{"id":299,"date":"2013-10-10T20:38:44","date_gmt":"2013-10-10T20:38:44","guid":{"rendered":"http:\/\/phsites.technion.ac.il\/soker\/?p=299"},"modified":"2013-12-18T06:14:39","modified_gmt":"2013-12-18T06:14:39","slug":"explosion-supernova-2011fe-frame-core-degenerate-scenario-october-2013","status":"publish","type":"post","link":"https:\/\/phsites.technion.ac.il\/soker\/explosion-supernova-2011fe-frame-core-degenerate-scenario-october-2013\/","title":{"rendered":"The explosion of supernova 2011fe in the frame of the core-degenerate scenario (October 2013)"},"content":{"rendered":"<p>W<span style=\"color: #000000;\">e <span style=\"color: #0000ff;\">(Noam Soker, Enrique Garcia-Berro, and Leandro G. Althaus)<\/span> <\/span>argue that the properties of the Type Ia supernova \u00a0<span style=\"background-color: #ffff00;\"><strong>SN 2011fe can be best explained within the frame of the core-degenerate (CD) scenario<\/strong><\/span>.\u00a0<\/p>\n<p><span style=\"text-decoration: underline;\">More:<\/span> In the CD scenario a white dwarf (WD) merges with the core of an asymptotic giant branch (AGB) star and forms a rapidly rotating WD,\u00a0with a mass close to and above the critical mass for explosion.\u00a0Rapid rotation prevents immediate collapse and\/or explosion. Spinning down over a time of 0-10 billion year brings the WD to explosion.\u00a0A very long delayed explosion to post-crystallization phase, which lasts for about 2 billion years leads to the formation of a highly carbon-enriched outer layer.\u00a0This can account for the\u00a0carbon-rich composition of the fastest-moving ejecta of SN 2011fe.\u00a0In reaching the conclusion that the CD scenario best explains the observed properties of SN 2011fe we consider both its specific properties,\u00a0like a very compact exploding object and carbon rich composition of the fastest-moving ejecta,\u00a0and the general properties of SNe Ia. \u00a0The full paper is <a href=\"http:\/\/arxiv.org\/abs\/1309.0368\" target=\"_blank\">here<\/a>.\u00a0<\/p>\n<p>&nbsp;<\/p>\n","protected":false},"excerpt":{"rendered":"<p>We (Noam Soker, Enrique Garcia-Berro, and Leandro G. Althaus) argue that the properties of the Type Ia supernova \u00a0SN 2011fe can be best explained within the frame of the core-degenerate (CD) scenario.\u00a0 More: In the CD scenario a white dwarf (WD) merges with the core of an asymptotic giant branch (AGB) star and forms a &hellip;<\/p>\n","protected":false},"author":6,"featured_media":0,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"_genesis_hide_title":false,"_genesis_hide_breadcrumbs":false,"_genesis_hide_singular_image":false,"_genesis_hide_footer_widgets":false,"_genesis_custom_body_class":"","_genesis_custom_post_class":"","_genesis_layout":"","footnotes":""},"categories":[2],"tags":[],"class_list":{"0":"post-299","1":"post","2":"type-post","3":"status-publish","4":"format-standard","6":"category-news","7":"entry"},"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v27.4 - https:\/\/yoast.com\/product\/yoast-seo-wordpress\/ -->\n<title>The explosion of supernova 2011fe in the frame of the core-degenerate scenario (October 2013) Prof. Noam Soker<\/title>\n<meta name=\"robots\" content=\"index, follow, max-snippet:-1, max-image-preview:large, max-video-preview:-1\" \/>\n<link rel=\"canonical\" href=\"https:\/\/phsites.technion.ac.il\/soker\/explosion-supernova-2011fe-frame-core-degenerate-scenario-october-2013\/\" \/>\n<meta property=\"og:locale\" content=\"en_US\" \/>\n<meta property=\"og:type\" content=\"article\" \/>\n<meta property=\"og:title\" content=\"The explosion of supernova 2011fe in the frame of the core-degenerate scenario (October 2013) Prof. Noam Soker\" \/>\n<meta property=\"og:description\" content=\"We (Noam Soker, Enrique Garcia-Berro, and Leandro G. 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