Mildly relativistic X-ray transient 080109 and SN2008D: Towards a continuum from energetic GRB/XRF to ordinary Ibc SN

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dc.creatorXu, Dong
dc.creatorZou, Yuan-Chuan
dc.creatorFan, Yi-Zhong
dc.date2008-01-28
dc.date2008-01-29
dc.date.accessioned2026-07-07T08:56:51Z
dc.date.available2026-07-07T08:56:51Z
dc.descriptionWe 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.
dc.description4 pages, 2 figures
dc.identifierhttps://arxiv.org/abs/0801.4325
dc.identifierhttp://arxiv.org/abs/0801.4325
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/146760
dc.subjectAstrophysics
dc.titleMildly relativistic X-ray transient 080109 and SN2008D: Towards a continuum from energetic GRB/XRF to ordinary Ibc SN
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