黑洞吸积盘伽玛射线暴的形成率
摘要
尽管已提出许多模型用于解释伽玛射线暴（GRB），但目前被接受的模型都基于形成和/或快速吸积到恒星质量黑洞。我们采用蒙特卡罗方法进行 Population synthesis 计算。我们估算了每类模型的事件率以及那些在形成与爆发生产之间存在显著延迟的模型的传播距离，即双中子星（DNS）合并和中子星-黑洞（BH/NS）合并。对于合理假设，我们计算出宇宙中每日事件率为：i) 合并中子星：~100/天；ii) 中子星-黑洞合并：~450/天；iii) 坍塌星（collapsars）：~10,000/天；iv) helium 星质量黑洞合并：~1000/天；v) 白矢星-黑洞合并：~20/天。然而，这些数的不确定范围非常大，通常为两个到三个数量级。这些率还必须乘以任何相关的棱镜因子和抽样分数（如果并非观察整个模型集合）。 Depending upon the mass of the host galaxy, half of the DNS and BH/NS mergers will happen within 60kpc (for a Milky-Way massed galaxy) to 5Mpc (for a galaxy with negligible mass) from the galactic center. Because of the delay time, neutron star and black hole mergers will happen at a redshift 0.5 to 0.8 times that of the other classes of models. Information is still lacking regarding the hosts of short hard bursts, but we suggest that they are due to DNS and BH/NS mergers and thus will ultimately be determined to lie outside of galaxies and at a closer mean distance than long complex bursts (which we attribute to collapsars).
引用
@article{arxiv.astro-ph/9904122,
title = {Formation Rates of Black Hole Accretion Disk Gamma-Ray Bursts},
author = {C. L. Fryer and S. E. Woosley and D. H. Hartmann},
journal= {arXiv preprint arXiv:astro-ph/9904122},
year = {2008}
}
备注
57 pages total, 23 figures, submitted by ApJ