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• W276015309 abstract "The asteroid 2687 Steins was encountered by Rosetta in 2008. Prior to the fly-by, ground-based observations ofSteins were performed [1, 2, 3, 4, 5, 6]. We present a summary of ground-based VIS and NIR reflectance spectraof Steins and compare them with VIRTIS-M-spectra obtained during the fly-by. On the basis of these spectral datawe discuss the relationship to meteorite materials, and the classification of Steins.The ground-based spectra cover a wavelength range from 0.4-2.5 μm. All spectra show a clear absorption featureat ∼0.5 μm and a steep spectral slope between ∼0.6-0.8 μm. At wavelengths >1 μm the spectra show a neutralto slightly reddish trend. The absorption band at ∼0.5 μm is commonly linked to the feature at that wavelengthin the oldhamite spectrum [7]. The oldhamite spectrum shows another weaker feature at 0.96 μm. This weakerfeature at ∼0.96 μm is visible in two of the ground-based spectra. Spectral slopes of most Earth-based spectra arecomparable within arrow bars. The uniform spectral characteristics indicate a homogenous surface of Steins.The VIRTIS-M-spectra of Steins cover the wavelength range from 0.25-1 μm (VIS) and 1-5 μm (IR). The spectrashow an overall flat behavior with a steep red slope at wavelengths <1 μm. The absorption feature located at ∼0.5μm is clearly visible. At wavelengths >3.5 μm thermal emission contributes significantly to the detected radiation.The thermal properties derived from VIRTIS-M long wavelength measurements suggest a thin regolith layer anda low porosity. The shape of the asteroid is consistent with the hypothesis that Steins is a rubble-pile.Ground-based and fly-by spectra of Steins are in good agreement with each other considering the overall spectralcharacteristics and the occurrence of the absorption feature at 0.5 μm. Prior to the Rosetta fly-by Steins has beenclassified (by e.g. [1, 5]) as an E[II]-type asteroid (after [8, 9], also Xe after [10]). VIRTIS data suggest thatSteins can be classified as an igneous E-type asteroid, being a member of the E[II]-subclass. E-type asteroids arelinked to aubrites, which are nearly monomineralic enstatite achondrites [11]. This interpretation is supported bycomparative laboratory reflectance measurements. Although aubrites give the best agreement with Steins spectra,several spectral features cannot be assigned unambiguously. Ti-rich minerals or space weathering implantedproducts were alternatively proposed to reproduce the observed spectral characteristics [1, 12]. Currently nometeorite in our present collection fits the Steins spectra, indicating that Steins is probably not the parent body ofthese meteorites. Because Steins is a reduced anhydrous body, it can be argued that it formed in the inner planetarysystem and was scattered to the main belt. This opens interesting parallels between the E-type population and theformation of Mercury.[1] Barucci et al. (2005) A&A, 430, 313-317. [2] Dotto et al. (2009) A&A, 494, L29-L32. [3] Fornasier etal. (2007) A&A, 474, L29-L32. [4] Fornasier et al. (2008) Icarus, 196, 119-134. [5] Nedelcu et al. (2007) A&A,473, L33-L36. [6] Weissman et al. (2008) Met. Planet. Sci, 43, 905-914. [7] Burbine at al. (2002) Met. Planet. Sci.,37, 1233-1244. [8] Tholen D. J. (1989) in Asteroids II, 1139-1150. [9] Gaffey and Kelley (2004) LPSC XXXV.Abstract #1812. [10] Bus and Binzel (2002) Icarus, 158, 146-177. [11] Keil (2010) Chem. Erde-Geochem., 70,295-317. [12] Shestopalov et al. (2010) Planet. Space Sci., 58, 1400-1403." @default.
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• W276015309 date "2012-04-27" @default.
• W276015309 modified "2023-09-23" @default.
• W276015309 title "Analysis of ground-based and VIRTIS-M/ROSETTA reflectance spectra of asteroid 2687 Šteins: A comparison" @default.
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