Soderberg 2007 Ib/c型超新星的射电成分

主要内容:
给出了30个Ib/c型超新星的射电观测，并和伽玛暴的射电作对比。一般伽玛暴的明显要比超新星的高，不过也有像980425，060218等和超新星差不多的。

我觉得伽玛暴的射电辐射比较高的原因可能在于它是正轴观测，如果Ibc型超新星也有伽玛暴成分，但喷流没指向观测着，由于极束效应而使射电流量降低。也许就低于超新星自身的射电辐射了，如果喷流的射电辐射碰巧高一点（光变也是先上升后下降的），可能在超新星的射电出现鼓包，called 超新星的伽玛暴成分。

精彩摘抄:

伽玛暴（上面两个）和30个Ibc型超新星的射电光变。

动能－速度图。


文章信息:

arXiv:0706.3047 [ps, pdf, other]

Title: The Radio Properties of Type Ibc Supernovae

Authors: Alicia M. Soderberg (Caltech)

Comments: 8 pages, Proceedings for "Supernova 1987A: 20 Years After: Supernovae and Gamma-Ray Bursters" AIP, New York, eds. S. Immler, K.W. Weiler, and R. McCray

Subjects: Astrophysics (astro-ph)

Over the past few years, long-duration gamma-ray bursts (GRBs), including the subclass of X-ray flashes (XRFs), have been revealed to be a rare variety of Type Ibc supernova (SN Ibc). While all these events result from the death of massive stars, the electromagnetic luminosities of GRBs and XRFs exceed those of ordinary Type Ibc SNe by many orders of magnitude. The observed diversity of stellar death corresponds to large variations in the energy, velocity, and geometry of the explosion ejecta. Using multi-wavelength (radio, optical, X-ray) observations of the nearest GRBs, XRFs, and SNe Ibc, I show that while GRBs and XRFs couple at least 10^48 erg to relativistic material, SNe Ibc typically couple less than 10^48 erg to their fastest (albeit non-relativistic) outflows. Specifically, I find that less than 3% of local SNe Ibc show any evidence for association with a GRB or XRF. Recently, a new class of GRBs and XRFs has been revealed which are under-luminous in comparison with the statistical sample of GRBs. Owing to their faint high-energy emission, these sub-energetic bursts are only detectable nearby (z <>