Nonlinear and Diamagnetic Nature of Plasma and Activities in the Solar Atmosphere

Details Nonlinear and Diamagnetic Nature of Plasma and Activities in the Solar Atmosphere Nonlinear and Diamagnetic Nature of Plasma and Activities in the Solar Atmosphere

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.3001s&link_type=abstract

American Astronomical Society, SPD meeting #40, #30.01; Bulletin of the American Astronomical Society, Vol. 41, p.864

Astronomy and Astrophysics

Astronomy

Scientific paper

Plasma is a nonlinear and diamagnetic media. Magnetic moment of each charged particle in thermal plasma is μ=-kT/B, where k is the Boltzmann constant, T is the plasma temperature and B is the magnetic flux density. It does not depend on mass or charge. Negative value means that the magnetic moment is anti-parallel to B, or diamagnetic.
This nonlinear and diamagnetic nature of plasma is often not explicitly treated due to low plasma beta assumption. The plasma beta is the ratio between magnetic moment per unit volume and the magnetic flux density. However, if the plasma beta exceeds several percent, nonlinear nature becomes important. This is one of the reasons why nuclear fusion experiment in magnetically confined plasmas is difficult. This condition should be the same in the solar atmosphere.
Particles with magnetic moment anti-parallel to B are pushed toward weak field region along the field. This force (mirror force, f = μ dB/dr = -kT/L) is proportional to the plasma temperature and is inversely proportional to the magnetic scale length L (=1/ (1/B dB/dr)). Generally, magnetic field strength decreases upwards, hence the force is directed upwards. At higher temperature, this force exceeds the gravity force and generates temperature dependent up-flows. If the magnetic field is closed, plasma will be accumulated around the top where magnetic field is the weakest and they suppress B further due to their diamagnetism, hence a high beta region spontaneously appears around the loop top. High-beta plasma around the loop top is unstable against the interchange mode or the ballooning mode due to convex outward curvature (or bad curvature) of B. High-beta disruption will be expected from the outer surface of the loop top.

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