STUDY OF SOLAR FLARE MECHANISM AND ITS APPLICATION TO GAMMA RAY BURSTS

本研究的目的是通过对重联、质量抛射和粒子加速等基本机制的研究，阐明太阳耀斑的能量释放机制，并将太阳耀斑机制应用于宇宙耀斑和γ射线爆发。主要研究成果如下。1)基于磁重联模型解释耀斑硬X射线和H α图像的明显差异。2)发现与耀斑硬X射线爆发有关的下行流。3)莫尔顿波的H α和X射线同时观测4)发现与莫尔顿波有关的X射线膨胀特征（首次发现日冕快模激波的三维结构）。5)EIT波和莫尔顿波的MHD模拟6)巨型拱廊中快、慢激波的识别。7)重联入流的MHD模拟。8)日冕加热和纳米耀斑的非线性阿尔芬波模型。9)日冕中“黎明-黄昏不对称”的发现。10)巨冕拱发射测量-温度分析及耀斑/拱环长度标度律检验。11）太阳/恒星耀斑和日冕的“HR图”。12)吸积盘日冕的重联加热模型。13)作为伽玛射线暴模型的BSSAR的广义相对论MHD模拟。14）CME/耀斑的对数正态分布和γ暴的新模型。

The purpose of this research is to clarify energy release mechanism of solar flares, by examining basic mechanism of reconnection and associated mass ejections and particle acceleration, and to apply solar flare mechanism to cosmic flares and gamma ray bursts. Main research results are as follows. 1)Explanation of apparent difference between hard X-rays and H alpha images of flares based on magnetic reconnection model. 2)Discovery of downflow associated with hard X-ray bursts of flares. 3)Simultaneous observation of Moreton wave with H alpha and X-rays. 4)Discovery of X-ray expanding features associated with Moreton wave (first discovery of 3D structure of coronal fast mode shock). 5)Modeling of EIT wave and Moreton wave with MHD simulations. 6)Identification of fast and slow shocks in giant arcade. 7)MHD modeling of reconnection inflow. 8)Nonlinear Alfven wave model of coronal heating and nanoflares. 9)Discovery of "dawn-dusk asymmetry" in the solar corona. 10)Emission measure -temperature analysis of giant coronal arcade and test of flare/arcade loop length scaling law. 11)"HR diagram" of solar/stellar flares and coronae. 12)Reconnection heating model of accretion disk corona. 13)General relativistic MHD simulation of collapsars as a model of gamma ray bursts. 14)Log-normal distribution of CME/flare and new model of gamma ray bursts.