TY - JOUR
T1 - Collapsar jets, bubbles, and Fe lines
AU - Mészáros, P.
AU - Rees, M. J.
N1 - Funding Information:
We thank NASA for support under grants NAG5-9192 and NAG5-9153, the Sackler Foundation, the Royal Society, and the referee for comments.
PY - 2001/7/20
Y1 - 2001/7/20
N2 - In the collapsar scenario, gamma-ray bursts are caused by relativistic jets expelled along the rotation axis of a collapsing stellar core. We discuss how the structure and time dependence of such jets depend on the stellar envelope and central engine properties, assuming a steady jet injection. It takes a few seconds for the jet to bore its way through the stellar core; most of the energy output during that period goes into a cocoon of relativistic plasma surrounding the jet. This material subsequently forms a bubble of magnetized plasma that takes several hours to expand, subrelativistically, through the envelope of a high-mass supergiant. Jet breakthrough and a conventional burst would be expected not only in He stars but possibly also in blue supergiants. Shock waves and magnetic dissipation in the escaping bubble can contribute a nonthermal UV/X-ray afterglow, and also excite Fe line emission from thermal gas, in addition to the standard jet deceleration power-law afterglow.
AB - In the collapsar scenario, gamma-ray bursts are caused by relativistic jets expelled along the rotation axis of a collapsing stellar core. We discuss how the structure and time dependence of such jets depend on the stellar envelope and central engine properties, assuming a steady jet injection. It takes a few seconds for the jet to bore its way through the stellar core; most of the energy output during that period goes into a cocoon of relativistic plasma surrounding the jet. This material subsequently forms a bubble of magnetized plasma that takes several hours to expand, subrelativistically, through the envelope of a high-mass supergiant. Jet breakthrough and a conventional burst would be expected not only in He stars but possibly also in blue supergiants. Shock waves and magnetic dissipation in the escaping bubble can contribute a nonthermal UV/X-ray afterglow, and also excite Fe line emission from thermal gas, in addition to the standard jet deceleration power-law afterglow.
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U2 - 10.1086/322934
DO - 10.1086/322934
M3 - Article
AN - SCOPUS:0035920026
SN - 0004-637X
VL - 556
SP - L37-L40
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1 PART 2
ER -