Please use this identifier to cite or link to this item:
|Title:||Deconvolution of mixtures with high plagioclase content for the remote interpretation of lunar plagioclase-rich regions||Authors:||Serventi, G.
|Issue Date:||2016||Journal:||ICARUS||Number:||272||First Page:||1||Abstract:||Anorthositic rocks are widespread on the lunar surface and have probably been formed by flotation of PL over a magma ocean. A large portion of pristine rocks are characterized by a low Mg/(Mg+Fe) ratio, and have been classified as ferroan anorthosite, and recently, after observation from SELENE Spectral Profiler,pure anorthosites regions with more than 98% PL have been recognized. In this paper, we analyze a set of mixtures with PL content similar to the ferroan anorthosites and to the pure anorthosite regions, using the Origin Software and the Modified Gaussian Model. We consider three plagioclases with varying FeOwt% contents (PL1, PL2 and PL3)andthree mafic end-members (1) 100% orthopyroxene, (2) 56% orthopyroxene and 44% clinopyroxene, and (3) 100% olivine (OL). The spectral parameters considered here are: band depth, band center, band width, c0 (the continuum intercept) and c1 (the continuum offset). Here we have shown that in pyroxene (PX)-bearing mixtures, the PX is distinguishable even in mixtures with only 1% PX and that PX band at ca. 900 nm is always deeper than PL1 band while PL2 and PL3 are deeperthan OPX 900 nm band from 95, 96% PL. In OL-bearing mixtures, OL detection limit is 2% when mixed with PL1, and 3% and 4% if mixed with PL2 and PL3. We also demonstrated how spectral parameters vary with PL%, and, generally, increasing the PL content: (1) 1250 nm band depth decreases when mixed with OL, while it deepens in mixtures with PX; (2) 1250 nm band centers generally move towards longer wavelength for PL1-bearing mixtures, while do not show significant variations considering PL2/PL3-mixtures; (3) 1250 nm band width of PL1 in E1 and E5-mixtures substantially widens while in other mixtures it only slightly varies. Here we also proposed an application to a real case, from Proclus crater, revealing how studying terrestrial analogues is fundamental to infer hypothesis on the mineralogical composition of a planetary surface, but also how the spectral convergence of spectra characterized by different compositions can led to misleading interpretations.||Note:||Spectroscopic measurements were carried out at Inaf-IAPS Istituto Nazionale di Astrofisica, Roma. EMPA analyses have been performed at Dipartimento di Geoscienze, Padova. E4 end-member has been kindly provided by Dr. Sabrina Ferrari, Department of Geosciences, University of Padova. Financial support by Agenzia Spaziale Italiana, SIMBIO-SYS project. The authors are also grateful to Leah Cheek and to an anonymous reviewer for the stimulating comments and useful suggestions.||URI:||http://hdl.handle.net/20.500.12386/24685||URL:||https://www.sciencedirect.com/science/article/abs/pii/S0019103516000312?via%3Dihub||ISSN:||0019-1035||DOI:||10.1016/j.icarus.2016.01.020||Bibcode ADS:||2016Icar..272....1S||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
Show full item record
Files in This Item:
|Serventi et al_accepted.pdf||postprint||7.15 MB||Adobe PDF||View/Open|
|Serventi et al2016_Icarus_mixtures with high pl content.pdf||[administrators only]||3.92 MB||Adobe PDF|
checked on Sep 18, 2020
checked on Sep 18, 2020
Items in DSpace are published in Open Access, unless otherwise indicated.