Robinson, Peter B. 2010 前身星的紫外发射线

主要内容:
他们计算前身星喷出的物质的发射线，发现可以印证告诉运动的线不能被观测到。说以前看到的那些高速线挺奇怪。

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Title:		The rest-frame ultraviolet spectra of GRBs from massive rapidly rotating stellar progenitors
Authors:		Robinson, Peter B.; Perna, Rosalba; Lazzati, Davide; van Marle, Allard J.
Affiliation:		AA(JILA, University of Colorado, 440 UCB, Boulder, CO 80309-0440, USA), AB(JILA, University of Colorado, 440 UCB, Boulder, CO 80309-0440, USA), AC(Department of Physics, NC State University, Campus Box 8202, Raleigh, NC 27695-8202, USA), AD(Bartol Research Institute, University of Delaware, 102 Sharp Laboratory, Newark, DE 19716, USA)
Publication:		Monthly Notices of the Royal Astronomical Society, Volume 401, Issue 1, pp. 88-98. (MNRAS Homepage)
Publication Date:		01/2010
Origin:		WILEY
MNRAS Keywords:		line: formation, methods: numerical, supernovae: general, gamma-rays: bursts, gamma-rays: theory
DOI:		10.1111/j.1365-2966.2009.15672.x
Bibliographic Code:		2010MNRAS.401...88R

Abstract

The properties of a massive star prior to its final explosion are imprinted in the circumstellar medium (CSM) created by its wind and termination shock. We perform a detailed, comprehensive calculation of the time-variable and angle-dependent transmission spectra of an average-luminosity gamma-ray burst (GRB) which explodes in the CSM structure produced by the collapse of a 20 M_solar, rapidly rotating, Z = 0.001 progenitor star. We study both the case in which metals are initially in the gaseous phase and the situation in which they are heavily depleted into dust. We find that high-velocity lines from low-ionization states of silicon, carbon and iron are initially present in the spectrum only if the metals are heavily depleted into dust prior to the GRB explosion. However, such lines disappear on time-scales of a fraction of a second for a burst observed on-axis, and of a few seconds for a burst seen at high latitude, making their observation virtually impossible. Rest-frame lines produced in the termination shock are instead clearly visible in all conditions. We conclude that time-resolved, early-time spectroscopy is not a promising way in which the properties of the GRB progenitor wind can be routinely studied. Previous detections of high-velocity features in GRB ultraviolet spectra must have been either due to a superposition of a physically unrelated absorber or due to a progenitor star with very unusual properties.

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