Shock propagation and the generation of magnetohydrodynamic wave fields in inhomogeneous molecular clouds

Details Shock propagation and the generation of magnetohydrodynamic wave fields in inhomogeneous molecular clouds Shock propagation and the generation of magnetohydrodynamic wave fields in inhomogeneous molecular clouds

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...432..622m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 432, no. 2, p. 622-640

Other

13

Interstellar Matter, Magnetohydrodynamic Waves, Molecular Clouds, Shock Wave Generators, Shock Wave Interaction, Shock Wave Propagation, Star Formation, Kinetic Energy, Mach Number, Magnetic Fields, Shock Waves, Wave Generation

Scientific paper

We develop a simple one-dimensional model for the interaction of a steady, thin, planar shock wave with a nonrigid cloud which may be in motion relative to the surrounding medium, and we apply the model to shocks impinging on, and propagating through, molecular clouds. Both 'adiabatic' (gamma = 5/3) and radiative (gamma = 1) shocks are considered and we allow for the presence of a uniform magnetic field directed either parallel or perpendicular to the shock normal. The former field orientation is equivalent to the hydrodynamic case, and the latter involves only fast MHD shocks. We focus on the manner in which such shocks can generate internal kinetic motions in the cloud on a range of size and density scales through the direct acceleration of cores and clumps by shocks transmitted into them and through the generation of an MHD wavefield via the reflection of the incident shock at clump boundaries. We find that stronger incident Mach numbers and smaller density contrasts lead to more efficient cloud acceleration, as do isothermal intercloud shocks and small intercloud magnetic field strengths. The acceleration efficiency is insensitive to the adiabatic index and the magnetic field strength in the cloud itself. For typical parameter choices, the direct acceleration of clouds and clumps by strong shocks is found to be substantial and could at least in part account for their observed velocity dispersions. If the shocks are moderately weak, the final velocity of the cloud is linearly related to its initial velocity, with higher acceleration giving shallower slopes (i.e., final velocity distributions which are less sensitive to the initial distribution). Compared to the kinetic energy of the postshock cloud, the energy given to the wavefield at each encounter is small, and the heating of the interclump medium by the dissipation of this wavefield is found to be insufficient to balance the cooling rate in the cloud as a whole (although it may be important in particular regions), even if this medium is warm, unless it is also extremely tenuous (n approximately less than 0.1/cu cm). Nevertheless, the correction for the velocity imparted to the cloud leads to a substantial increase in the critical incident Mach number for wave emission over that reported by Spitzer for the rigid case. The implications of our model for shock-induced star formation are discussed briefly.

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