{"id":8681,"date":"2016-05-11T07:09:06","date_gmt":"2016-05-11T05:09:06","guid":{"rendered":"http:\/\/karmaka.de\/?p=8681"},"modified":"2016-05-11T07:09:34","modified_gmt":"2016-05-11T05:09:34","slug":"igneous-cooling-history-of-olivine-phyric-shergottite-yamato-980459-constrained-by-dynamic-crystallization-experiments","status":"publish","type":"post","link":"https:\/\/karmaka.de\/?p=8681","title":{"rendered":"Igneous cooling history of olivine-phyric shergottite Yamato 980459 constrained by dynamic crystallization experiments."},"content":{"rendered":"<p>First, E. and Hammer, J.<\/p>\n<p>Meteoritics &#038; Planetary Science. doi: 10.1111\/maps.12659<br \/>\nArticle first published online: 10 MAY 2016<\/p>\n<p><a href=\"http:\/\/onlinelibrary.wiley.com\/doi\/10.1111\/maps.12659\/abstract\" target=\"_blank\"><strong>LINK<\/strong><\/a><\/p>\n<p>&#8220;Dynamic crystallization experiments were performed on a liquid having the bulk composition of olivine-phyric shergottite Yamato 980459, to constrain the igneous thermal history of this meteorite. Key characteristics of the meteorite&#8217;s mineralogy and texture, including several morphologically distinct olivine and pyroxene crystal populations and a glassy mesostasis devoid of plagioclase, were replicated upon cooling from 1435 to 909 \u00b0C at 1 atmosphere under reducing conditions. Three sequential cooling ramps are required to produce synthetic samples with textures and compositions matching Yamato 980459. Olivine phenocrysts formed at <1 \u00b0C h\u22121, presumably at depth in the Martian crust. Pyroxene phenocrysts formed mainly at ~10 \u00b0C h\u22121, consistent with crystallization within a lava flow at depths of 25\u201345 cm. Increased cooling rate (~100 \u00b0C h\u22121) in a third stage suppressed the formation of plagioclase and produced groundmass crystals, consistent with crystallization at lava flow depths of 5\u20137 cm. Although Y 980459 is unique among Martian meteorites (i.e., preserving a primary glassy mesostasis), its emplacement did not require unique physical conditions. Rather, the second and third cooling stages may reflect cooling within the core of a p\u0101hoehoe-like flow and subsequent breakout on the surface of Mars.\"\n<\/p>\n","protected":false},"excerpt":{"rendered":"<p>First, E. and Hammer, J. Meteoritics &#038; Planetary Science. doi: 10.1111\/maps.12659 Article first published online: 10 MAY 2016 LINK &#8220;Dynamic crystallization experiments were performed on a liquid having the bulk composition of olivine-phyric shergottite Yamato&#8230;<\/p>\n","protected":false},"author":1,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[42,43],"tags":[2794,1829,370,1117],"_links":{"self":[{"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/posts\/8681"}],"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=8681"}],"version-history":[{"count":2,"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/posts\/8681\/revisions"}],"predecessor-version":[{"id":8683,"href":"https:\/\/karmaka.de\/index.php?rest_route=\/wp\/v2\/posts\/8681\/revisions\/8683"}],"wp:attachment":[{"href":"https:\/\/karmaka.de\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=8681"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/karmaka.de\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=8681"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/karmaka.de\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=8681"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}