Asteroid 3628 Božněmcová: Covered with angrite-like basalts?

Cloutis, E. A.; Binzel, Richard P.; Burbine, T. H.; Gaffey, M. J.; McCoy, T. J.

doi:10.1111/j.1945-5100.2006.tb00512.x

Cited by 12 publications

(8 citation statements)

References 31 publications

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“…So even though Fe 2+ is concentrated in the M1 site, bands due to the Fe 2+ in the M1 site will not be apparent unless there is little to no discernible Fe 2+ in the M2 site. Cloutis et al (2006) find that Angra dos Reis has a higher percentage of Fe 2+ in the M2 site than D'Orbigny or LEW 86010, which is consistent with the spectral properties of these angrites.…”

Section: Resultssupporting

confidence: 82%

“…Hardersen et al (2006) has proposed that S-type asteroid 138 Tolosa could possibly be a mixture of Type A and B pyroxenes, but this object does not appear spectrally similar to measured angrites. Cloutis et al (2006) has investigated whether 3628 BoûnÏmcová could be covered with angritic material. Asteroids classified as Sr in the Bus and Binzel (2002b) taxonomy, such as 3819 Robinson (semimajor axis of 2.77 AU), have spectra that match angrites very closely in the visible wavelength region (0.44 to 0.92 µm) (Fig.…”

Section: Asteroidsmentioning

confidence: 99%

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Spectral properties of angrites

Burbine

McCoy

Hinrichs

et al. 2006

Meteoritics &Amp; Planetary Science

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86010, and Sahara 99555) are composed predominately of anorthite, Al-Ti diopside-hedenbergite, and Ca-rich olivine, except for the type specimen, Angra dos Reis, which is composed almost entirely of Al-Ti diopside-hedenbergite. D'Orbigny, LEW 86010, and Sahara 99555 also have spectral properties very different from Angra dos Reis. These newly measured angrites all have broad absorption features centered near 1 µm with very weak to absent absorption bands at ∼2 µm, which is characteristic of some clinopyroxenes. The spectrum of Angra dos Reis has the characteristic 1 and 2 µm features due to pyroxene. One asteroid, 3819 Robinson, has similar spectral properties to the newly measured angrites in the visible wavelength region, but does not appear to spectrally match these angrites in the near-infrared.

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Section: Resultssupporting

confidence: 82%

Section: Asteroidsmentioning

confidence: 99%

Spectral properties of angrites

Burbine

McCoy

Hinrichs

et al. 2006

Meteoritics &Amp; Planetary Science

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“…The only asteroid that provides a good spectral match to the angrites is the km-sized Mars Trojan asteroid (5261) Eureka Trilling et al 2007). The Srclass asteroid 3819 Robinson matches some angrites in the visible region but not in the near-infra-red , and asteroid 3628 Boznemcova´might be an unsampled angrite-like body (Cloutis et al 2006). Both are £10 km in diameter.…”

Section: Introductionmentioning

confidence: 91%

“…The Sr‐ class asteroid 3819 Robinson matches some angrites in the visible region but not in the near‐infra‐red (Burbine et al. 2006), and asteroid 3628 Boznemcová might be an unsampled angrite‐like body (Cloutis et al. 2006).…”

Section: Introductionmentioning

confidence: 99%

Impact histories of angrites, eucrites, and their parent bodies

Scott

Bottke

2011

Meteorit & Planetary Scien

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Abstract-Eucrites, which are probably from 4 Vesta, and angrites are the two largest groups of basaltic meteorites from the asteroid belt. The parent body of the angrites is not known but it may have been comparable in size to Vesta as it retained basalts and had a core dynamo. Both bodies were melted early by 26 Al and formed basalts a few Myr after they accreted. Despite these similarities, the impact histories of the angrites and eucrites are very different: angrites are very largely unshocked and none are breccias, whereas most eucrites are breccias and many are shocked. We attribute the lack of shocked and unbrecciated angrites to an impact, possibly at 4558 Myr ago-the radiometric age of the younger angrites-that extracted the angrites from their original parent body into smaller bodies. These bodies, which may have had a diameter of approximately 10 km, suffered much less impact damage than Vesta during the late heavy bombardment because small bodies retain shocked rocks less efficiently than large ones and because large bodies suffer near-catastrophic impacts that deposit vastly more impact energy per kg of target. Our proposed history for the angrites is comparable to that proposed by Bogard and Garrison (2003) for the unbrecciated eucrites with Ar-Ar ages of 4.48 Gyr and that for unbrecciated eucrites with anomalous oxygen isotopic compositions that did not come from Vesta. We infer that the original parent bodies of the angrites and the anomalous eucrites were lost from the belt when the giant planets migrated and the total mass of asteroids was severely depleted. Alternatively, their parent bodies may have formed in the terrestrial planet region and fragments of these bodies were scattered out to the primordial Main Belt as a consequence of terrestrial planet formation.

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“…Abundant plagioclase feldspar has also been identified in O-type asteroid 3628 Božněmcová using VNIR reflectance spectra by Cloutis et al (2006). The spectrum of Božněmcová can be matched by an assemblage of clinopyroxene (~55-75%) and plagioclase feldspar (~20-33%), which would be broadly similar to angrite meteorites (Binzel et al, 2001;Cloutis et al, 2006). They suggested that Božněmcová could have formed by melting and differentiation under oxidizing conditions and probably represents an unsampled angritelike body.…”

Section: Plagioclase On the Asteroidsmentioning

confidence: 98%

Mid‐Infrared Optical Constants of Labradorite, a Triclinic Plagioclase Mineral

Cheng

Rucks

Arnold

et al. 2019

Earth and Space Science

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Plagioclase feldspar is the most abundant rock-forming mineral in the crust of the Earth, Moon, and Mars and is also an important component in some minor bodies in the Solar System. The distribution, abundance, and precise composition of plagioclase on planetary surfaces from remote sensing data are important measurements for evaluating changing conditions during magma evolution. Optical constants are critical input parameters in radiative transfer theory, which enables modeling of spectra for the extraction of mineral abundances and grain sizes from a remotely sensed spectrum. Mid-infrared (MIR) optical constants of most triclinic rock-forming minerals are not available due to the complexity associated with the derivation of optical constants of low-symmetry minerals. In this work, we have calculated the MIR optical constants of a labradorite single crystal using dispersion theory and laboratory reflectance spectra at non-normal incidence. The optical constants we derived here will assist in modeling spectra in the MIR region and quantifying mineral composition, particle size, and abundances from remote sensing data.

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Asteroid 3628 Božněmcová: Covered with angrite-like basalts?

Cited by 12 publications

References 31 publications

Spectral properties of angrites

Spectral properties of angrites

Impact histories of angrites, eucrites, and their parent bodies

Mid‐Infrared Optical Constants of Labradorite, a Triclinic Plagioclase Mineral

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