Magnetic fields and radiative shocks in protogalaxies and the origin of globular clusters

Details Magnetic fields and radiative shocks in protogalaxies and the origin of globular clusters Magnetic fields and radiative shocks in protogalaxies and the origin of globular clusters

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...389..269s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 389, April 10, 1992, p. 269-285. Research supported by Robert A. Welch Foun

Astronomy and Astrophysics

Astrophysics

7

Galactic Evolution, Globular Clusters, Interstellar Gas, Interstellar Magnetic Fields, Magnetohydrodynamic Waves, Shock Wave Interaction, Active Galactic Nuclei, Conservation Equations, Gravitational Fields, Magnetic Effects, Radiative Transfer, Thermal Instability, Ultraviolet Radiation

Scientific paper

The paper examines the hypothesis that globular clusters formed from gravitational instability in dense sheets of gas produced behind radiative shocks inside protogalaxies, such as those produced by the collision of subgalactic mass fragments partaking of the virial motions within the protogalaxy, in order to determine the differences which result if a magnetic field is present in the preshock medium. The MHD conservation equations are solved along with rate equations for nonequilibrium ionization, recombination, molecular formation and dissociation, and the equations of radiative transfer for steady-state shocks of velocity 300 km/s in a gas of preshock densities of 0.1-1 cu cm, and magnetic field strengths of 0.1-6 micro-G. The magnetic field is found to limit the degree of postshock compression and, thereby, to reduce the level of external radiation flux required to suppress H2 formation and cooling.

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