ANGEO Annales Geophysicae ANGEO Ann. Geophys. 1432-0576 Copernicus Publications Göttingen, Germany 10.5194/angeo-29-1071-2011 Hybrid models of solar wind plasma heating Ofman L. 1 2 4 Viñas A.-F. 2 Moya P. S. 3 Department of Physics, The Catholic University of America, Washington, D.C. 20064, USA NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Departamento de Fisica, Facultad de Ciencias, Universidad de Chile, Las Palmeras 3425, Casilla 653, Santiago, Chile visiting: Dept. of Geophysics and Planetary Sciences, Tel Aviv University, Tel Aviv, Israel 20 06 2011 29 6 1071 1079 Copyright: © 2011 L. Ofman et al. 2011 This work is licensed under the Creative Commons Attribution 3.0 Unported License. To view a copy of this licence, visit https://creativecommons.org/licenses/by/3.0/ This article is available from https://angeo.copernicus.org/articles/29/1071/2011/angeo-29-1071-2011.html The full text article is available as a PDF file from https://angeo.copernicus.org/articles/29/1071/2011/angeo-29-1071-2011.pdf

Remote sensing and in-situ observations show that solar wind ions are often hotter than electrons, and the heavy ions flow faster than the protons by up to an Alfvén speed. Turbulent spectrum of Alfvénic fluctuations and shocks were detected in solar wind plasma. Cross-field inhomogeneities in the corona were observed to extend to several tens of solar radii from the Sun. The acceleration and heating of solar wind plasma is studied via 1-D and 2-D hybrid simulations. The models describe the kinetics of protons and heavy ions, and electrons are treated as neutralizing fluid.The expansion of the solar wind is considered in 1-D hybrid model. A spectrum of Alfvénic fluctuations is injected at the computational boundary, produced by differential streaming instability, or initial ion temperature anisotropy, and the parametric dependence of the perpendicular heating of H<sup>+</sup>-He<sup>++</sup> solar wind plasma is studied. It is found that He<sup>++</sup> ions are heated efficiently by the Alfvénic wave spectrum below the proton gyroperiod.

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