NASA Logo

NTRS

NTRS - NASA Technical Reports Server

Back to Results
Solar Wind Proton Temperature Anisotropy: Linear Theory and WIND/SWE ObservationsWe present a comparison between WIND/SWE observations (Kasper et al., 2006) of beta parallel to p and T perpendicular to p/T parallel to p (where beta parallel to p is the proton parallel beta and T perpendicular to p and T parallel to p are the perpendicular and parallel proton 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 beta parallel to c and T perpendicular to c/T parallel to c (where beta parallel to c is the core proton parallel beta and T perpendicular to c and T parallel to c are the perpendicular and parallel core proton temperatures, respectively) similar to that observed in the HELIOS data (Marsch et al., 2004).
Document ID
20070011610
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Hellinger, P. (Ceskoslovenska Akademie Ved Prague, Czechoslovakia)
Travnicek, P. (Ceskoslovenska Akademie Ved Prague, Czechoslovakia)
Kasper, J. C. (Massachusetts Inst. of Tech. Cambridge, MA, United States)
Lazarus, A. J. (Massachusetts Inst. of Tech. Cambridge, MA, United States)
Date Acquired
August 23, 2013
Publication Date
May 6, 2006
Publication Information
Publication: Geophysical Research Letters
Volume: 33
Issue: 9
Subject Category
Solar Physics
Funding Number(s)
CONTRACT_GRANT: NNG05GB44G
Distribution Limits
Public
Copyright
Other