Physics of Space Plasma ActivitySpace plasma is so hot that the atoms break up into charged particles which then become trapped and stored in magnetic fields. When critical conditions are reached the magnetic field breaks up, releasing a large amount of energy and causing dramatic phenomena. The largest space plasma activity events observed in the solar system occur on the Sun, when coronal mass ejections expel several billion tons of plasma mass into space. This book provides a coherent and detailed treatment of the physical background of large plasma eruptions in space. It provides the background necessary for dealing with space plasma activity, and allows the reader to reach a deeper understanding of this fascinating natural event. The book employs both fluid and kinetic models, and discusses the applications to magnetospheric and solar activity. This will form an interesting reference for graduate students and academic researchers in the fields of astrophysics and plasma physics. |
Contents
| 7 | |
Plasma models | 25 |
Introduction | 57 |
Particle picture of steady states | 107 |
A unified theory of steady states | 123 |
Quasistatic evolution and the formation of thin | 133 |
Nonideal effects | 185 |
Selected macroinstabilities | 203 |
Aspects of bifurcation and nonlinear dynamics | 343 |
Magnetospheric activity | 371 |
Models of solar activity | 407 |
Discussion | 433 |
details and derivations | 441 |
Variational principle for collisionless plasmas | 451 |
Symbols and fundamental constants | 465 |
| 503 | |
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Common terms and phrases
activity applies approach approximation assume becomes Birn boundary conditions component configuration conservation consider constant constraint corresponding current density current sheet depend derived described determined different direction discontinuity discussed dynamics effects electric field electron energy equation equilibrium et al example exist expression fact field lines finds first flow flux flux tube force function given gives gravity ideal implies important indicate initial instability integration invariance layer leads length limit magnetic field magnetic flux magnetospheric mode motion neutral normal Note observed obtained parallel parameter particle perturbations phase physical plasma plasma sheet possible potential present pressure problem properties reconnection region requires resistive respect role scales Section shown shows side simulations singular solar solution space stability steady structure surface takes term thin tion typical vanishes velocity
Popular passages
Page 483 - Sizes and locations of coronal mass ejections: SMM observations from 1980 and 19841989, J.
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Page 480 - A region of intense plasma wave turbulence on auroral field lines, J.
Page 485 - T. (1998). An X-ray pulsar with a superstrong magnetic field in the soft gamma-ray repeater SGR 1806-20.
Page 480 - X-ray flares and mass outflows driven by magnetic interaction between a protostar and its surrounding disk Igea.