2010/02/03 by Enrico Camporeale, E. Camporeale, David Burgess +1 · 16 citations
Physics and Astronomy · #Anisotropy #Dust and Plasma Wave Phenomena #Electron #Electron temperature #Instability #Ionosphere and magnetosphere dynamics #Kinetic energy #Plasma #Solar and Space Plasma Dynamics #astro-ph.SR #physics.plasm-ph #physics.space-ph
paper · pdf · doi:10.1088/0004-637x/710/2/1848
published in The Astrophysical Journal 710(2), 1848-1856 (IOP Publishing) · This is an author-created, un-copyedited version of an article accepted for publication in Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The definitive publisher authenticated version is available online at DOI:10.1088/0004-637X/710/2/1848
openalex publication_date 2010/02/03 · arxiv created 2010/02/11 · arxiv updated 2010/02/26 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We perform fully kinetic particle-in-cell simulations of a hot plasma that expands radially in a cylindrical geometry. The aim of the paper is to study the consequent development of the electron temperature anisotropy in an expanding plasma flow as found in a collisionless stellar wind. Kinetic plasma theory and simulations have shown that the electron temperature anisotropy is controlled by fluctuations driven by electromagnetic kinetic instabilities. In this study, the temperature anisotropy is driven self-consistently by the expansion. While the expansion favors an increase of parallel anisotropy ( T ∥ > T ⊥ ), the onset of the fire-hose instability will tend to decrease it. We show the results for supersonic, subsonic, and static expansion flows and suggest possible applications of the results for the solar wind and other stellar winds.