| Optical Flash of GRB 990123: Constraints on the Physical Parameters of the Reverse Shock |
| |
| 作者姓名： | Yi-Zhong Fan Zi-Gao Dai Yong-Feng Huang and Tan Lu |
| |
| 作者单位： | Yi-Zhong Fan，Zi-Gao Dai，Yong-Feng Huang and Tan Lu Department of Astronomy，Nanjing University，Nanjing 210093 |
| |
| 基金项目： | the National Natural Science Foundationof China, the National 973 project (NKBRSF G19990754)，the Special Funds for Major State Basic Research Projects，the Foundation for the Author of National Excellent Doctoral Dissertation of P. R. China (Project No |
| |
| 摘 要： | The optical flash accompanying GRB 990123 is believed to be powered by the reverse shock of a thin shell. With the best-fit physical parameters for GRB 990123 and the assumption that the parameters in the optical flash are the same as in the afterglow, we show that: 1) the shell is thick rather than thin, and we have provided the light curve for the thick shell case which coincides with the observation; 2) the theoretical peak flux of the optical flash accounts for only 3×10~-4 of the observed. In order to remove this discrepancy, the physical parameters, the electron energy and magnetic ratios, εe and εB, should be 0.61 and 0.39, which are very different from their values for the late afterglow.
|
| 关 键 词： | 伽玛射线 爆发 物理参数 反转震动 闪光 电子能 余辉 |
Optical Flash of GRB 990123: Constraints on the Physical Parameters of the Reverse Shock |
| |
| Yi-Zhong Fan,Zi-Gao Dai,Yong-Feng Huang and Tan Lu.Optical Flash of GRB 990123: Constraints on the Physical Parameters of the Reverse Shock[J].Chinese Journal of Astronomy and Astrophysics,2002,2(5):449-453. |
| |
| Authors: | Yi-Zhong Fan Zi-Gao Dai Yong-Feng Huang TAN Lu |
| |
| Abstract: | The optical flash accompanying GRB 990123 is believed to be powered by the reverse shock of a thin shell. With the best-fit physical parameters forGRB 990123 and the assumption that the parameters in the optical flash are the same as in the afterglow, we show that: 1) the shell is thick rather than thin, and we have provided the light curve for the thick shell case which coincides with the observation; 2) the theoretical peak flux of the optical flash accounts for only 3×10-4 of the observed. In order to remove this discrepancy, the physical parameters, the electron energy and magnetic ratios, ∈e and ∈B, should be 0.61 and 0.39, which are very different from their values for the late afterglow. |
| |
| Keywords: | gamma rays: bursts - gamma rays: theory |
| 本文献已被 CNKI 万方数据 等数据库收录！ |
