Solar wind proton temperature anisotropy: Linear theory and WIND/SWE observations

Details Solar wind proton temperature anisotropy: Linear theory and WIND/SWE observations Solar wind proton temperature anisotropy: Linear theory and WIND/SWE observations

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006georl..3309101h&link_type=abstract

Geophysical Research Letters, Volume 33, Issue 9, CiteID L09101

Physics

Plasma Physics

61

Interplanetary Physics: Solar Wind Plasma, Interplanetary Physics: Plasma Waves And Turbulence, Space Plasma Physics: Kinetic Waves And Instabilities, Space Plasma Physics: Kinetic And Mhd Theory, Space Plasma Physics: Wave/Particle Interactions (2483, 6984)

Scientific paper

We present a comparison between WIND/SWE observations (Kasper et al., 2006) of β$\parallel$p and T$\perp$p/T$\parallel$p (where β$\parallel$p is the proton parallel beta and T$\perp$p and T$\parallel$p are the perpendicular and parallel proton temperatures, respectively; here parallel and perpendicular indicate directions with respect to the ambient magnetic field) and predictions of the Vlasov linear theory. In the slow solar wind, the observed proton temperature anisotropy seems to be constrained by oblique instabilities, by the mirror one and the oblique fire hose, contrary to the results of the linear theory which predicts a dominance of the proton cyclotron instability and the parallel fire hose. The fast solar wind core protons exhibit an anticorrelation between β$\parallel$c and T$\perp$c/T$\parallel$c (where β$\parallel$c is the core proton parallel beta and T$\perp$c and T$\parallel$c are the perpendicular and parallel core proton temperatures, respectively) similar to that observed in the HELIOS data (Marsch et al., 2004).

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