Time-dependent galactic winds

2012/02/14 by E. A. Dorfi, D. Breitschwerdt
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Galaxies: Formation, Evolution, Phenomena #Solar and Space Plasma Dynamics #astro-ph.GA #astro-ph.HE #msc:85-08

paper · pdf · doi:10.1051/0004-6361/201118082

published as 2012A&A...540A..77D · 15 pages, 7 figures

openalex publication_date 2012/02/14 · arxiv created 2013/04/04 · arxiv updated 2013/04/05 · openalex created_date 2022/10/04 · openalex updated_date 2026/07/28

Abstract

Context. Cosmic rays (CRs) are transported out of the galaxy by diffusion and advection due to streaming along magnetic field lines and resonant scattering off self-excited MHD waves. Thus momentum is transferred to the plasma via the frozen-in waves as a mediator assisting the thermal pressure in driving a galactic wind.

Citations

• The Contribution of Population III to the Enrichment and Preheating of the Intracluster Medium
• Direct simulations of a supernova-driven galactic dynamo
• Dynamics of the Interplanetary Gas and Magnetic Fields.
• Particle acceleration at astrophysical shocks: A theory of cosmic ray origin