Nonlinear alfven waves in high speed solar wind streams

Journal Article · Tue Feb 01 04:00:00 EST 1977 · J. Geophys. Res.; (United States)

DOI:https://doi.org/10.1029/JA082i004p00618· OSTI ID:5085901

Abraham-Shrauner, B; Feldman, W C

A nonlinear proton distribution function that is an exact stationary solution of the nonlinear Vlasov equation and Maxwell's equations and which supports a single nonlinear transverse Alfven (ion cyclotron) wave that is circularly polarized and nondispersive is proposed for most of the observations during high speed solar wind streams. This nonlinear distribution removes the strong Alfven wave instability, inconsistent with the persistence of the observed proton distribution functions in high speed streams, found by the linear stability analysis. Model temperature anisotropies and drift velocities of the two spatially inhomogeneous bi-Maxwellian components are consistent with typical proton velocity distributions measured in high speed streams at 1 AU. Two derived relations for each of the wave number and the phase velocity of the wave are obeyed within experimental uncertainties by two typical proton measurements. The model also predicts that the alpha particle bulk flow velocity exceeds the proton particle bulk flow velocity, as is observed.

• Research Organization: Los Alamos Scientific Lab., NM
• OSTI ID: 5085901
• Journal Information: J. Geophys. Res.; (United States), Journal Name: J. Geophys. Res.; (United States) Vol. 82:4; ISSN JGREA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ALFVEN WAVES
ANISOTROPY
BARYONS
BOLTZMANN-VLASOV EQUATION
DIFFERENTIAL EQUATIONS
DISTRIBUTION FUNCTIONS
ELEMENTARY PARTICLES
EQUATIONS
FERMIONS
FLUID FLOW
GAS FLOW
HADRONS
HYDROMAGNETIC WAVES
MAXWELL EQUATIONS
NONLINEAR PROBLEMS
NUCLEONS
PHASE VELOCITY
PROTONS
RADIATION STREAMING
RADIATIONS
SOLAR ACTIVITY
SOLAR PARTICLES
SOLAR PROTONS
SOLAR RADIATION
SOLAR WIND
STABILITY
STELLAR RADIATION
TEMPERATURE DEPENDENCE
VELOCITY