Olivine-dominated asteroids: Mineralogy and origin

  title={Olivine-dominated asteroids: Mineralogy and origin},
  author={Juan A. S{\'a}nchez and Vishnu Reddy and Michael S. P. Kelley and Edward A. Cloutis and William F. Bottke and David Nesvorn'y and Michael P. Lucas and P. S. Hardersen and Michael J. Gaffey and P. A. Abell and Lucille Le Corre},

Early Impact History and Dynamical Origin of Differentiated Meteorites and Asteroids

Laboratory studies of igneously formed meteorites suggest that numerous meteorite parent bodies were melted to form metallic cores and silicate mantles. Studies by the Dawn spacecraft confirm that

The olivine-dominated composition of the Eureka family of Mars Trojan asteroids

We have used the XSHOOTER echelle spectrograph on the European Southern Obseratory (ESO) Very Large Telescope (VLT) to obtain UVB-VIS-NIR (ultraviolet-blue (UVB), visible (VIS) and near-infrared

Olivine-rich asteroids in the near-Earth space

In the framework of a 30-night spectroscopic survey of small near-Earth asteroids (NEAs) we present new results regarding the identification of olivine-rich objects. The following NEAs were

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Methods to constrain the surface mineralogy of asteroids have seen considerable development during the last decade with advancement in laboratory spectral calibrations and validation of our

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Visible and near‐infrared spectroscopy is a widely used method to determine the mineral compositions of meteorites and asteroids. In this study, we first investigated the association of multiple



Mineralogies and source regions of near-Earth asteroids

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Abstract— Melting models indicate that the composition and abundance of olivine systematically co‐vary and are therefore excellent petrologic indicators. However, heliocentric distance, and thus

Contamination of the asteroid belt by primordial trans-Neptunian objects

It is shown that the violent dynamical evolution of the giant-planet orbits required by the so-called Nice model leads to the insertion of primitive trans-Neptunian objects into the outer belt, implying that the observed diversity of the asteroid belt is not a direct reflection of the intrinsic compositional variation of the proto-planetary disk.

Mineralogical Variations within the S-Type Asteroid Class

Abstract A systematic spectral analysis has been Carried out on a large subset (39 of 144) of the S-type asteroid population. The S-asteroid class includes a number of distinct compositional subtypes

Thermal alteration of asteroids: evidence from meteorites

Small main-belt asteroid spectroscopic survey: Initial results

The spectral characterization of small asteroids is important for understanding the evolution of their compositional and mineralogical properties. We report the results of a CCD spectroscopic survey

E‐type asteroid spectroscopy and compositional modeling

[1] We present near-infrared spectroscopic observations (0.8–2.5 μm) of E-type asteroids. We combine these observations with visible wavelength spectra obtained by other researchers and perform Hapke

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— Enstatite meteorites are highly reduced rocks that consist of major, nearly FeO-free enstatite, variable amounts of metallic Fe, Ni and troilite, and a host of rare minerals formed under

Implications of the inferred compositions of asteroids for their collisional evolution

The inferred compositions of mainbelt asteroids set constraints on the nature and degree of collisional evolution of the asteroids. The existence of a basaltic crust on 4 Vesta seems to require that