【摘要】：伽瑪射線暴(簡稱伽瑪暴)是宇宙中最猛烈的Y射線爆發(fā)現(xiàn)象。在Y射線爆發(fā)爆發(fā)之后,一般能夠觀測到X射線耀發(fā)。一般認為X射線耀發(fā)起源于中心引擎的晚期活動,產(chǎn)生于相對論性的火球中。本論文對X射線耀發(fā)的光變曲線、譜演化進行了系統(tǒng)的研究。同時,也研究了具有X射線鼓包成分的伽瑪暴屬性。第一章,簡要介紹了伽瑪暴觀測和理論上的研究進展。結合本人碩士期間所開展的工作,第二章詳細介紹了Swift時期伽瑪暴的研究進展。第三章,介紹了我們對于X射線耀發(fā)下降段的研究工作。在曲率效應模型框架下,我們對29個比較亮的X射線耀發(fā)的光變曲線和譜指數(shù)的演化行為進行了聯(lián)合擬合,估算了X射線耀發(fā)的洛倫茲因子和輻射區(qū)位置。結果顯示,我們所研究的X射線耀發(fā),其快速下降段的特征時標大約在35秒到351秒,而洛倫茲因子在10到78之間。基于此可以估計出X射線耀發(fā)的輻射區(qū)位置,也就是：Rx～7.1×1014至2.7×1016cm。這個結果顯示,X射線耀發(fā)發(fā)生的位置比X射線耀發(fā)時間處的余輝位置靠內。第四章,介紹了我們對于具有X射線鼓包成分的伽瑪暴所開展的研究工作。從光變和譜兩個角度,我們系統(tǒng)分析了所找到的這些暴的X射線鼓包成分。發(fā)現(xiàn)鼓包成分的譜指數(shù)基本不隨時間演化；另外,光變曲線可以用多成分的冪律函數(shù)進行擬合。對X射線鼓包、光學起始鼓包以及光學晚期增亮鼓包的參數(shù)進行比較,發(fā)現(xiàn)它們基本一致,也就是：峰值光度和半寬均和時間有緊密的相關性,分別為Lp∝tp-0.71±0.07和w∝tp0.94±0.07。最后,假定x射線鼓包起源于伽瑪暴瞬時輻射火球的減速,對于有紅移觀測的源,我們估算了伽瑪暴瞬時輻射的洛倫茲因子和輻射效率,分別在20到130及0.02%到3.55%的范圍內。
[Abstract]:Gamma-ray burst (gamma-ray burst) is the most violent Y-ray burst in the universe. X-ray flares are generally observed after Y-ray bursts. X-ray flares are thought to originate from late central engine activity and from relativistic fireballs. In this paper, the optical curve and spectral evolution of X-ray flares are systematically studied. At the same time, the gamma-ray burst properties with X-ray tympanic composition are also studied. In the first chapter, the research progress of Gamma-ray burst observation and theory is briefly introduced. In the second chapter, the research progress of Gamma burst during Swift period is introduced in detail. In the third chapter, we introduce our research work on the falling section of X-ray flares. In the framework of curvature effect model, the phototropic curves of 29 bright X-ray flares and the evolution of spectral exponents are fitted together, and the Lorentz factor and the location of radiation region of X-ray flares are estimated. The results show that the characteristic time scale of the rapid descent of the X-ray flares is about 35 seconds to 351 seconds and the Lorentz factor is between 10 and 78 seconds. Based on this, the location of the radiation region of the X-ray flares can be estimated, that is, 7. 1 脳 1014 to 2. 7 脳 10 ~ (16) cm ~ (-1) of the X ray flares. The results show that the position of the X ray flares is inward than that of the afterglow at the time of the X ray flares. In chapter 4, we introduce our research work on gamma bursts with X-ray tympanic composition. From the point of view of light variation and spectrum, we have systematically analyzed the X-ray tympanic compositions of these storms. It is found that the spectral exponent of the bulge component does not evolve with time, and that the optical variation curve can be fitted by the power law function of multiple components. By comparing the parameters of X-ray bulge, optical initial tympanic bag and late optical brightening drum, it is found that they are basically the same, that is, the peak luminosity and half width are closely correlated with time, which are Lp 鈭，

本文編號：2223875