ChapmanChapman 2007 短暴两个来源更符合观测

主要内容:
考虑到SGR如果放到河外星系，可能被当做短暴。如果考虑短暴来自SGR或者NS-NS并合，与观测到的形成率更符合：短暴的诞生率=NS-NS形成率(理论)+SGR形成率（银河系外推）。

精彩摘抄:


文章信息:
Two populations are better than one: Short gamma-ray bursts from SGR giant flares and NS-NS mergers

Authors: Robert Chapman (1), Robert S. Priddey (1), Nial R. Tanvir (2) ((1) University of Hertfordshire, UK. (2) University of Leicester, UK.)

(Submitted on 28 Sep 2007)

Abstract: With a peak luminosity of ~10^47 erg/s, the December 27th 2004 giant flare from SGR1806-20 would have been visible by BATSE (the Burst and Transient Source Experiment) out to ~50 Mpc. It is thus plausible that some fraction of the short duration Gamma-Ray Bursts (sGRBs) in the BATSE catalogue were due to extragalactic magnetar giant flares. According to the most widely accepted current models, the remaining BATSE sGRBs were most likely produced by compact object (neutron star-neutron star or neutron star-black hole) mergers with intrinsically higher luminosities. Previously, by examining correlations on the sky between BATSE sGRBs and galaxies within 155 Mpc, we placed limits on the proportion of nearby sGRBs. Here, we examine the redshift distribution of sGRBs produced by assuming both one and two populations of progenitor with separate Luminosity Functions (LFs). Using the local Galactic SGR giant flare rate and theoretical NS-NS merger rates evolved according to well-known Star Formation Rate parameterisations, we constrain the predicted distributions by BATSE sGRB overall number counts. We show that only a dual population consisting of both SGR giant flares and NS-NS mergers can reproduce the likely local distribution of sGRBs as well as the overall number counts. In addition, the best fit LF parameters of both sub-populations are in good agreement with observed luminosities.

Comments:	3 pages, 7 figures. To be included in the proceedings of "40 Years of Pulsars" held at McGill University, Montreal, 2007. Proceedings to be published by American Institute of Physics
Subjects:	Astrophysics (astro-ph)
Cite as:	arXiv:0709.4640v1 [astro-ph]