Hybrid simulations of the expanding solar wind: Temperatures and drift velocities

Details Hybrid simulations of the expanding solar wind: Temperatures and drift velocities Hybrid simulations of the expanding solar wind: Temperatures and drift velocities

Mar 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003georl..30e..15h&link_type=abstract

Geophysical Research Letters, Volume 30, Issue 5, pp. 15-1, CiteID 1211, DOI 10.1029/2002GL016409

Physics

Plasma Physics

9

Interplanetary Physics: Solar Wind Plasma, Interplanetary Physics: Plasma Waves And Turbulence, Space Plasma Physics: Numerical Simulation Studies, Space Plasma Physics: Waves And Instabilities, Space Plasma Physics: Wave/Wave Interactions

Scientific paper

We study the evolution of the expanding solar wind using a one-dimensional and a two-dimensional expanding box model [Grappin et al., 1993] implemented here within a hybrid code [Liewer et al., 2001]. We first consider a plasma with protons and 5% of alpha particles, without drift between the protons and alphas, considering successively the low-beta and high-beta cases. Then we consider a strong drift between protons and alphas, again separately the low-beta and high-beta case. Without drift, the evolution of the low-beta plasma is adiabatic. In the high-beta plasma without drift, the fire hose instabilities (both parallel and oblique) disrupt the adiabatic evolution. Finally, with a drift, the adiabatic evolution is stopped by the oblique Alfvén instability and the parallel magnetosonic instability for low-beta plasma and for high-beta plasma, respectively. The two instabilities slow down thealphas and heat alphas and protons.

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