2015/09/11 by Robi Banerjee, Banerjee, Robi, Bastian Körtgen +1
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph.GA
paper · pdf · doi:10.48550/arxiv.1509.03436
Invited contribution to the NIC proceedings 2016 for the John von Neumann-Institut für Computing (NIC) Symposium 2016
arxiv created 2015/09/11 · openalex publication_date 2015/09/11 · arxiv updated 2015/09/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
Molecular clouds, the birthplaces of stars in galaxies, form dynamically from the diffuse atomic gas of the interstellar medium (ISM). The ISM is also threaded by magnetic fields which have a large impact on its dynamics. In particular, star forming regions must be magnetically supercrit- ical in order to accomodate gas clumps which can collapse under their own weight. Based on a parameter study of three dimensional magneto-hydrodyamical (MHD) simulations, we show that the long-standing problem of how such supercritical regions are generated is still an open issue.