Analytical light curves in the realistic model for gamma-ray burst afterglows
文献类型：期刊论文
| 作者 | Wu, XF ; Dai, ZG; Huang, YF; Lu, T
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| 刊名 | ASTROPHYSICAL JOURNAL
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| 出版日期 | 2005-02-01 |
| 卷号 | 619期号:2页码:968-982 |
| 关键词 | gamma rays : bursts hydrodynamics ISM : jets and outflows radiation mechanisms : nonthermal relativity stars : mass loss |
| 英文摘要 | Afterglow light curves are constructed analytically for realistic gamma-ray burst remnants decelerating in either a homogeneous interstellar medium or a stellar wind environment, taking into account the radiative loss of the blast wave, which affects the temporal behaviors significantly. Inverse Compton scattering, which plays an important role when the energy equipartition factor epsilon(e) of electrons is much larger than that of the magnetic field (epsilon(B)), is considered. The inverse Compton effect prolongs the fast cooling phase markedly, during which the relativistic shock is semiradiative and the radiation efficiency is approximately constant, epsilon = epsilon(e). It is further shown that the shock is still semiradiative for quite a long time after it transits into the slow cooling phase because of a slow decreasing rate of the radiation efficiency of electrons. The temporal decaying index of the X-ray afterglow light curve in this semiradiative phase is (3p + 2 + 2epsilon)/(4 - epsilon) in the interstellar medium case and [3p - 2 - (p - 2)epsilon]/2(2 - epsilon) in the stellar wind case, where p is the distribution index of the shock-accelerated electrons. Taking p = 2.2-2.3 as implied from the common shock acceleration mechanism and assuming epsilon(e) similar to 1/3, the temporal index is more consistent with the observed (alpha(X)) similar to 1.3 than the commonly used adiabatic one. The observability of the inverse Compton component in soft X-ray afterglows is also investigated. To manifest as a bump or even dominant in the X-ray afterglows during the relativistic stage, the density must be larger than similar to1-10 cm(-3) in the interstellar medium case, or the wind parameter A(*) must be larger than similar to1 in the stellar wind case. |
| WOS标题词 | Science & Technology ; Physical Sciences |
| 学科主题 | Astronomy & Astrophysics |
| 类目[WOS] | Astronomy & Astrophysics |
| 研究领域[WOS] | Astronomy & Astrophysics |
| 关键词[WOS] | RELATIVISTIC BLAST WAVES ; 25 APRIL 1998 ; RADIATIVE EFFICIENCY ; UNUSUAL SUPERNOVA ; COMPTON EMISSION ; FLUID-DYNAMICS ; FIREBALL MODEL ; KINETIC-ENERGY ; SHOCKS ; ENVIRONMENTS |
| 收录类别 | SCI |
| 语种 | 英语 |
| WOS记录号 | WOS:000226589100026 |
| 公开日期 | 2015-04-14 |
| 源URL | [http://libir.pmo.ac.cn/handle/332002/11107]  |
| 专题 | 紫金山天文台_院士文集_陆埮 |
| 作者单位 | 1.Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China 2.Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China |
| 推荐引用方式 GB/T 7714 | Wu, XF,Dai, ZG,Huang, YF,et al. Analytical light curves in the realistic model for gamma-ray burst afterglows[J]. ASTROPHYSICAL JOURNAL,2005,619(2):968-982. |
| APA | Wu, XF,Dai, ZG,Huang, YF,&Lu, T.(2005).Analytical light curves in the realistic model for gamma-ray burst afterglows.ASTROPHYSICAL JOURNAL,619(2),968-982. |
| MLA | Wu, XF,et al."Analytical light curves in the realistic model for gamma-ray burst afterglows".ASTROPHYSICAL JOURNAL 619.2(2005):968-982. |
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来源：紫金山天文台
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