等离子体天体物理学.第二部分-重联与耀斑-(影印版)_PDF下载[58MB-百度云]索莫夫

节选

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本书是影印版学术专著,原书由斯普林格出版社于2007年出版。等离子体天体物理学是天体物理学中的一个重要分支。本书作为《等离子体天体物理学》的第二部分,在**部分的基础上,专门探讨了重联和耀斑现象。本书同样具有**部分讲述清晰、深入浅出的优点,而且,其讲述的是目前*前沿的知识。对于这一领域的科研工作者和研究生来说,都是不可错过好书。

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本书特色

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　　本书是影印版学术专著，原书由斯普林格出版社于2007年出版。等离子体天体物理学是天体物理学中的一个重要分支。本书作为《等离子体天体物理学》的第二部分，在**部分的基础上，专门探讨了重联和耀斑现象。本书同样具有**部分讲述清晰、深入浅出的优点，而且，其讲述的是目前*前沿的知识。对于这一领域的科研工作者和研究生来说，都是不可错过好书。

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内容简介

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　　《等离子天体物理学》共分两册，是关于等离子体天体物理学的经典理论和实验基础、当前发展水平的深入浅出的专著。本书作为其第二部分，分别系统地探讨了太阳系、单双星系统、相对论物体、吸积盘和日冕内磁重联和耀斑现象。本书主要是给等离子体天体物理领域的研究者提供参考之用，也同时会成为本专业以及空间物理、地球物理等专业的研究生感兴趣的读物。本书主要是给等离子体天体物理领域的研究者提供参考之用，也同时会成为本专业以及空间物理、地球物理等专业的研究生感兴趣的读物。对于想统一理解等离子体物理和流体力学的应用物理和数学专业的学生也会有帮助。

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1 Magnetic Reconnection1.1 What is magnetic reconnection？1.1.1 Neutral points of a magnetic field1.1.2 Reconnection in vacuum1.1.3 Reconnection in plasma1.1.4 Three stages in the reconnection process1.2 Acceleration in current layers why and how？1.2.1 The origin of particle acceleration1.2.2 Acceleration in a neutral current layer1.3 Practice：Exercises and Answers2 Reconnection in a Strong Magnetic Field2.1 Small perturbations near a neutralline2.1.1 Historical comments2.1.2 Reconnection in a strong magnetic field2.1.3 A linearized problem in ideal MHD2.1.4 Converging waves and the cumulative effect2.2 Large perturbations near the neutralline2.2.1 Magnetic field line deformations2.2.2 Plasma density variations2.3 Dynamic dissipation of magnetic field2.3.1 Conditions of appearance2.3.2 The physical meaning of dynamic dissipation2.4 Nonstationary analytical models of RCL2.4.1 Self-similar 2D MHD solutions2.4.2 Magnetic collapse at the zeroth point2.4.3 From collisional to collisionless reconnection3 Evidence of Reconnection in Solar Flares3.1 The role of magnetic fields3.1.1 Basic questions3.1.2 Concept of magnetic reconnection3.1.3 Some results of observations3.2 Three-dimensional reconnection in fiares3.2.1 Topological model of an active region3.2.2 Topological portrait of an active region3.2.3 Features of the fiare topological model3.2.4 The S-like morphology and eruptive activity3.3 A current layer as the source of energy3.3.1 Pre-flare accumulation of energy3.3.2 Flare energy release3.3.3 The RCL as a part of an electric circuit3.4 Reconnection in action3.4.1 Solar flares of the Syrovatsky type3.4.2 Sakao-type flares3.4.3 New topologicalmodels3.4.4 Reconnection between active regions4 The Bastille Day 2000 Flare4.1 Main observational properties4.1.1 General characteristics of the flare4.1.2 Overlay HXR images on magnetograms4.1.3 Questions ofinterpretaion4.1.4 Motion of the HXR kernels4.1.5 Magnetic field evolution4.1.6 The HXR kernels and field evolution4.2 Simplified topological model4.2.1 Photospheric field model. Topological portrait4.2.2 Coronal field model. Separators4.2.3 Chromospheric ribbons and kernels4.2.4 Reconnected magnetic flux. Electric field4.2.5 Discussion of topological model5 Electric Currents Related to Reconnection5.1 Magnetic reconnection in the corona5.1.1 Plane reconnection model as a starting point5.1.2 Three-component reconnection5.2 Photospheric shear and coronal reconnection5.2.1 Accumulation of magnetic energy5.2.2 Flare energy release and CMEs……6 Models of Reconnecting Current Layers7 Reconnection and Collapsing Traps in Solar Flares8 Solar-type Flares in Laboratory and Space9 Particle Acceleration in Current Layers10 Structural Instability of Reconnecting Current Layers11 Tearing Instability of Reconnecting Current Layers12 Magnetic Reconnection and Turbulence13 Reconnection in Weakly-Ionized Plasma14 Magnetic Reconnection of Electric CurrentsEpilogueAppendix 1. AcronymsAppendix 2. NotationAppendix 3. Useful FormulaeAppendix 4. ConstantsBibliographyIndex