Shen 2009 喷流装上超新星的外流产生X射线耀发

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Title:		The late jet in gamma-ray bursts and its interactions with a supernova ejecta and a cocoon
Authors:		Shen, Rongfeng; Kumar, Pawan; Piran, Tsvi
Affiliation:		AA(Department of Astronomy, University of Texas, Austin, TX 78712, USA), AB(Department of Astronomy, University of Texas, Austin, TX 78712, USA), AC(Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel)
Publication:		Monthly Notices of the Royal Astronomical Society, Volume 403, Issue 1, pp. 229-245. (MNRAS Homepage)
Publication Date:		03/2010
Origin:		WILEY
MNRAS Keywords:		supernovae: general, gamma-rays: bursts, gamma-rays: theory
DOI:		10.1111/j.1365-2966.2009.16155.x
Bibliographic Code:		2010MNRAS.403..229S

Abstract

Late X-ray flares observed in X-ray afterglows of gamma-ray bursts (GRBs) suggest late central engine activities at a few minutes to hours after the burst. A few unambiguously confirmed cases of supernova associations with nearby long GRBs imply that an accompanying supernova-like component might be a common feature in all long GRB events. These motivate us to study the interactions of a late jet, responsible for an X-ray flare, with various components in a stellar explosion, responsible for a GRB. These components include a supernova shell-like ejecta and a cocoon that was produced when the main jet producing the GRB itself was propagating through the progenitor star. We find that the interaction between the late jet and the supernova ejecta may produce a luminous (up to 10⁴⁹ergs^-1) thermal X-ray transient lasting for ~10s. The interaction between the late jet and the cocoon produces synchrotron self-absorbed non-thermal emission, with the observed peak X-ray flux density from 0.001μJy to 1mJy at 1 keV and a peak optical flux density from 0.01μJy to 0.1Jy (for a redshift z = 2). The light curve due to the late-jet-cocoon interaction has a very small pulse-width-to-time ratio, Δt/t ~ 0.01-0.5, where t is the pulse peak time since the burst trigger. Identifying these features in current and future observations would open a new frontier in the study of GRB progenitor stars.

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