温和相对论X射线瞬变080109和SN2008D：从高能GRB/XRF到普通Ibc SN的连续谱
Mildly relativistic X-ray transient 080109 and SN2008D: Towards a continuum from energetic GRB/XRF to ordinary Ibc SN
摘要：
我们分析了迄今为止可用的空间X射线数据以及地面光学数据的X射线瞬态080109/SN 2008 D。根据这些数据，我们认为：（1）初始瞬变（\lesssim 800秒）是由密度大的恒星风引起的相对论性较弱的（\sim几）外流的反向激波发射引起的。(ii)随后的X射线余辉（\lesssim 2 \times 10 ^4 sec）可以归因于外流的前向激波发射，当扫过恒星风介质时，动能为\sim 10^{46} erg。(iii)后期的X射线变平（\gtrsim 2 \times 10^4$ sec）是由SN 2008 D喷出物中最快的非减速成分提供动力的。(iv)X射线瞬变的局部事件发生率的下限为\sim 1.6 \times 10^4 yr^{-1} Gpc^{-3}，表明绝大多数X射线瞬变具有\gtrsim 100度的宽张开角。离轴观察模型不太可能。(v)瞬变080109/SN 2008 D可能导致从GRB SN到欠亮GRB-/XRF-SN到X射线瞬变SN和普通Ibc SN的连续体（如果不是每个Ibc SN都有相对论性喷流），如本函图2所示。
英文摘要：
We analyze the hitherto available space-based X-ray data as well as ground-based optical data of the X-ray transient 080109/SN2008D. From the data we suggest that (i) The initial transient (\lesssim 800 sec) is attributed to the reverse shock emission of a mildly relativistic (Γ\sim a few) outflow stalled by the dense stellar wind. (ii) The subsequent X-ray afterglow (\lesssim 2\times 10^4 sec) can be ascribed to the forward shock emission of the outflow, with a kinetic energy \sim 10^{46} erg, when sweeping up the stellar wind medium. (iii) The late X-ray flattening (\gtrsim 2\times 10^4$ sec) is powered by the fastest non-decelerated component of SN2008D's ejecta. (iv) The local event rate of X-ray transient has a lower limit of \sim 1.6\times 10^4 yr^{-1} Gpc^{-3}, indicating a vast majority of X-ray transients have a wide opening angle of \gtrsim 100 degree. The off-axis viewing model is less likely. (v) Transient 080109/SN2008D may lead to a continuum from GRB-SN to under-luminous GRB-/XRF-SN to X-ray transient-SN and to ordinary Ibc SN (if not every Ibc SN has a relativistic jet), as shown in Figure 2 of this Letter.
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