γ射线暴的研究进展(Ⅰ):γ暴的观测特征及能源机制  

Progress of the Study of Gamma-ray Bursts(Ⅰ):The Observational Feature and Energy Source

作　　者：韦大明[1] 陆埮[1] 

机构地区：[1]南京大学天文系,南京210093

出　　处：《天文学进展》1995年第3期206-219,共14页Progress In Astronomy

摘　　要：文中评述了过去20年中对γ暴的观测结果，包括它的时间特性、能谱特征和空间分布。γ暴的时间结构非常复杂，持续时间相差很大，从小于1s到1000s，平均大约为15s。它的能谱表现为从10keV到10MeV间的连续谱，有的能谱中还含有吸收线和发射线。空间分布表明γ暴源是各向同性的，这说明γ暴要么位于银盘里，要么位于银晕里，或者位于宇宙学距离上。我们还简要讨论了中子星作为γ暴能源的几种机制。We discuss the observational features of gammaray bursts obtained in past twodecades, including temporal structures, energy spectra and spatial distribution. GRBsdisplay very diverse temporal structures, their durations spanning from the shortest < 1sto the longest 1000s, the average is about 15s. The emission has been measured overa broad band of energies from 10keV to 10MeV, there are the absorption and emissionlines in some GRB spectra. The spatial distribution of GRBs appears isotropic. We alsodiscuss some energy source mechainsms originated in the neutron star.

关 键 词：Γ射线暴 Γ暴 观测特征 能源机制 

分 类 号：P172.3[天文地球—天文学]