Near-infrared reflectance spectroscopy of Ca-rich clinopyroxenes and prospects for remote spectral characterization of planetary surfaces

Schade, U.; Wäsch, R.; Moroz, L. V.

doi:10.1016/j.icarus.2003.10.016

Cited by 50 publications

(59 citation statements)

References 33 publications

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“…A calibration of mineral chemistry does not exist for high-Ca Type A clinopyroxenes, although Schade et al (2004) suggest that a possible association may exist between the 1.15 μm feature in the pyroxene M1 coordination site and Fe content.…”

Section: Discussionmentioning

confidence: 96%

“…It is also important to note that Type B pyroxenes (orthopyroxenes, low-Ca clinopyroxenes) are the relevant types of pyroxenes for basaltic achondrites and display both primary absorption features, unlike the high-Ca Type A pyroxenes (generally along the diopside-hedenbergite trend in the pyroxene quadrilateral) that often include only the ∼0.9 μm absorption (Adams 1974;Schade et al 2004). A calibration of mineral chemistry does not exist for high-Ca Type A clinopyroxenes, although Schade et al (2004) suggest that a possible association may exist between the 1.15 μm feature in the pyroxene M1 coordination site and Fe content.…”

Section: Discussionmentioning

confidence: 99%

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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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Section: Discussionmentioning

confidence: 96%

Section: Discussionmentioning

confidence: 99%

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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“…The 1-and 2-μm absorption bands of the pyroxenes result from crystal field transitions of iron in octahedral coordination. The positions of these absorptions vary systematically as a function of composition and crystal structure (Adams, 1974;Cloutis and Gaffey, 1991;Schade et al 2004). The presence of calcium, iron, and magnesium in the crystallographic sites affects the locations and shape of these distinct absorptions.…”

Section: Choice Of the End-membersmentioning

confidence: 99%

Quantitative compositional analysis of martian mafic regions using the MEx/OMEGA reflectance data 1. Methodology, uncertainties and examples of application

Poulet

Bibring

Langevin

et al. 2009

Icarus

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This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. OMEGA measurements of mafic surfaces, we develop several sensitivity tests to assess the extent to which the model can be applied to predict pyroxene composition (high-calcium phase and low-calcium phase), abundance of almost neutral components (plagioclase) in the near-infrared wavelength as well as grain sizes, by using a library of selected end-members.Results of the sensitivity tests indicate that the scattering model can estimate both abundances and grain sizes of major basaltic materials of low albedo regions within uncertainties (+/-5 to 15 vol. %). The model is then applied to data from dissected cratered terrains located in Terra Meridiani. The derived grain size including uncertainties is in the 50-500 µm range. This is consistent with the thermal inertia and albedo of this region, which indicates a fine sand-sized surface with little dust. The abundances of plagioclase (43-57%) and pyroxenes (35-45+/-10%, including 11+/-5% of low-calcium phase) are in good agreement with previous basaltlike compositions of low albedo regions from thermal infrared spectral measurements. The method presented in this paper will provide a valuable tool for evaluating the modal mineralogy of other mafic regions of Mars observed in the near-infrared wavelength range.

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“…All eight asteroid band-band data plot slightly above the HED data, which suggests a possible minor contribution from olivine or a high-Ca pyroxene phase. These minerals (olivine, Type A clinopyroxene) only exhibit Band I absorption features; however, Band I centers for olivine will increase with increasing relative abundances while no band center trend is seen for Type A clinopyroxenes (King and Ridley, 1987;Burns, 1993a;Schade et al, 2004;Sanchez et al, 2014). However, any contribution from these phases will be minor as the Figure 4 data plots only slightly above the HED data and a significant contribution from another mineral phase is not apparent in Figure 3 or Figure 5.…”

Section: Pyroxene Band-band Plot Analysismentioning

confidence: 93%

“…All of the average spectra exhibit variably deep absorption features in the ~0.9-and ~1.9-µm spectral regions that are typical of asteroid surfaces dominated by pyroxene (Adams, 1974;Singer, 1981;Cloutis and Gaffey, 1991;Schade et al, 2004). The ~0.9-µm absorption feature for each average spectrum exhibits uniformly high signal-to-noise ratio (SNR); all the spectra extend to the short-wavelength maxima of the absorption features at ~0.70-0.75-µm.…”

Section: Average Asteroid Nir Reflectance Spectramentioning

confidence: 99%

More chips off of Asteroid (4) Vesta: Characterization of eight Vestoids and their HED meteorite analogs

Hardersen

Reddy

Roberts

et al. 2014

Icarus

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Vestoids are generally considered to be fragments from Asteroid (4) Vesta that were ejected by past collisions that document Vesta's collisional history. Dynamical Vestoids are defined by their spatial proximity with Vesta (Zappala et al., 1995;Nesvorny et al., 2012). Taxonomic Vestoids are defined as V-type asteroids that have a photometric, visible-wavelength spectral, or other observational relationship with Vesta (Tholen, 1984; Bus and Binzel, 2002; Carvano et al., 2010). We define 'genetic Vestoids' as V-type asteroids that are probable fragments ejected from (4) Vesta based on the supporting combination of dynamical, near-infrared (NIR) spectral, and taxonomic evidence. NIR reflectance spectroscopy is one of the primary ground-based techniques to constrain an asteroid's major surface mineralogy (Burns, 1993a). Despite the reasonable likelihood that many dynamical and taxonomic Vestoids likely originate from Vesta, ambiguity exists concerning the fraction of these populations that are from Vesta as compared to the fraction of asteroids that might not be related to Vesta.Currently, one of the most robust techniques to identify the genetic Vestoid population is through NIR reflectance spectroscopy from ~0.7-2.5 µm. The derivation of spectral band parameters, and the comparison of those band parameters with those from representative samples from the Howardite-Eucrite-Diogenite (HED) meteorite types, allows a direct comparison of their primary mineralogies. Establishing tighter constraints on the genetic Vestoid population will better inform mass estimates for the current population of probable Vestoids, will provide more accurate orbital information of Vestoid migration through time that will assist dynamical models, and will constrain the Icarus, accepted for publication, August 12, 2014 3 overall current abundance of basaltic material in the main asteroid belt (Moskovitz et al., 2008).This work reports high-quality NIR spectra, and their respective interpretations, for eight V p -type asteroids, as defined by Carvano et al. (2010), that were observed at the

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Near-infrared reflectance spectroscopy of Ca-rich clinopyroxenes and prospects for remote spectral characterization of planetary surfaces

Cited by 50 publications

References 33 publications

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

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

Quantitative compositional analysis of martian mafic regions using the MEx/OMEGA reflectance data 1. Methodology, uncertainties and examples of application

More chips off of Asteroid (4) Vesta: Characterization of eight Vestoids and their HED meteorite analogs

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Near-infrared reflectance spectroscopy of Ca-rich clinopyroxenes and prospects for remote spectral characterization of planetary surfaces

Cited by 50 publications

References 33 publications

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

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

Quantitative compositional analysis of martian mafic regions using the MEx/OMEGA reflectance data 1. Methodology, uncertainties and examples of application

More chips off of Asteroid (4) Vesta: Characterization of eight Vestoids and their HED meteorite analogs

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

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