Asteroid surface materials: Mineralogical characterizations from reflectance spectra

Gaffey, M. J.; McCord, T. B.

doi:10.1007/bf00240908

Cited by 113 publications

(58 citation statements)

References 96 publications

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“…Similarly, the same correlation is observed in carbonaceous chondrites, which contain a significant fraction of hydrated silicates, such as phyllosilicates. Therefore, it has been suggested that the (U-B) colour might be also useful as an indicator of the presence hydrated materials (Gaffey and McCord 1978). These UV/visible wavelength features have not yet been observed in MBCs.…”

Section: Absorption Features From Surface Ice or Coma Ice Grainsmentioning

confidence: 99%

The Main Belt Comets and ice in the Solar System

Snodgrass

Agarwal

Combi

et al. 2017

Astron Astrophys Rev

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We review the evidence for buried ice in the asteroid belt; specifically the questions around the so-called Main Belt Comets (MBCs). We summarise the evidence for water throughout the Solar System, and describe the various methods for detecting it, including remote sensing from ultraviolet to radio wavelengths. We review progress in the first decade of study of MBCs, including observations, modelling of ice survival, and discussion on their origins. We then look at which methods will likely be most effective for further progress, including the key challenge of direct detection of (escaping) water in these bodies.

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Section: Absorption Features From Surface Ice or Coma Ice Grainsmentioning

confidence: 99%

The Main Belt Comets and ice in the Solar System

Snodgrass

Agarwal

Combi

et al. 2017

Astron Astrophys Rev

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“…Under this scenario, HED meteorites would not have originated from the collisional event that created the 460-km crater and Class 3 dynamical Vesta family members. Yet, the diogenites sample the deeper crust and mantle (cf., Consolmagno and Drake, 1977;Gaffey and McCord, 1978) and should be well represented spectroscopically in the Class 3 Vesta dynamical family members if they are associated with that crater-forming event. Thus, the HED meteorites may not be providing information about Vesta, but rather a similar parent body long ago destroyed.…”

Section: The Origin Of Hed Meteoritesmentioning

confidence: 99%

Closing in on HED meteorite sources

Sykes

Vilas

2014

Earth Planet Sp

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Members of the Vesta dynamical family have orbital elements consistent with ejecta from a single large excavating collision from a single hemisphere of Vesta. The portion of Vesta's orbit at which such an event must have occurred is slightly constrained and depends on the hemisphere impacted. There is some evidence for subsequent disruptions of these ejected objects. Spectroscopy suggests that the dynamical family members are associated with material from Vesta's interior that was excavated by the event giving rise to the crater covering much of Vesta's southern hemisphere. The 505-nm pyroxene feature seen in HED meteorites is relatively absent in a sample of Vesta dynamical family members raising the question of whether this collisional event was the source of the HED meteorites. Asteroids spectroscopically associated with Vesta that possess this feature are dynamically distinct and could have arisen from a different collisional event on Vesta or originated from a body geochemically similar to Vesta that was disrupted early in the history of the solar system.

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“…However, the spectral reflectance of S-type asteroids has a redder slope and weaker 1.0 and 2.0/•m absorption bands than do the spectra of ordinary chondrites measured in terrestrial laboratories [Gaffey and McCord, 1978; Pieters and McFadden, 1994;Galley et al, 1993]. The absence of asteroids with the spectral features of the ordinary chondrites has led to alternative explanations for this apparent paucity of ordinary chondrite analogues in the asteroid belt.…”

Section: Introductionmentioning

confidence: 99%

Surface modification of olivine by H⁺ and He⁺ bombardment

Dukes¹,

Baragiola²,

McFadden³

1999

J. Geophys. Res.

112

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Abstract. Laboratory simulations of solar wind irradiation of olivine, a constituent of ordinary chondritic meteorites and S-type asteroids, show a dramatic chemical reduction of surface iron and, to a lesser extent, silicon. Earth's atmosphere oxidizes any reduced iron instantaneously, whereas irradiated material on the surface of an asteroid would remain reduced. Changes in optical reflectance, due to metallization of the surface, provide a possible explanation for differences in the near-infrared spectra of ordinary chondrite meteorites and their likely parent bodies, the S(IV) asteroids. IntroductionIn an equilibrium condensation model of the formation of the solar system [Grossman, 1972], the mineral phases present in ordinary chondrite meteorites, olivine, pyroxene, plagioclase, and metallic iron, are formed at primordial temperatures consistent with the inner edge of the asteroid belt; therefore one might expect to find ordinary chondritic parent bodies within this region. However, the spectral reflectance of S-type asteroids has a redder slope and weaker 1.

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Asteroid surface materials: Mineralogical characterizations from reflectance spectra

Cited by 113 publications

References 96 publications

The Main Belt Comets and ice in the Solar System

The Main Belt Comets and ice in the Solar System

Closing in on HED meteorite sources

Surface modification of olivine by H⁺ and He⁺ bombardment

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Asteroid surface materials: Mineralogical characterizations from reflectance spectra

Cited by 113 publications

References 96 publications

The Main Belt Comets and ice in the Solar System

The Main Belt Comets and ice in the Solar System

Closing in on HED meteorite sources

Surface modification of olivine by H+ and He+ bombardment

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Surface modification of olivine by H⁺ and He⁺ bombardment