{"id":528,"date":"2014-02-08T06:46:29","date_gmt":"2014-02-08T06:46:29","guid":{"rendered":"http:\/\/phsites.technion.ac.il\/soker\/?p=528"},"modified":"2015-12-16T15:36:19","modified_gmt":"2015-12-16T13:36:19","slug":"528","status":"publish","type":"post","link":"https:\/\/phsites.technion.ac.il\/soker\/528\/","title":{"rendered":"WD\u2013NS reverse evolution (February 2014)"},"content":{"rendered":"<p>&nbsp;<\/p>\n<p><img loading=\"lazy\" decoding=\"async\" class=\"alignright\" style=\"line-height: 1.5em;\" src=\"http:\/\/mnras.oxfordjournals.org\/content\/early\/2014\/02\/06\/mnras.stu022\/F1.large.jpg\" alt=\"Schematic evolution of binary stars where the less massive star forms a neutron star. \" width=\"378\" height=\"394\" \/><strong>Efrat S<\/strong><strong style=\"line-height: 1.5em;\">abach<\/strong><span style=\"line-height: 1.5em;\"> and <\/span><strong style=\"line-height: 1.5em;\">Noam Soker<\/strong><span style=\"line-height: 1.5em;\"> examine rare evolutionary routes of binary systems where the initially\u00a0more massive\u00a0primary star forms a white dwarf (WD), while the secondary\u00a0<\/span><span style=\"line-height: 1.5em;\">star\u00a0accretes mass from the evolved primary and later ter<\/span><span style=\"line-height: 1.5em;\">minates as acore-collapse supernova (CCSN).\u00a0In such a WD\u2013NS (neutron star) reverse evolution a NS\u00a0or a potential NS-progenitor massive core is formed after the WD. \u00a0<\/span><span style=\"font-size: 14px; line-height: 1.5em;\">These SN explosions\u00a0<\/span><span style=\"font-size: 14px; line-height: 1.5em;\">are likely to be prec<\/span><span style=\"font-size: 14px; line-height: 1.5em;\">eded by strong interaction of the WD with the giant secondary\u2019s core,<\/span><span style=\"line-height: 1.5em;\">\u00a0<\/span><span style=\"background-color: #ffff00;\">leading to an Intermediate-Luminosity Optical Transient<\/span><span style=\"line-height: 1.5em;\"> (<\/span><a style=\"line-height: 1.5em;\" href=\"http:\/\/physics.technion.ac.il\/~ILOT\/\" target=\"_blank\">ILOT<\/a><span style=\"line-height: 1.5em;\">). \u00a0 \u00a0 \u00a0<\/span><a style=\"line-height: 1.5em;\" href=\"http:\/\/adsabs.harvard.edu\/abs\/2013arXiv1310.0388S\" target=\"_blank\">Paper <\/a><span style=\"line-height: 1.5em;\">published in MNRAS.\u00a0<\/span><\/p>\n","protected":false},"excerpt":{"rendered":"<p>&nbsp; Efrat Sabach and Noam Soker examine rare evolutionary routes of binary systems where the initially\u00a0more massive\u00a0primary star forms a white dwarf (WD), while the secondary\u00a0star\u00a0accretes mass from the evolved primary and later terminates as acore-collapse supernova (CCSN).\u00a0In such a WD\u2013NS (neutron star) reverse evolution a NS\u00a0or a potential NS-progenitor massive core is formed after &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-528","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 v27.6 - https:\/\/yoast.com\/product\/yoast-seo-wordpress\/ -->\n<title>WD\u2013NS reverse evolution (February 2014) 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\/528\/\" \/>\n<meta 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