期刊
ASTROPHYSICAL JOURNAL
卷 760, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/760/1/93
关键词
supernovae: individual (SN2011ht)
资金
- NASA [NAS5-26555]
- NSF [AST-9987045, AST-1019394]
- Ohio Board of Regents
- Ohio State University Office of Research
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1109394] Funding Source: National Science Foundation
SN2011ht has been described both as a true supernova (SN) and as an impostor. In this paper, we conclude that it does not match some basic expectations for a core-collapse event. We discuss SN2011ht's spectral evolution from a hot dense wind to a cool dense wind, followed by the post-plateau appearance of a faster low density wind during a rapid decline in luminosity. We identify a slow dense wind expanding at only 500-600 km s(-1), present throughout the eruption. A faster wind speed V similar to 900 km s(-1) occurred in a second phase of the outburst. There is no direct or significant evidence for any flow speed above 1000 km s(-1); the broad asymmetric wings of Balmer emission lines in the hot wind phase were due to Thomson scattering, not bulk motion. We estimate a mass-loss rate of order 0.05 M-circle dot yr(-1) during the hot dense wind phase of the event. The same calculations present difficulties for a hypothetical unseen SN blast wave. There is no evidence that the kinetic energy greatly exceeded the luminous energy, roughly 3 x 10(49) erg; so the radiative plus kinetic energy was small compared to a typical SN. We suggest that SN2011ht may have been a giant eruption driven by super-Eddington radiation pressure, perhaps beginning a few months before the discovery. A strongly non-spherical SN might also account for the data at the cost of more free parameters.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据