Numerical Studies of Shocked Magnetic Gas Clouds - Part One

Details Numerical Studies of Shocked Magnetic Gas Clouds - Part One Numerical Studies of Shocked Magnetic Gas Clouds - Part One

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.197..699n&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 197, P. 699, 1981

Astronomy and Astrophysics

Astronomy

11

Scientific paper

A numerical technique is used for the analysis of non-steady flow fields generated by shocks in interstellar gas. The governing set of Eulerian, partial differential, equations describing the system are integrated using a finite difference scheme which is based on an extension of the fluid in cell (FLIC) method. This paper investigates the influence of large scale interstellar magnetic fields on the early evolution (time ≤ 3.0 × 106 yr) of a high density gas cloud (mass ˜700Msun.) which is hit by a strong shock wave. The incident shock is assumed a priori to be driven by a spiral density wave. Results are presented for the flow fields which develop in gaseous systems having magnetic field strengths of 0, 1 and 3 μG.

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