等离子体天体物理学.第二部分-重联与耀斑-(影印版) 本书特色

　　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。

等离子体天体物理学.第二部分-重联与耀斑-(影印版) 内容简介

　　《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。

等离子体天体物理学.第二部分-重联与耀斑-(影印版) 目录

1 Magnetic Reconnection
1.1 What is magnetic reconnection？
1.1.1 Neutral points of a magnetic field
1.1.2 Reconnection in vacuum
1.1.3 Reconnection in plasma
1.1.4 Three stages in the reconnection process
1.2 Acceleration in current layers why and how？
1.2.1 The origin of particle acceleration
1.2.2 Acceleration in a neutral current layer
1.3 Practice：Exercises and Answers

2 Reconnection in a Strong Magnetic Field
2.1 Small perturbations near a neutralline
2.1.1 Historical comments
2.1.2 Reconnection in a strong magnetic field
2.1.3 A linearized problem in ideal MHD
2.1.4 Converging waves and the cumulative effect
2.2 Large perturbations near the neutralline
2.2.1 Magnetic field line deformations
2.2.2 Plasma density variations
2.3 Dynamic dissipation of magnetic field
2.3.1 Conditions of appearance
2.3.2 The physical meaning of dynamic dissipation
2.4 Nonstationary analytical models of RCL
2.4.1 Self-similar 2D MHD solutions
2.4.2 Magnetic collapse at the zeroth point
2.4.3 From collisional to collisionless reconnection

3 Evidence of Reconnection in Solar Flares
3.1 The role of magnetic fields
3.1.1 Basic questions
3.1.2 Concept of magnetic reconnection
3.1.3 Some results of observations
3.2 Three-dimensional reconnection in fiares
3.2.1 Topological model of an active region
3.2.2 Topological portrait of an active region
3.2.3 Features of the fiare topological model
3.2.4 The S-like morphology and eruptive activity
3.3 A current layer as the source of energy
3.3.1 Pre-flare accumulation of energy
3.3.2 Flare energy release
3.3.3 The RCL as a part of an electric circuit
3.4 Reconnection in action
3.4.1 Solar flares of the Syrovatsky type
3.4.2 Sakao-type flares
3.4.3 New topologicalmodels
3.4.4 Reconnection between active regions

4 The Bastille Day 2000 Flare
4.1 Main observational properties
4.1.1 General characteristics of the flare
4.1.2 Overlay HXR images on magnetograms
4.1.3 Questions ofinterpretaion
4.1.4 Motion of the HXR kernels
4.1.5 Magnetic field evolution
4.1.6 The HXR kernels and field evolution
4.2 Simplified topological model
4.2.1 Photospheric field model. Topological portrait
4.2.2 Coronal field model. Separators
4.2.3 Chromospheric ribbons and kernels
4.2.4 Reconnected magnetic flux. Electric field
4.2.5 Discussion of topological model

5 Electric Currents Related to Reconnection
5.1 Magnetic reconnection in the corona
5.1.1 Plane reconnection model as a starting point
5.1.2 Three-component reconnection
5.2 Photospheric shear and coronal reconnection
5.2.1 Accumulation of magnetic energy
5.2.2 Flare energy release and CMEs
……
6 Models of Reconnecting Current Layers
7 Reconnection and Collapsing Traps in Solar Flares
8 Solar-type Flares in Laboratory and Space
9 Particle Acceleration in Current Layers

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自然科学 物理学 等离子体物理学

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