Proton core-beam system in the expanding solar wind: Hybrid simulations

Details Proton core-beam system in the expanding solar wind: Hybrid simulations Proton core-beam system in the expanding solar wind: Hybrid simulations

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011jgra..11611101h&link_type=abstract

Journal of Geophysical Research, Volume 116, Issue A11, CiteID A11101

Physics

Plasma Physics

1

Interplanetary Physics: Plasma Waves And Turbulence, Interplanetary Physics: Solar Wind Plasma, Space Plasma Physics: Kinetic And Mhd Theory, Space Plasma Physics: Kinetic Waves And Instabilities, Space Plasma Physics: Mathematical And Numerical Techniques (0500, 3200)

Scientific paper

Results of a two-dimensional hybrid expanding box simulation of a proton beam-core system in the solar wind are presented. The expansion with a strictly radial magnetic field leads to a decrease of the ratio between the proton perpendicular and parallel temperatures as well as to an increase of the ratio between the beam-core differential velocity and the local Alfvén velocity creating a free energy for many different instabilities. The system is indeed most of the time marginally stable with respect to the parallel magnetosonic, oblique Alfvén, proton cyclotron and parallel fire hose instabilities which determine the system evolution counteracting some effects of the expansion and interacting with each other. Nonlinear evolution of these instabilities leads to large modifications of the proton velocity distribution function. The beam and core protons are slowed with respect to each other and heated, and at later stages of the evolution the two populations are not clearly distinguishable. On the macroscopic level the instabilities cause large departures from the double adiabatic prediction leading to an efficient isotropization of effective proton temperatures in agreement with Helios observations.

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