Proton temperature anisotropy constraint in the solar wind: ACE observations

Details Proton temperature anisotropy constraint in the solar wind: ACE observations Proton temperature anisotropy constraint in the solar wind: ACE observations

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001georl..28.2759g&link_type=abstract

Geophysical Research Letters, Volume 28, Issue 14, p. 2759-2762

Physics

Plasma Physics

36

Interplanetary Physics: Solar Wind Plasma, Space Plasma Physics: Wave/Particle Interactions

Scientific paper

The electromagnetic proton cyclotron anisotropy instability may arise in collisionless plasmas in which the proton velocity distribution is approximately bi-Maxwellian with T⊥p/T∥p>1, where ⊥ and ∥ denote directions relative to the background magnetic field Bo. Theory and simulations predict that enhanced field fluctuations from this instability impose a constraint on proton temperature anisotropies 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. Plasma and magnetic field observations from the ACE spacecraft reported here show for the first time that this constraint is statistically satisfied in the high speed solar wind near 1 AU, and magnetic power spectra provide evidence that this instability is the source of the constraint.

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