{"id":10416,"date":"2016-11-07T08:07:04","date_gmt":"2016-11-07T06:07:04","guid":{"rendered":"http:\/\/karmaka.de\/?p=10416"},"modified":"2016-11-07T08:07:44","modified_gmt":"2016-11-07T06:07:44","slug":"modeling-orbital-gamma-ray-spectroscopy-experiments-at-carbonaceous-asteroids-2","status":"publish","type":"post","link":"https:\/\/karmaka.de\/?p=10416","title":{"rendered":"Modeling orbital gamma-ray spectroscopy experiments at carbonaceous asteroids"},"content":{"rendered":"<p>Lucy F. Lim, Richard D. Starr, Larry G. Evans, Ann M. Parsons, Michael E. Zolensky and William V. Boynton<\/p>\n<p>Meteoritics &#038; Planetary Science. doi: 10.1111\/maps.12786<br \/>\nVersion of Record online: 6 NOV 2016<\/p>\n<p><a href=\"http:\/\/onlinelibrary.wiley.com\/doi\/10.1111\/maps.12786\/full\" target=\"_blank\"><strong>LINK<\/strong><\/a><\/p>\n<p>&#8220;To evaluate the feasibility of measuring differences in bulk composition among carbonaceous meteorite parent bodies from an asteroid or comet orbiter, we present the results of a performance simulation of an orbital gamma-ray spectroscopy (GRS) experiment in a Dawn-like orbit around spherical model asteroids with a range of carbonaceous compositions. The orbital altitude was held equal to the asteroid radius for 4.5 months. Both the asteroid gamma-ray spectrum and the spacecraft background flux were calculated using the MCNPX Monte-Carlo code. GRS is sensitive to depths below the optical surface (to \u224820\u201350 cm depth depending on material density). This technique can therefore measure underlying compositions beneath a sulfur-depleted (e.g., Nittler et al. 2001) or desiccated surface layer. We find that 3\u03c3 uncertainties of under 1 wt% are achievable for H, C, O, Si, S, Fe, and Cl for five carbonaceous meteorite compositions using the heritage Mars Odyssey GRS design in a spacecraft-deck-mounted configuration at the Odyssey end-of-mission energy resolution, FWHM = 5.7 keV at 1332 keV. The calculated compositional uncertainties are smaller than the compositional differences between carbonaceous chondrite subclasses.&#8221;<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Lucy F. Lim, Richard D. Starr, Larry G. Evans, Ann M. Parsons, Michael E. Zolensky and William V. Boynton Meteoritics &#038; Planetary Science. doi: 10.1111\/maps.12786 Version of Record online: 6 NOV 2016 LINK &#8220;To evaluate&#8230;<\/p>\n","protected":false},"author":1,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[77,9,127],"tags":[1854,3274,2419],"_links":{"self":[{"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/posts\/10416"}],"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=10416"}],"version-history":[{"count":2,"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/posts\/10416\/revisions"}],"predecessor-version":[{"id":10418,"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/posts\/10416\/revisions\/10418"}],"wp:attachment":[{"href":"https:\/\/karmaka.de\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=10416"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/karmaka.de\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=10416"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/karmaka.de\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=10416"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}