Physics of Space Plasma Activity
Space 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.
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adiabatic adiabatic invariant American Geophysical Union assume bifurcation boundary conditions collisionless conﬁguration constant constraint coronal coronal mass ejections corresponding current density current layer deﬁned deﬁnition diﬀerent diﬀerential diﬀusion region discussed dispersion relation distribution function dynamics Earth’s eﬀects eigenvalue electric ﬁeld electron energy equilibrium Euler potentials ﬁeld component ﬁnds ﬁnite ﬁrst ﬂare ﬂuctuations ﬂuid ﬂux function ﬂux rope gravity gyroradius Harris sheet ideal MHD instability integration kinetic line conservation magnetic ﬁeld lines magnetic ﬂux magnetic reconnection magnetopause magnetospheric magnetotail mode motion neutral point nonideal obtained Ohm’s law parameter particle perturbations plasma ﬂow plasma physics plasma sheet plasmoid poloidal properties quasi-neutrality quasi-static reconnection rate satisﬁed scales Section separatrix signiﬁcant simulations singular solar solar wind solution space plasma stability steady structure substorm suﬃciently symmetry term thin current sheets tion two-dimensional vanishes vector velocity Vlasov
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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.