Electromagnetic heavy ion cyclotron instability: Anisotropy constraint in the solar corona

Details Electromagnetic heavy ion cyclotron instability: Anisotropy constraint in the solar corona Electromagnetic heavy ion cyclotron instability: Anisotropy constraint in the solar corona

Jun 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001jgr...10610715g&link_type=abstract

Journal of Geophysical Research, Volume 106, Issue A6, p. 10715-10722

Physics

Plasma Physics

23

Interplanetary Physics: Sources Of The Solar Wind, Solar Physics, Astrophysics, And Astronomy: Corona, Space Plasma Physics: Wave/Particle Interactions, Space Plasma Physics: Waves And Instabilities

Scientific paper

The electromagnetic proton cyclotron anisotropy instability is driven by T⊥p/T∥p>1 where p represents protons and the directional subscripts denote directions relative to the background magnetic field. Fluctuating field growth leads to wave-particle scattering, which in turn imposes an upper bound on the anisotropy of the form T⊥p/T∥p-1=Sp/β∥pαp, where β∥p≡8πnpkBT∥p/Bo2, and the fitting parameters Sp<~1 and αp~=0.4. Recent SOHO observations indicate that minority heavy ions are substantially hotter and more anisotropic than protons in the solar corona. Here linear theory and hybrid simulations have been carried out in a model of a homogeneous, magnetized, collisionless plasma with anisotropic minority oxygen ions (denoted by subscript O). These calculations show that the electromagnetic oxygen ion cyclotron anisotropy instability also leads to wave-particle scattering, which constrains that anisotropy by the form T⊥O/T∥O-1=SO/[(mp/mO)β~∥O]αo, where β~∥O≡8πnekBT∥O/Bo2, So~10 and αO~0.4. This constraint should be observable in the solar corona.

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