Turbulent Cooling Flows in Molecular Clouds

Details Turbulent Cooling Flows in Molecular Clouds Turbulent Cooling Flows in Molecular Clouds

1998-11-03

arxiv.org/abs/astro-ph/9811044v1

Astrophys.J. 507 (1998) L157

Astronomy and Astrophysics

Astrophysics

To appear ApJL, Nov.10, 4 ApJ style pages, Postscript

Scientific paper

10.1086/311700

We propose that inward, subsonic flows arise from the local dissipation of turbulent motions in molecular clouds. Such "turbulent cooling flows" may account for recent observations of spatially extended inward motions towards dense cores. These pressure-driven flows may arise from various types of turbulence and dissipation mechanisms. For the example of MHD waves and turbulence damped by ion-neutral friction, sustained cooling flow requires that the outer gas be sufficiently turbulent, that the inner gas have marginal field-neutral coupling, and that this coupling decrease sufficiently rapidly with increasing density. These conditions are most likely met at the transition between outer regions ionized primarily by UV photons and inner regions ionized primarily by cosmic rays. If so, turbulent cooling flows can help form dense cores, with speeds faster than expected for ambipolar diffusion. Such motions could reduce the time needed for dense core formation and could precede and enhance the motions of star-forming gravitational infall.

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