伽玛暴外流与介质相互作用的研究
摘要
伽玛射线暴(简称伽玛暴)是一种来自宇宙空间任意方向的短时间内伽玛射线突然增亮的现象。伽玛暴虽然早在1967年就由Vela卫星发现,但直到1997年人们才通过余辉观测确定其宿主星系,并通过宿主星系的红移最终确定了伽玛暴的宇宙学起源。无论是由于大质量恒星死亡产生的长暴、还是由于双致密星并合产生的短暴,它们爆后都将产生一个相对论性的喷流。本论文就集中讨论此喷流与暴周环境的相互作用及其表现形式。
论文第一章是对伽玛暴研究领域的综述。详细介绍了伽玛暴及其余辉的观测与理论,特别是由于Swift卫星和Fermi卫星观测的最新结果导致的新进展。伽玛暴标准火球模型也在这章中做了详细的介绍。本章另一个重点是介绍伽玛暴余辉的起源：相对论性外流与暴周环境介质相互作用,包括动力学演化、辐射机制等。另外,伽玛暴的前身星也在这一章中做了介绍。
第二章介绍一种特别的伽玛暴喷流：环状喷流。此章详细论述了环状喷流的形成、动力学演化,给出了此种喷流与暴周环境介质相互作用产生的多波段余辉光变曲线。各种参数对余辉光变曲线的影响也做了详尽的讨论。结合Swift的观测数据,我们发现环状喷流模型可以很好地解释早期X射线余辉的平滑增亮现象。
第三章介绍了伽玛暴的磁星能量注入模型与余辉平台。Swift时代观测到伽玛暴的一个新特征就是余辉的平台相,此平台相在伽玛暴的标准余辉模型下是无法理解的。但是如果有持续的能量注入到产生余辉的外激波,那么余辉光变曲线将自然产生一个衰减变缓的过程,即产生一个平台相。我们发现磁星可以很好地提供此种形式的能量注入。应用此能量注入模型,我们很好地拟合了具有长期平台相及晚期X余辉异常亮的GRB 060729的多波段余辉光变曲线。对有红移及明显余辉平台相的伽玛暴,通过统计分析我们发现了一个新的伽玛暴参数间的统计关系：伽玛暴X射线余辉平台结束时的X射线光度、平台结束时间以及伽玛暴瞬时阶段的各向同性辐射能量三者之间存在一个非常好的相关性。假设此样本的平台相来源于磁星的能量注入模型,我们发现这个相关性可以得到自然的解释。我们还应用此统计关系对宇宙学的参数进行了一定的限制。这种有明显余辉平台相的伽玛暴可能可以用来当作宇宙学标准烛光。
第四章介绍了失败的伽玛暴的辐射。我们提出了一个失败的伽玛暴火球瞬时辐射的解析模型,发现对于失败的伽玛暴,其光球的半径将大于标准模型中的内激波半径。失败的伽玛暴瞬时辐射将不再是高能伽玛射线波段的非热辐射,而是软X射线或紫外波段的热辐射。失败的伽玛暴产生的余辉在其辐射的早期具有特殊的光谱及光变曲线,利用这些早期余辉的特殊性质我们可以很容易把它与正常伽玛暴的余辉及由于偏轴引起的孤立余辉相区分开来。
第五章介绍了相对论性超新星喷流与介质的相互作用。多年的观测发现一些近距离的长暴与超新星成协,它们都来源于大质量恒星的死亡。一般认为伽玛暴外流是极端相对论性的而超新星外流是非相对论性的。虽然它们之间的洛伦兹因子相差很大,但它们与介质相互作用过程及其辐射机制是相同的,即都是被激波加速的相对论性电子的同步加速辐射。最近观测的中心引擎驱动的超新星更加强了两者本质上的联系。我们发现对于超新星SN 2007gr,可以用一个偏轴的相对论性喷流模型来解释其多波段的观测。
第六章是对整个攻读博士学位期间所作工作的总结以及对未来工作的展望。
Gamma-Ray Bursts (GRBs) are short and intense flashes of gamma-rays observed from the sky in arbitrary directions. Although they are discovered in 1967 by Vela satellite, GRBs were confirmed to be of cosmological origin by the detection of their afterglows and redshifts of their host galaxies till 1997. Relativistic outflows are formed in both long GRBs from the deaths of massive stars and short GRBs from mergers of binary compact stars. In this thesis, we focus on the interactions between the relativistic outflows and surrounding medium.
A brief review on GRBs is given in Chapter 1. We first introduce the recent progress in observations and theories, especially for the Swift and Fermi eras. The standard fireball model is reviewed in detail. A detail afterglow origin, i.e., synchrotron radia-tion of relativistic electrons which are accelerated by the shocks from the interactions between the relativistic outflows and surrounding medium, is also presented here. We also describe the shock physics and the nonthermal radiation mechanisms in this chap-ter. The progenitors of GRBs are also reviewed in this chapter.
In Chapter 2, we introduce one of the GRB jet models, the ring-shaped jet model, including the formation, structure, and dynamical evolution. We numerically calculate the multiband afterglow light curves for this ring-shaped jet colliding with surrounding medium. The effects of parameters on the afterglow light curves are also discussed in detail. We find some Swift GRB afterglows with early rebrightenings can be well reproduced based on our model.
In Chapter 3, we study the model of energy injections from magnetars for GRB af-terglows with plateau phases, which is unpredicted from standard fireball model. We investigate the process of energy injection into the external shock and find that the shallow decay phase is produced in the afterglow light curve. We find that if a strong magnetic pulsar is formed after a GRB, this new born magnetar can provide this kind of energy injection. Using this model, we reproduced the multiband lightcurves for GRB 060729 whose X-ray afterglow has long term plateau and very late time X-ray afterglow. As for a subsample of GRBs with known redshifts and obvious X-ray after-glow plateaus, there is a tight correlation among the luminosity at plateau ending time, plateau ending time and GRB's isotropicγ-ray energy. This correlation could be nat-urally explained if we assume that the plateaus in our sample are resulted from energy injection from magnetars. Using our new three-parameter correlation, we could con-strain directly the cosmological parameters. The subsample of the GRBs with obvious plateaus might be the candidates of the cosmological standard candles.
In Chapter 4, we study the emission from failed GRBs (FGRBs). We derive an analytical solution for the photospheric emission from FGRBs. We find that the radius of the photosphere is larger than that of the internal shock. The radiation in the prompt phase is no longer high energy nothermalγ-ray emission from internal shocks but much lower energy thermal soft X-ray or UV emission from the photosphere. Afterglows from the FGRBs are particular in the early stages and can be distinguished from normal GRB afterglows and off-axis orphan afterglows.
In Chapter 5, we investigate the interactions between relativistic supernova jets and surrounding medium. Nearby long GRBs are observed to be associated with SNe for a few GRB events. They are all resulted from the death of massive stars. In general, the outflows in GRBs are ultra-relativistic, while the outflows in SNe are non-relativistic. However, the processes of interactions between outflows and medium are similar. The radiation mechanisms are both the synchrotron radiation of electrons accelerated to rel-ativistic speeds by shocks. The recent observations of central-engine-driven supernova make the two sources correlated more tightly. We find that the multiband emission from SN 2007gr can be explained by an off-axis relativistic jet colliding with stellar wind.
In Chapter 6, we review our researches briefly. Our discussion and the research prospects are also given in this Chapter.
论文第一章是对伽玛暴研究领域的综述。详细介绍了伽玛暴及其余辉的观测与理论,特别是由于Swift卫星和Fermi卫星观测的最新结果导致的新进展。伽玛暴标准火球模型也在这章中做了详细的介绍。本章另一个重点是介绍伽玛暴余辉的起源：相对论性外流与暴周环境介质相互作用,包括动力学演化、辐射机制等。另外,伽玛暴的前身星也在这一章中做了介绍。
第二章介绍一种特别的伽玛暴喷流：环状喷流。此章详细论述了环状喷流的形成、动力学演化,给出了此种喷流与暴周环境介质相互作用产生的多波段余辉光变曲线。各种参数对余辉光变曲线的影响也做了详尽的讨论。结合Swift的观测数据,我们发现环状喷流模型可以很好地解释早期X射线余辉的平滑增亮现象。
第三章介绍了伽玛暴的磁星能量注入模型与余辉平台。Swift时代观测到伽玛暴的一个新特征就是余辉的平台相,此平台相在伽玛暴的标准余辉模型下是无法理解的。但是如果有持续的能量注入到产生余辉的外激波,那么余辉光变曲线将自然产生一个衰减变缓的过程,即产生一个平台相。我们发现磁星可以很好地提供此种形式的能量注入。应用此能量注入模型,我们很好地拟合了具有长期平台相及晚期X余辉异常亮的GRB 060729的多波段余辉光变曲线。对有红移及明显余辉平台相的伽玛暴,通过统计分析我们发现了一个新的伽玛暴参数间的统计关系：伽玛暴X射线余辉平台结束时的X射线光度、平台结束时间以及伽玛暴瞬时阶段的各向同性辐射能量三者之间存在一个非常好的相关性。假设此样本的平台相来源于磁星的能量注入模型,我们发现这个相关性可以得到自然的解释。我们还应用此统计关系对宇宙学的参数进行了一定的限制。这种有明显余辉平台相的伽玛暴可能可以用来当作宇宙学标准烛光。
第四章介绍了失败的伽玛暴的辐射。我们提出了一个失败的伽玛暴火球瞬时辐射的解析模型,发现对于失败的伽玛暴,其光球的半径将大于标准模型中的内激波半径。失败的伽玛暴瞬时辐射将不再是高能伽玛射线波段的非热辐射,而是软X射线或紫外波段的热辐射。失败的伽玛暴产生的余辉在其辐射的早期具有特殊的光谱及光变曲线,利用这些早期余辉的特殊性质我们可以很容易把它与正常伽玛暴的余辉及由于偏轴引起的孤立余辉相区分开来。
第五章介绍了相对论性超新星喷流与介质的相互作用。多年的观测发现一些近距离的长暴与超新星成协,它们都来源于大质量恒星的死亡。一般认为伽玛暴外流是极端相对论性的而超新星外流是非相对论性的。虽然它们之间的洛伦兹因子相差很大,但它们与介质相互作用过程及其辐射机制是相同的,即都是被激波加速的相对论性电子的同步加速辐射。最近观测的中心引擎驱动的超新星更加强了两者本质上的联系。我们发现对于超新星SN 2007gr,可以用一个偏轴的相对论性喷流模型来解释其多波段的观测。
第六章是对整个攻读博士学位期间所作工作的总结以及对未来工作的展望。
Gamma-Ray Bursts (GRBs) are short and intense flashes of gamma-rays observed from the sky in arbitrary directions. Although they are discovered in 1967 by Vela satellite, GRBs were confirmed to be of cosmological origin by the detection of their afterglows and redshifts of their host galaxies till 1997. Relativistic outflows are formed in both long GRBs from the deaths of massive stars and short GRBs from mergers of binary compact stars. In this thesis, we focus on the interactions between the relativistic outflows and surrounding medium.
A brief review on GRBs is given in Chapter 1. We first introduce the recent progress in observations and theories, especially for the Swift and Fermi eras. The standard fireball model is reviewed in detail. A detail afterglow origin, i.e., synchrotron radia-tion of relativistic electrons which are accelerated by the shocks from the interactions between the relativistic outflows and surrounding medium, is also presented here. We also describe the shock physics and the nonthermal radiation mechanisms in this chap-ter. The progenitors of GRBs are also reviewed in this chapter.
In Chapter 2, we introduce one of the GRB jet models, the ring-shaped jet model, including the formation, structure, and dynamical evolution. We numerically calculate the multiband afterglow light curves for this ring-shaped jet colliding with surrounding medium. The effects of parameters on the afterglow light curves are also discussed in detail. We find some Swift GRB afterglows with early rebrightenings can be well reproduced based on our model.
In Chapter 3, we study the model of energy injections from magnetars for GRB af-terglows with plateau phases, which is unpredicted from standard fireball model. We investigate the process of energy injection into the external shock and find that the shallow decay phase is produced in the afterglow light curve. We find that if a strong magnetic pulsar is formed after a GRB, this new born magnetar can provide this kind of energy injection. Using this model, we reproduced the multiband lightcurves for GRB 060729 whose X-ray afterglow has long term plateau and very late time X-ray afterglow. As for a subsample of GRBs with known redshifts and obvious X-ray after-glow plateaus, there is a tight correlation among the luminosity at plateau ending time, plateau ending time and GRB's isotropicγ-ray energy. This correlation could be nat-urally explained if we assume that the plateaus in our sample are resulted from energy injection from magnetars. Using our new three-parameter correlation, we could con-strain directly the cosmological parameters. The subsample of the GRBs with obvious plateaus might be the candidates of the cosmological standard candles.
In Chapter 4, we study the emission from failed GRBs (FGRBs). We derive an analytical solution for the photospheric emission from FGRBs. We find that the radius of the photosphere is larger than that of the internal shock. The radiation in the prompt phase is no longer high energy nothermalγ-ray emission from internal shocks but much lower energy thermal soft X-ray or UV emission from the photosphere. Afterglows from the FGRBs are particular in the early stages and can be distinguished from normal GRB afterglows and off-axis orphan afterglows.
In Chapter 5, we investigate the interactions between relativistic supernova jets and surrounding medium. Nearby long GRBs are observed to be associated with SNe for a few GRB events. They are all resulted from the death of massive stars. In general, the outflows in GRBs are ultra-relativistic, while the outflows in SNe are non-relativistic. However, the processes of interactions between outflows and medium are similar. The radiation mechanisms are both the synchrotron radiation of electrons accelerated to rel-ativistic speeds by shocks. The recent observations of central-engine-driven supernova make the two sources correlated more tightly. We find that the multiband emission from SN 2007gr can be explained by an off-axis relativistic jet colliding with stellar wind.
In Chapter 6, we review our researches briefly. Our discussion and the research prospects are also given in this Chapter.
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