Spectral reflectance properties of HED meteorites + CM2 carbonaceous chondrites: Comparison to HED grain size and compositional variations and implications for the nature of low-albedo features on Asteroid 4 Vesta

Cloutis, E. A.; Izawa, M. R. M.; Pompilio, L.; Reddy, V.; Hiesinger, H.; Nathues, A.; Mann, P.; Corre, Lucille Le; Palomba, E.; Bell, James F.

doi:10.1016/j.icarus.2013.02.003

Cited by 55 publications

(56 citation statements)

References 101 publications

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“…On the whole, band centers are consistent with previous measurements of bulk HED spectra [11,12], although there are some intriguing trends that become apparent only at the small spatial resolution (Fig. 3).…”

Section: Pyroxenesupporting

confidence: 90%

Using VSWIR microimaging spectroscopy to explore the mineralogical diversity of HED meteorites

Fraeman

Ehlmann

Northwood-Smith

et al. 2016

2016 8th Workshop on Hyperspectral Image and Signal Processing: Evolution in Remote Sensing (WHISPERS)

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We use VSWIR microimaging spectroscopy to survey the spectral diversity of HED meteorites at 80-µm/pixel spatial scale. Our goal in this work is both to explore the emerging capabilities of microimaging VSWIR spectroscopy and to contribute to understanding the petrologic diversity of the HED suite and the evolution of Vesta. Using a combination of manual and automated hyperspectral classification techniques, we identify four major classes of materials based on VSWIR absorptions that include pyroxene, olivine, Febearing feldspars, and glass-bearing/featureless materials. Results show microimaging spectroscopy is an effective method for rapidly and non-destructively characterizing small compositional variations of meteorite samples and for locating rare phases for possible follow-up investigation. Future work will include incorporating SEM/EDS results to quantify sources of spectral variability and placing observations within a broader geologic framework of the differentiation and evolution of Vesta.

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Section: Pyroxenesupporting

confidence: 90%

Using VSWIR microimaging spectroscopy to explore the mineralogical diversity of HED meteorites

Fraeman

Ehlmann

Northwood-Smith

et al. 2016

2016 8th Workshop on Hyperspectral Image and Signal Processing: Evolution in Remote Sensing (WHISPERS)

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“…This slight offset in position in Figure 3, however, does not affect the resulting interpretations for these asteroids. The HED data in Figure 3 do not encompass the entire range of measured HED band center data, which extend out to ∼0.98 μm for Band I (Figure 4, Cloutis et al 2013). The asteroid Band I positions may also suggest a slight enrichment in an olivine or high-Ca clinopyroxene component to the average surface composition (Hardersen et al 2014), but not enough of an enrichment to lead to a significant non-basaltic surface composition.…”

Section: Groupmentioning

confidence: 94%

Basalt or Not? Near-infrared Spectra, Surface Mineralogical Estimates, and Meteorite Analogs for 33 V_p-type Asteroids

Hardersen

Reddy

Cloutis

et al. 2018

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Investigations of the main asteroid belt and efforts to constrain that population's physical characteristics involve the daunting task of studying hundreds of thousands of small bodies. Taxonomic systems are routinely employed to study the large-scale nature of the asteroid belt because they utilize common observational parameters, but asteroid taxonomies only define broadly observable properties and are not compositionally diagnostic. This work builds upon the results of work by Hardersen et al., which has the goal of constraining the abundance and distribution of basaltic asteroids throughout the main asteroid belt. We report on the near-infrared (NIR: 0.7 to 2.5 μm) reflectance spectra, surface mineralogical characterizations, analysis of spectral band parameters, and meteorite analogs for 33 V p asteroids. NIR reflectance spectroscopy is an effective remote sensing technique to detect most pyroxene group minerals, which are spectrally distinct with two very broad spectral absorptions at ∼0.9 and ∼1.9 μm. Combined with the results from Hardersen et al., we identify basaltic asteroids for ∼95% (39/41) of our inner-belt V p sample, but only ∼25% (2/8) of the outer-belt V p sample. Inner-belt basaltic asteroids are most likely associated with (4) Vesta and represent impact fragments ejected from previous collisions. Outerbelt V p asteroids exhibit disparate spectral, mineralogical, and meteorite analog characteristics and likely originate from diverse parent bodies. The discovery of two additional likely basaltic asteroids provides additional evidence for an outer-belt basaltic asteroid population.

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“…Exogenic infall is also supported by certain HED (howardites, eucrite, diogenite) meteorites, originating from Vesta (e.g. Russell et al, 2013), that contain clasts of carbonaceous chondrite material within a matrix of pyroxene-rich basaltic material (Cloutis et al, 2013;Herrin et al, 2011;McCoy and Reynolds, 2007). Moreover, the broad correlation between dark material and OH signature, detected by VIR, and H abundance, detected by GRanD, (De Sanctis et al, 2012b;Prettyman et al, 2012) is a further indication of carbonaceous chondrite as darkening agent of the Vestan regolith.…”

Section: Introductionmentioning

confidence: 97%

The geological nature of dark material on Vesta and implications for the subsurface structure

Jaumann

Naß

Otto

et al. 2014

Icarus

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a b s t r a c tDeposits of dark material appear on Vesta's surface as features of relatively low-albedo in the visible wavelength range of Dawn's camera and spectrometer. Mixed with the regolith and partially excavated by younger impacts, the material is exposed as individual layered outcrops in crater walls or ejecta patches, having been uncovered and broken up by the impact. Dark fans on crater walls and dark deposits on crater floors are the result of gravity-driven mass wasting triggered by steep slopes and impact seismicity. The fact that dark material is mixed with impact ejecta indicates that it has been processed together with the ejected material. Some small craters display continuous dark ejecta similar to lunar dark-halo impact craters, indicating that the impact excavated the material from beneath a higher-albedo surface. The asymmetric distribution of dark material in impact craters and ejecta suggests non-continuous distribution in the local subsurface. Some positive-relief dark edifices appear to be impact-sculpted hills with dark material distributed over the hill slopes. Dark features inside and outside of craters are in some places arranged as linear outcrops along scarps or as dark streaks perpendicular to the local topography. The spectral characteristics of the dark material resemble that of Vesta's regolith. Dark material is distributed unevenly across Vesta's surface with clusters of all types of dark material exposures. On a local scale, some craters expose or are associated with dark material, while others in the immediate vicinity do not show evidence for dark material. While the variety of surface exposures of dark material and their different geological correlations with surface features, as well as their uneven distribution, indicate a globally inhomogeneous distribution in the subsurface, the dark material seems to be correlated with the rim and ejecta of the older Veneneia south polar basin structure. The origin of the dark material is still being debated, however, the geological analysis suggests that it is exogenic, from carbon-rich low-velocity impactors, rather than endogenic, from freshly exposed mafic material or melt, exposed or created by impacts.

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Spectral reflectance properties of HED meteorites + CM2 carbonaceous chondrites: Comparison to HED grain size and compositional variations and implications for the nature of low-albedo features on Asteroid 4 Vesta

Cited by 55 publications

References 101 publications

Using VSWIR microimaging spectroscopy to explore the mineralogical diversity of HED meteorites

Using VSWIR microimaging spectroscopy to explore the mineralogical diversity of HED meteorites

Basalt or Not? Near-infrared Spectra, Surface Mineralogical Estimates, and Meteorite Analogs for 33 V_p-type Asteroids

The geological nature of dark material on Vesta and implications for the subsurface structure

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Spectral reflectance properties of HED meteorites + CM2 carbonaceous chondrites: Comparison to HED grain size and compositional variations and implications for the nature of low-albedo features on Asteroid 4 Vesta

Cited by 55 publications

References 101 publications

Using VSWIR microimaging spectroscopy to explore the mineralogical diversity of HED meteorites

Using VSWIR microimaging spectroscopy to explore the mineralogical diversity of HED meteorites

Basalt or Not? Near-infrared Spectra, Surface Mineralogical Estimates, and Meteorite Analogs for 33 Vp-type Asteroids

The geological nature of dark material on Vesta and implications for the subsurface structure

Contact Info

Product

Resources

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Basalt or Not? Near-infrared Spectra, Surface Mineralogical Estimates, and Meteorite Analogs for 33 V_p-type Asteroids