2010/06/01 by Fabio Del Sordo, Axel Brandenburg
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Astrophysics and Star Formation Studies #Solar and Space Plasma Dynamics #astro-ph.GA
paper · pdf · doi:10.1017/s1743921311017868
published as Proceedings of the International Astronomical Union, 6, pp 375-376, 2010 · 2 pages, 1 figure, to be published in Proceedings of IAU Symp. 271, Astrophysical Dynamics: from Stars to Galaxies, ed. N. Brummell and A.S. Brun, CUP
openalex publication_date 2010/06/01 · arxiv created 2011/08/18 · arxiv updated 2011/08/19 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/03
Abstract In the interstellar medium the turbulence is believed to be forced mostly through supernova explosions. In a first approximation these flows can be written as a gradient of a potential being thus devoid of vorticity. There are several mechanisms that could lead to vorticity generation, like viscosity and baroclinic terms, rotation, shear and magnetic fields, but it is not clear how effective they are, neither is it clear whether the vorticity is essential in determining the turbulent diffusion acting in the ISM. Here we present a study of the role of rotation, shear and baroclinicity in the generation of vorticity in the ISM.