puzzling asteroid 21 Lutetia: our knowledge prior to the Rosetta fly-by

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

Asteroid target selection for the new Rosetta mission baseline

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