Thöne, C. C. 2011 GRB101225A来自于氦星和中子星的碰撞

主要内容:
认为来自红移为0.33. 一个伽马暴，来自氦星和中子星并合，余辉是穿过氦星的包层，最后还有超新星成分出来。（怎么又并合又超新星呢？）

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光变

谱

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Title:		The unusual γ-ray burst GRB 101225A from a helium star/neutron star merger at redshift 0.33
Authors:		Thöne, C. C.;... k, S.; Parrish, I.
Affiliation:		AA(IAA - CSIC, Glorieta de la Astronomía s/n, 18008 Granada
Publication:		Nature, Volume 480, Issue 7375, pp. 72-74 (2011). (Nature Homepage)
Publication Date:		12/2011
Origin:		NATURE
Abstract Copyright:		(c) 2011: Nature
DOI:		10.1038/nature10611
Bibliographic Code:		2011Natur.480...72T

Abstract

Long γ-ray bursts (GRBs) are the most dramatic examples of massive stellar deaths, often associated with supernovae. They release ultra-relativistic jets, which produce non-thermal emission through synchrotron radiation as they interact with the surrounding medium. Here we report observations of the unusual GRB 101225A. Its γ-ray emission was exceptionally long-lived and was followed by a bright X-ray transient with a hot thermal component and an unusual optical counterpart. During the first 10 days, the optical emission evolved as an expanding, cooling black body, after which an additional component, consistent with a faint supernova, emerged. We estimate its redshift to be z = 0.33 by fitting the spectral-energy distribution and light curve of the optical emission with a GRB-supernova template. Deep optical observations may have revealed a faint, unresolved host galaxy. Our proposed progenitor is a merger of a helium star with a neutron star that underwent a common envelope phase, expelling its hydrogen envelope. The resulting explosion created a GRB-like jet which became thermalized by interacting with the dense, previously ejected material, thus creating the observed black body, until finally the emission from the supernova dominated. An alternative explanation is a minor body falling onto a neutron star in the Galaxy.

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