类星体、伽玛暴及伽玛射线脉冲星中的高能辐射过程的研究

In this project, we will apply the classical radiation mechanisms and the new radiation mechanisms develpoed by us to the study of radiation in the high energy objects including gamma-ray pulsars (GRPs), gamma-ray bursts (GRBs) and active galactic nuclei (AGNs). The two aspects of our research are the followings: .(1). The study on the radiation properties of GRPs and GRBs. The traditional radiation mechanisms have encountered a number of problems to explain the gamma-ray emission of GRPs and GRBs, e.g., the low radiation efficiency of traditional mechanisms and different phase between radio and gamma-ray for GRPs; the formation of broken power-law spectra, the related deadline problem, the origin of Amati relation and polarization for GRBs. We try to give a solution for these puzzles by using the resonant inverse Compton scattering of relativistic electrons, which has much higher efficiency than the ordinary inverse Compton scattering under some cases..(2). The study on the high energy emission and the broad emission lines in quasars. Fermi's observation shows that there is prominent GeV-TeV emission in quasars, particularly the radio-loud subclass of blazars, which indicates that a large amount of electrons exist in quasars. Besides the traditional synchrotron radiation, inverse Compton scattering, ionization and excitation process，and bremsstrahlung radiation, other observational behaviors for these electrons would appear. The structured jets are supported by We will attempt to use the two-component jet model to explain radio emission and high energy emission in these sources and argue the possible origin of energy, and explore the contribution from these electrons to broad emission lines in quasars.

本项目中我们将结合传统辐射机制和新辐射机制研究高能天体的辐射，研究领域涉及伽玛射线脉冲星、伽玛暴和类星体等。.(1）利用我们建立的共振逆康普顿散射理论(RICS)探讨伽玛脉冲星和伽玛暴的伽玛射线辐射的起源，分析观测资料并做定量比较，结合传统的逆康普顿散射相比，完善这些天体的辐射模型，解释观测上存在的疑惑，为探讨伽玛脉冲星和伽玛暴的伽玛射线的产生机制提供一条新的途径。.(2）探讨类星体中高能辐射的起源和宽发射线的产生。Fermi卫星的观测发现类星体特别是射电噪Blazar天体中存在极强的GeV/TeV高能辐射，暗示了其中存在着大量的相对论电子。对这些相对论电子而言，除了传统的同步辐射，逆康普顿散射，电离激发及轫致辐射外，应还有别的观测效应的出现。我们尝试利用双成份喷流模型来解释这些源的射电和高能辐射，论证其可能的能量来源，并探讨相对论电子对类星体中宽发射线的影响。

此课题要点是把我们提出的新辐射理论应用于天体物理研究。该项目我们完成以下三方面内容: (1).推广的Kompaneets方程. 电子与光子的非弹性碰撞造成的辐射转移-----康普顿化过程，在天体物理学中，特别是伽玛射线天文学和X射线天文中和另一极端低频光子穿过高温等离子体辐射转移如CMB光子谱被相对论电子的distortion相当重要.最近我们得出新的推广的Kompaneets方程，并初步应用于天体物理, 并计划探讨致密天体中微子扩散. (2). 类星体宽发射线起源. 基于我们提出的混合线模型，即类星体中的宽氢线可能是正常的原子（离子）发射线和切伦科夫类发射线的混合线，第一次对类星体中不同宽氢线之间不同的红移给出了定量的理论解释，支持类星体的宽氢线是正常的原子发射线和切伦科夫类发射线的混合线的观点，并且定量拟合中发现两者近似满足强度均分。 (3). 催化机制---固体表面填隙H的化学活性起源于泡利排斥各类固体表面常对外来原子(离子)施加泡利排斥作用. 它明显改变了表面填隙或者替位原子(离子)的物理性质. 本文首先说明泡利排斥作用广泛存在于各类固体表面.我们指出, 过渡族金属`表面下的H原子'正是被泡利激活的填隙H.`泡利激活'原则上可以推广到均相催化中, 我们计划探讨石墨烯表面填隙锂原子的泡利激活.近来的天文观测中发现, 很多有机分子云团中(例如H$_{2}$O, CH$_{4}$, C$_{2}$H$_{2}$, C$_{2}$H$_{4}$ $\cdots$等云团), 同时存在一些尺寸约约$0.001-10~\mu$m 的尘埃物质(如C颗粒, SiO$_{2}$颗粒等等). 两者的并存使我们猜测, 或许这些尘埃物质(包括纳米颗粒)本身就是多相催化剂, 其表面存在的`泡利穴'可能对分子的形成有重要贡献.