Interface Instabilities in the Interstellar Medium

Details Interface Instabilities in the Interstellar Medium Interface Instabilities in the Interstellar Medium

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995nyasa.773...32h&link_type=abstract

Waves in Astrophysics, vol. Volume 773, p. 32-43

Astronomy and Astrophysics

Astrophysics

Interstellar Matter, Kelvin-Helmholtz Instability, Star Formation, Velocity Distribution, Stellar Gravitation, Temperature Effects, Vortices, Gas Streams, Perturbation, Gravitational Binding Energy, Supersonic Flow, Turbulence, Shock Wave Propagation

Scientific paper

In the present communication, we reexamine two limiting cases of star-forming mechanisms involving self-gravity, thermodynamics, and velocity fields, that we believe must be ubiquitous in the ISM -- the generally oblique collision of supersonic gas streams or turbulent eddies. The general case of oblique collisions has not yet been examined. However, two limiting cases have been studied in detail: (1) The head-on collision of two identical gas streams that form dense, cool accretion shocks that become unstable and may form Jeans mass clouds, which subsequently undergo collapse. (2) Linearly unstable tangential velocity discontinuities, which result in Kelvin-Helmholtz (K-H) instabilities and related phenomena. The compressible K-H instabilities exhibit rich and unexpected behaviors. Moreover a new thermal-dynamic (T-D) mode was discovered that arises from the coupling of the perturbed thermal behavior and the unperturbed flow. The T-D mode has the curious characteristic that it may be strongly unstable to interface modes when the global modes in either medium are absolutely thermally stable. In the present communication additional models of case 1 are described and discussed, and self-gravity is added in the linear theory of tangential discontinuities, case 2. We prove that self-gravity fundamentally changes the behavior of interfacial modes -- density discontinuities (or steps) are inherently unstable on roughly the free-fall timescale of the denser medium to perturbations of all wavelengths.

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