Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...321..321w&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 321, Oct. 1, 1987, p. 321-333.
Astronomy and Astrophysics
Astrophysics
26
Astronomical Models, Interstellar Gas, Magnetohydrodynamic Waves, Molecular Clouds, Oblique Shock Waves, Transonic Flow, Wave Propagation
Scientific paper
The structure of oblique steady plane-parallel radiative reacting C-type shocks in diffuse molecular clouds is examined. Numerical models are presented for typical parameters: n(H2) = 20/cu cm, n(H) = 10/cu cm, and v(s) = 10 km/s. C-type shock structure is weakly dependent on the angle (theta) between the upstream magnetic field B0 and the direction of shock propagation. For typical field strengths there is a critical angle below which the neutral flow must have at least one critical point (implying that the shock must be either transonic C-type or J-type), although in general this angle need not exist. Models differing only in the component of B0 parallel to the direction of shock propagation (i.e., having identical transverse components of B0) can have markedly different hydrodynamic structures. The column densities of most shock-produced species vary only mildly with theta between 90 and 40 deg when either B0 or B0 sin theta are held constant.
Draine Bruce T.
Wardle Mark
No associations
LandOfFree
Oblique magnetohydrodynamic shock waves in molecular clouds does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Oblique magnetohydrodynamic shock waves in molecular clouds, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Oblique magnetohydrodynamic shock waves in molecular clouds will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1773536