2010A&A...517A..23D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST03:25:18

2010A&A...517A..23D - Astronomy and Astrophysics, volume 517, A23-23 (2010/7-1)

Observations, compositional, and physical characterization of near-Earth and Mars-crosser asteroids from a spectroscopic survey.

DE LEON J., LICANDRO J., SERRA-RICART M., PINILLA-ALONSO N. and CAMPINS H.

Abstract (from CDS):

We analyse a significantly large sample of spectroscopic data to provide a compositional characterization of the near-Earth asteroid population. We present visible and near-infrared spectra of a total of 74 near-Earth asteroids (NEAs) and Mars-crossers (MCs), covering the wavelength region from 0.5 to 2.5µm. Using spectra of NEAs from other databases to enlarge our sample, and compiling two comparison samples of main belt asteroids (MBs) and ordinary chondrites (OCs), we analyse a total of 79 NEAs, 91 MBs, and 103 OCs. We obtained our visible and near-infrared spectra using the instruments and the telescopes located at ``El Roque de los Muchachos'' Observatory, in the island of La Palma (Spain). We compute several diagnostic spectral parameters from the reflectance spectra of NEAs, MBs, and OCs, that are used to infer the mineralogical composition. The distribution of the obtained values are analysed in 2 different parameter spaces. We also apply a robust statistical method based on neuronal networks to those spectral parameters, to compare the NEAs with OCs. Space weathering effects and dynamical and physical properties of NEAs and MBs are also studied. Compositional differences between MBs and NEAs are inferred from the mineralogical analysis. The most remarkable results are: (1) the high olivine content of the NEAs; (2) the compositional similarity between NEAs and a small group of meteorites, the LL ordinary chondrites; and (3) that NEAs are not compositionally similar to OCs, implying that they are not the most likely parent bodies of those meteorites, as has been widely believed. To explain their apparently fresh surfaces (NEAs are on average less red than MBs), a combination of composition and size distribution (NEAs have diameters of some kilometres) should be invoked. Dynamical models applied to our sample of NEAs indicate that most of them originate in the inner part of the main belt, as expected.

Abstract Copyright:

Journal keyword(s): minor planets, asteroids: general - methods: observational - techniques: spectroscopic - surveys

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 11532 PM* 01 53 18.3712379665 +00 22 23.275219132   10.36 9.71     G8III/IV 53 1
2 HD 28099 BY* 04 26 40.1215422118 +16 44 48.884181598 8.98 8.78 8.12 7.56 7.23 G2+V 371 0
3 HD 292561 * 06 51 33.7279121561 -00 11 31.522487958 11.277 11.183 10.574 10.226 9.905 F8 45 0
4 BD+00 2717 * 10 57 04.0449104240 -00 13 12.886842194 10.822 10.567 9.903 9.537 9.206 ~ 55 0
5 HD 139287 PM* 15 37 18.1482181279 -00 09 49.690868022   9.04 8.44     G2/3V 32 0
6 BD+00 3383 * 15 38 16.2767705448 +00 15 21.656125086   11.10 10.50     ~ 27 0
7 GSC 02581-02323 * 16 31 33.8125078770 +30 08 46.398483547 13.576 12.972 12.917 12.564 12.212 G2V 62 0
8 TYC 447-508-1 * 18 42 45.0084598923 +00 08 04.694699960 13.092 13.057 12.425 12.064 11.716 ~ 29 0
9 BD-00 4074 * 20 43 11.9568844973 +00 26 13.072595097   10.63 9.90     F8 30 0
10 BD-00 4557 PM* 23 42 41.8263315718 +00 45 13.136892747 10.411 10.305 9.693 9.339 8.991 F8 50 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-03:25:18

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