Theory of Active Galactic Nuclei

1)开发了自洽求解吸积盘垂直结构和发射光谱的数值编码。数值结果与观测到的活动星系核的软x射线过剩和紫外凸起进行了比较。我们证明了观测结果可以在爱丁顿吸积附近重现。我们还表明，硬x射线的发射可以用热日冕来解释。2)我们证明了耀变体的伽马射线发射可以成功地用逆康普顿散射来解释。我们确定了与激波加速度理论相一致的电子谱，估计了喷流的物理量。我们认为粒子的能量密度高于磁场的能量密度，喷射等离子体很可能由电子-正电子对组成。伽马射线发射被证明发生在距离中心黑洞100到1000史瓦西半径的地方。这些结果为研究射流的整体加速机理提供了重要线索。3)用蒙特卡罗方法研究了激波，特别是斜激波对扩散粒子的加速作用。我们已经证明，与平行冲击相比，加速时间尺度明显缩短。4)我们研究了对活跃星系核中热气体物理状态诊断有重要意义的原子和等离子体过程。我们已经将它们应用于各种天体物理对象。

1) We have developed the numerical code which self-consistently solves the vertical structure of and emission spectrum from accretion disks. Numerical results are compared with observations of soft X-ray excess and UV bump of active galactic nuclei. We showed that observations are reproduced for nearly Eddington accretion. We also showed that hard X-ray emission is explained by a hot corona.2) We showed that gamma-ray emission from blazars is successfully interpreted in terms inverse Compton scattering. We determined electron spectrum consistent with shock acceleration theory, estmated physical quantities of the jets. We argued that energy density of particles dominates that of magnetic fields and that jet plasma most likely consists of electron-positron pairs. Gamma-ray emission was shown to occur at the distance of 100 to 1000 Schwarzschild radii from the central black hole. These results give an important clue to the bulk acceleration mechanism of jets.3) We studied diffusive particle acceleration by shock waves, especially oblique shocks by the Monte Carlo method. We have shown that acceleration time scale is significantly shortened compared with parallel shocks.4) We studied atomic and plasma processes which are important in diagnosing the physical states of hot gas in active galactic nuclei. We have applied them to various astrophysical objects.