Quasilinear Evolution and Perpendicular Ion Heating in the Turbulent Solar Wind*

Details Quasilinear Evolution and Perpendicular Ion Heating in the Turbulent Solar Wind* Quasilinear Evolution and Perpendicular Ion Heating in the Turbulent Solar Wind*

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43c1967r&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH43C-1967

Physics

Plasma Physics

[2164] Interplanetary Physics / Solar Wind Plasma, [7863] Space Plasma Physics / Turbulence

Scientific paper

The measured spectrum of kinetic Alfven wave (KAW) fluctuations in the turbulent solar wind plasma is used to calculate the electron and ion distribution functions resulting from quasi-linear diffusion. Quasi-linear diffusion establishes a step-like profile on the distribution function over parallel velocity [1]. The size of "plateau" vme/vte~0.5 , which can be created within the time of travel of solar wind plasma to the Earth ~ 10^5 s, is estimated for electrons as , while for ions vmi/vti~3. In this case the evolution of the ion tail distribution function can be approximated as ftail~exp(-vz^7/vmi^7). As a result, the Landau damping of KAW and whistlers in the high beta solar wind plasma is strongly diminished. Also the ion tail distribution function is found to be unstable to electromagnetic ion cyclotron (EMIC) waves [2]. These waves pitch angle scatter the parallel component of the ion velocity into the perpendicular velocity. With less than 1% of turbulent magnetic field energy in EMIC waves the perpendicular ion heating can be possible. [1] L. Rudakov et. al., Phys. Plasma, 18, 012307 (2011). [2] L. Rudakov et. al., arxiv.org:physics.plasm-ph:1012.2398v2, (2011b). * Supported by ONR.

Affiliated with

Also associated with

No associations

Rating

Quasilinear Evolution and Perpendicular Ion Heating in the Turbulent Solar Wind* does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Quasilinear Evolution and Perpendicular Ion Heating in the Turbulent Solar Wind*, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Quasilinear Evolution and Perpendicular Ion Heating in the Turbulent Solar Wind* will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-879850