A computer program for calculating the structure of magnetohydrodynamical shocks in interstellar clouds

Published: 1 January 1990| Version 1 | DOI: 10.17632/2653cn4wxz.1
L. Heck, D.R. Flower, G. Pineau Des Forêts


Abstract The program solves for the stationary-state profile of a shock propagating in the interstellar medium under the influence of a magnetic field. The number densities of a given set of atomic and molecular species are computed point by point through the shock. Heavy molecules of the polycyclic aromatic hydrocarbon type, for example, may be included amongst the molecular species. Title of program: MHD Catalogue Id: ABLS_v1_0 Nature of problem Shocks are known to be generated in the interstellar medium, for example, in regions of star formation. The structure of the shocks is modified by the interstellar magnetic field. The continuous or C-type shocks which are anticipated in such regions change the physical and chemical state of the gas. Chemical changes to the degree of ionization impinge, in turn, on the shock structure, and so the magnetohydrodynamical (MHD) and chemical rate equations need to be solved simultaneously. The column ... Versions of this program held in the CPC repository in Mendeley Data ABLS_v1_0; MHD; 10.1016/0010-4655(90)90143-O This program has been imported from the CPC Program Library held at Queen's University Belfast (1969-2019)



Astronomy, Astrophysics, Computational Physics