Structure and Stability of Phase Transition Layers in the Interstellar Medium

Details Structure and Stability of Phase Transition Layers in the Interstellar Medium Structure and Stability of Phase Transition Layers in the Interstellar Medium

2006-04-27

arxiv.org/abs/astro-ph/0604564v2

Astrophys.J.652:1331-1338,2006

Astronomy and Astrophysics

Astrophysics

19 pages, 9 figures, accepted for publication in the Astrophysical Journal

Scientific paper

10.1086/508334

We analyze the structure and stability of the transition layer (or front) that connects the cold neutral medium and warm neutral medium in the plane-parallel geometry. Such fronts appear in recent numerical simulations of a thermally bistable interstellar medium. The front becomes an evaporation or condensation front depending on the surrounding pressure. The stability analysis is performed in both long- and short-wavelength approximations. We find that the plane-parallel evaporation front is unstable under corrugational deformations, whereas the condensation front seems to be stable. The instability is analogous to the Darrieus-Landau instability in combustion front. The growth rate of the instability is proportional to the speed of the evaporation flow and the corrugation wavenumber for modes with wavelength much longer than the thickness of the front, and it is suppressed at scales approximately equal to the thickness of the front. The timescale of the instability is smaller than the cooling timescale of the warm neutral medium ($\sim 1$ Myr), and can be as small as the cooling timescale of the cold neutral medium ($\sim 0.01-0.1$ Myr). Thus, this instability should be one of the processes for driving the interstellar turbulence.

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