{ "id": "1909.07738", "version": "v1", "published": "2019-09-17T12:03:25.000Z", "updated": "2019-09-17T12:03:25.000Z", "title": "C-type shock modelling -- the effect of new H$_2$-H collisional rate coefficients", "authors": [ "A. V. Nesterenok", "D. Bossion", "Y. Scribano", "F. Lique" ], "comment": "10 pages, 4 figures, accepted for publication in MNRAS", "doi": "10.1093/mnras/stz2441", "categories": [ "astro-ph.GA" ], "abstract": "We consider collisional excitation of H$_2$ molecules in C-type shocks propagating in dense molecular clouds. New data on collisional rate coefficients for (de-)excitation of H$_2$ molecule in collisions with H atoms and new H$_2$ dissociation rates are used. The new H$_2$-H collisional data are state of the art and are based on the most accurate H$_3$ potential energy surface. We re-examine the excitation of rotational levels of H$_2$ molecule, the para-to-ortho-H$_2$ conversion, and H$_2$ dissociation by H$_2$-H collisions. At cosmic ray ionization rates $\\zeta \\geq 10^{-16}$ s$^{-1}$ and at moderate shock speeds, the H/H$_2$ ratio at the shock front is mainly determined by the cosmic ray ionization rate. The H$_2$-H collisions play the main role in the para-to-ortho-H$_2$ conversion and, at $\\zeta \\geq 10^{-15}$ s$^{-1}$, in the excitation of vibrationally excited states of H$_2$ molecule in the shock. The H$_2$ ortho-to-para ratio (OPR) of the shocked gas and column densities of rotational levels of vibrationally excited states of H$_2$ are found to depend strongly on the cosmic ray ionization rate. We discuss the applicability of the presented results to interpretation of observations of H$_2$ emission in supernova remnants.", "revisions": [ { "version": "v1", "updated": "2019-09-17T12:03:25.000Z" } ], "analyses": { "keywords": [ "collisional rate coefficients", "cosmic ray ionization rate", "c-type shock modelling", "rotational levels", "vibrationally excited states" ], "tags": [ "journal article" ], "note": { "typesetting": "TeX", "pages": 10, "language": "en", "license": "arXiv", "status": "editable" } } }