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

本研究的目的是通过研究重联和伴随的物质抛射和粒子加速的基本机制，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伽马射线暴。主要研究成果如下。1)用磁重联模型解释了耀斑硬X射线图像与Hα图像的明显差异。2)发现了与硬X射线耀斑爆发有关的下行流。3)用Hα和X射线同时观测Moreton波。4)发现了与Moreton波有关的X射线扩展特征(首次发现了日冕快模式激波的三维结构)。5)用MHD模拟EIT波和Moreton波。6)巨型拱廊的快慢激波识别。7)重联流入的MHD模拟。8)日冕加热和纳米耀斑的非线性Alfven波模型。9)发现了日冕的“黎明-黄昏不对称”现象。10)辐射测量--巨型日冕拱门的温度分析和耀斑/拱廊环路长度标度规律的测试。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)作为伽马射线暴模型的崩塌星的广义相对论MHD模拟。14)CME/耀斑的对数正态分布和新的伽马射线暴模型。

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.