Characterization of the 1.2 μm M1 pyroxene band: Extracting cooling history from near‐IR spectra of pyroxenes and pyroxene‐dominated rocks

Abstract

in the M1 site measured by Mössbauer spectroscopy. The strength of the 1.2 µm band relative to the combined strengths of the 1.2 and 2 µm bands, or the M1 intensity ratio, is calculated for 51 howardite, eucrite, and diogenite (HED) meteorites. Diogenites and cumulate eucrites exhibit the lowest M1 intensity ratios, consistent with their formation as slowly cooled cumulates. Basaltic eucrites exhibit a large range of M1 intensity ratios, all of which are consistently higher than the diogenites and cumulate eucrites. This example illustrates how the M1 intensity ratio can be a used as a tool for characterizing the cooling history of remotely detected pyroxene-dominated rocks.

The origin of Vesta’s crust: Insights from spectroscopy of the Vestoids

“…Band center values produced by MGM will be referred to hereafter as 'MGM-derived band centers'. This approach has been shown to successfully resolve the absorptions of overlapping bands (Mustard, 1992;Sunshine and Pieters, 1993;Schade and Wäsch, 1999b;Sunshine et al, 1990Sunshine et al, , 2004Kanner et al, 2007;Klima et al, 2007Klima et al, , 2008, such as those seen in the HED and Vestoid spec-tra. Three diogenite (EET A79002, LAP 91900, GRO 95555) and howardite (EET 87503, QUE 94200, Y-791573) spectra were fit using MGM.…”

Lunar cryptomaria: Mineralogy and composition of ancient volcanic deposits

“…The presence of other minerals may play a role in the band center results from this study because lunar rocks contain many minerals in addition to pyroxene, including olivine, plagioclase, and other minor phases (e.g., ilmenite and spinel), that could influence the shape of the spectrum. For instance, plagioclase has a distinct mineral absorption at 1.25 μm (Conel and Nash, 1970), overlapping substantially with the 1.2 μm pyroxene absorption (e.g., Sunshine et al, 1990;Klima et al, 2008). While both the plagioclase and pyroxene absorption features at $ 1.2 μm are observable with trace amounts of Fe, pyroxene tends to dominate the spectrum due to its larger imaginary index of refraction (cf.…”

Spectroscopy of olivine basalts using FieldSpec and ASTER data: A case study from Wadi Natash volcanic field, south Eastern Desert, Egypt

“…Several authors dealt with the spectral characteristics of rocks and minerals (Hunt and Salisbury 1971;Adams 1974;Hunt 1977;Mackenzie et al 1983;Gaffey 1984Gaffey , 1986Cloutis et al 1986;King and Ridley 1987;Clark and Roush 1984;Cloutis 1985;Cloutis and Gaffey 1991a, b;Clark et al 1990;Clark 1999;Pieters 1993, 1998;Klima et al 2007Klima et al , 2008Klima et al , 2010Madani 2011). Spectral characteristics of carbonate and chlorite minerals are dealt by many authors (Hunt and Salisbury 1971;Adams 1974;Hunt 1977;Mackenzie et al 1983;Gaffey 1984Gaffey , 1986Madani 2011).…”