LINK<\/strong><\/a><\/p>\n“Highlights<\/p>\n
\u2022 35 Antarctic micrometeorites (AMMs) studied in Raman and IR spectroscopies.
\n\u2022 Identification of hydrated and carbon-enriched Fg-AMMs.
\n\u2022 Organic and mineralogical properties of hydrous AMMs are distinct from type 1 and 2 chondrites.
\n\u2022 Hydrous Fg-AMMs may have formed in distinct areas of the solar nebula and\/or evolved on a different parent body(ies) than typical type 1 and 2 chondrites.”<\/p>\n
“This work presents a multi-analysis on 35 Antarctic micrometeorites (AMMs) (Concordia collection 2006) by coupled Raman and Infrared (IR) spectroscopies, in comparison with samples from type 1 and 2 carbonaceous CM, CR and CI chondrites. We identified the Raman G- and D-bands revealing the presence of polyaromatic carbonaceous material on raw particles in a subset of 16 particles. Thirteen AMMs (10 Fg\u202f+\u202f1 Fg-Sc\u202f+\u202f1 Sc) were selected from this first subset, and analyzed by infrared microscopy along with 4 AMMs (2 Fg\u202f+\u202f1 Fg-Sc\u202f+\u202f1 Sc) from a previous study by Dobrica et al. (2011). These analyses showed that scoriaceous, fine-grained scoriaceous and part of the fine-grained AMMs are not hydrated, with a weak abundance of carbonaceous matter. According to the Raman criterion defined by Dobrica et al. (2011), hydrous AMMs do not show structural modifications induced by heating through the atmospheric entry. In several hydrous AMMs, the carbonaceous matter abundance is found larger than in Orgueil (CI), Murchison (CM) and QUE 99177 (CR) chondrites and their mineral content exhibit differences reflected by the structure of the silicate 10\u202f\u00b5m band. These observations suggest that part of the AMMs originates from one, or several, distinct parent bodies with respect to primitive carbonaceous chondrites. Each hydrous Fg-AMMS displays higher CH2\/CH3 ratio and a smaller carbonyl abundance than chondrites, which point toward a mild processing during atmospheric entry, possibly oxidation, which did not modify the carbon backbone and therefore do not induce differences in Raman spectroscopy.”<\/p>\n","protected":false},"excerpt":{"rendered":"
M. Battandier, L. Bonal, E. Quirico, P. Beck, C. Engrand, J. Duprat, E. Dartois Icarus Volume 306, 15 May 2018, Pages 74-93 LINK “Highlights \u2022 35 Antarctic micrometeorites (AMMs) studied in Raman and IR spectroscopies….<\/p>\n","protected":false},"author":1,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[9,3157,127],"tags":[4382,3273,1809,105,1810,327,107,1989,110,684],"_links":{"self":[{"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/posts\/14286"}],"collection":[{"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/users\/1"}],"replies":[{"embeddable":true,"href":"https:\/\/karmaka.de\/index.php?rest_route=%2Fwp%2Fv2%2Fcomments&post=14286"}],"version-history":[{"count":2,"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/posts\/14286\/revisions"}],"predecessor-version":[{"id":14288,"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/posts\/14286\/revisions\/14288"}],"wp:attachment":[{"href":"https:\/\/karmaka.de\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=14286"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/karmaka.de\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=14286"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/karmaka.de\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=14286"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}