High‐calcium pyroxene as an indicator of igneous differentiation in asteroids and meteorites

Sunshine, J. M.; Bus, S. J.; McCoy, T. J.; Burbine, T. H.; Corrigan, Catherine M.; Binzel, Richard P.

doi:10.1111/j.1945-5100.2004.tb00950.x

Cited by 103 publications

(90 citation statements)

References 57 publications

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“…If this were the case, the 2 μm band of our asteroid and meteorite spectra would resemble that of Vesta and eucrites, which is not the case. Thus, there is no evidence for partial melting on S-type surfaces, which is at odds with the conclusions of Sunshine et al (2004), Hardersen et al (2006), and Gietzen et al (2012).…”

Section: Compositional Analysis Of Our Meteorite and Asteroid Samplescontrasting

confidence: 46%

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

Vernazza

Zanda

Binzel

et al. 2014

ApJ

125

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Although petrologic, chemical, and isotopic studies of ordinary chondrites and meteorites in general have largely helped establish a chronology of the earliest events of planetesimal formation and their evolution, there are several questions that cannot be resolved via laboratory measurements and/or experiments alone. Here, we propose the rationale for several new constraints on the formation and evolution of ordinary chondrite parent bodies (and, by extension, most planetesimals) from newly available spectral measurements and mineralogical analysis of main-belt S-type asteroids (83 objects) and unequilibrated ordinary chondrite meteorites (53 samples). Based on the latter, we suggest that spectral data may be used to distinguish whether an ordinary chondrite was formed near the surface or in the interior of its parent body. If these constraints are correct, the suggested implications include that: (1) large groups of compositionally similar asteroids are a natural outcome of planetesimal formation and, consequently, meteorites within a given class can originate from multiple parent bodies; (2) the surfaces of large (up to ∼200 km) S-type main-belt asteroids mostly expose the interiors of the primordial bodies, a likely consequence of impacts by small asteroids (D < 10 km) in the early solar system; (3) the duration of accretion of the H chondrite parent bodies was likely short (instantaneous or in less than ∼10 5 yr, but certainly not as long as 1 Myr); (4) LL-like bodies formed closer to the Sun than H-like bodies, a possible consequence of the radial mixing and size sorting of chondrules in the protoplanetary disk prior to accretion.

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Section: Compositional Analysis Of Our Meteorite and Asteroid Samplescontrasting

confidence: 46%

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

Vernazza

Zanda

Binzel

et al. 2014

ApJ

125

View full text Add to dashboard Cite

show abstract

“…Recent work found that Ibitira differed in Δ 17 O [30] and pyroxene Fe/Mn ratio [31] from other eucrites and may sample a separate parent body. Additional basaltic asteroids have also been identified [32], including 17 Thetis, whose average semimajor axis at 2.47 AU is close to the meteorite-delivering 3:1 resonance in the asteroid belt. While the link between eucrites and Vesta seems strong, we cannot rule out Ibitira and/or most eucrites originating on a body like Thetis.…”

Section: Discussionmentioning

confidence: 99%

Formation of vesicles in asteroidal basaltic meteorites

McCoy

Ketcham

Wilson

et al. 2006

Earth and Planetary Science Letters

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“…However, because the Cloutis et al (1986) regression was based on simple mixtures of olivine and orthopyroxene, the presence of more than one pyroxene (or other additional phases) would complicate spectral interpretations of asteroids made using this calibration (Gaffey et al, 1993;Sunshine et al, 2004).…”

Section: +mentioning

confidence: 99%