Reflectance Spectra of Olivine–Orthopyroxene-Bearing Assemblages at Decreased Temperatures: Implications for Remote Sensing of Asteroids

Moroz, L. V.; Schade, U.; Wäsch, R.

doi:10.1006/icar.2000.6430

Cited by 86 publications

(71 citation statements)

References 37 publications

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“…In particular, the olivine absorption feature narrows with decreasing temperature. New measurements and analyses Hinrichs et al 1999;Moroz et al 2000;Schade and Wäsch 1999) confirmed the systematic temperature variations in olivine spectra reported by Singer and Roush. These temperature trends were used by Lucey et al (2002) to interpret observed variations in spatially resolved spectra across the surface of 433 Eros and to confirm the presence of olivine.…”

Section: Variations In Olivine Spectra With Temperaturesupporting

confidence: 68%

Untitled

2007

Meteorit & Planetary Scien

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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 surface temperature, has a significant effect on the spectra of olivine-rich asteroids. We show that composition and temperature complexly interact spectrally, and must be simultaneously taken into account in order to infer olivine composition accurately. We find that most (7/9) of the olivinedominated asteroids are magnesian and thus likely sampled mantles differentiated from ordinary chondrite sources (e.g., pallasites). However, two other olivine-rich asteroids (289 Nenetta and 246 Asporina) are found to be more ferroan. Melting models show that partial melting cannot produce olivine-rich residues that are more ferroan than the chondrite precursor from which they formed. Thus, even moderately ferroan olivine must have non-ordinary chondrite origins, and therefore likely originate from oxidized R chondrites or melts thereof, which reflect variations in nebular composition within the asteroid belt. This is consistent with the meteoritic record in which R chondrites and brachinites are rare relative to pallasites.

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Section: Variations In Olivine Spectra With Temperaturesupporting

confidence: 68%

Untitled

2007

Meteorit & Planetary Scien

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“…Therefore, the points for all the asteroids in Fig. 2 might be slightly shifted up and to the right of the given positions, according to Moroz et al (2000); in this case, the Band I and Band II centres for orthopyroxene move to longer wavelengths by nearly 0.003 and 0.02 µm, respectively, values that are smaller than our error bars.…”

Section: First Mineralogical Analysismentioning

confidence: 59%

Basaltic asteroids in the Near-Earth Objects population: a mineralogical analysis

Duffárd

León

Licandro

et al. 2006

A&A

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Aims. We present reflectance spectra of three V-type Near-Earth Objects obtained at the 3.6 m Telescopio Nazionale Galileo and at the 2.5 m Nordic Optical Telescope covering the near-infrared and visible range, respectively. The range from 0.5 to 2.5 µm, encompassing the 1 and 2 µm pyroxene features, allows a mineralogical characterization of these asteroids. Methods. A preliminary analysis using the classical methods has been applied to establish some constraints on the surface mineralogy of these objects. Then, the Modified Gaussian Method was applied to gain further insight on the possible mineral components present in the surface of the objects. Results. The comparison between these basaltic asteroids in near Earth orbits and the achondrite basaltic meteorites shows a quite clear mineralogical link, corroborating the long-standing hypothesis of the Near-Earth Objects population as the immediate source of these meteorites.

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“…Laboratory spectra are commonly collected at room temperature $293 K. It has been demonstrated that absorption band positions of silicate minerals vary with temperature (e.g. Singer and Roush, 1985;Roush and Singer, 1987;Schade and Wäsch, 1999a;Moroz et al, 2000). However, all current temperature corrections are based on data for pyxoxenes of a terrestrial composition.…”

Section: Collection Of Asteroid Spectramentioning

confidence: 99%