Gamma-ray bursts and density evolution of neutron star binary mergers

被引:0
|
作者
Bagot, P
Zwart, SFP
Yungelson, LR
机构
[1] Univ Montpellier 2, Graal, CNRS, Upresa 5024, F-34095 Montpellier, France
[2] Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands
[3] Russian Acad Sci, Astron Inst, Moscow 109017, Russia
[4] Observ Paris, DARC, Meudon Sect, F-92190 Meudon, France
来源
ASTRONOMY & ASTROPHYSICS | 1998年 / 332卷 / 03期
关键词
stars : binaries; stars : evolution; stars : neutron; cosmology : theory; gamma rays : bursts; gamma rays : theory;
D O I
暂无
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The evolution of the comoving cosmic merger-rate density of neutron star binaries n(c)(z) is calculated using a distribution of their merging times provided by population-synthesis computations of binary stars. We adopt an exponential law for the star formation rate with various timescales for different morphological types of galaxies. For elliptical galaxies also an initial burst of star formation, lasting one Gyr, is considered. The resulting n(c)(z) of most models agree with the form n(c)(z) proportional to (1 + z)(1.5-2) for z less than or similar to 2, which has been proposed for the source population of gamma-ray bursts. Assuming a standard candle luminosity, the computed brightness distribution is consistent with the BATSE results if bursts at the peak flux threshold, P = 0.4 photons cm(-2) s(-1), are located at a limiting redshift of 1.9 to 3.3. Progenitors of the systems producing gamma-ray bursts at small redshift (bright) are likely to host in spiral galaxies and star forming regions whereas these at high redshift (dim) reside mainly in elliptical galaxies. The location of a burst may be up to similar to 1 MPc away from the host galaxy.
引用
收藏
页码:L57 / L60
页数:4
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