Stability of Small-Scale Kelvin-Helmholtz Instability for Two-Component Protogalaxies

Details Stability of Small-Scale Kelvin-Helmholtz Instability for Two-Component Protogalaxies Stability of Small-Scale Kelvin-Helmholtz Instability for Two-Component Protogalaxies

Oct 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...506..289k&link_type=abstract

The Astrophysical Journal, Volume 506, Issue 1, pp. 289-291.

Astronomy and Astrophysics

Astronomy

6

Galaxy: Formation, Galaxy: Globular Clusters: General, Instabilities, Ism: Clouds, Ism: General, Ism: Structure

Scientific paper

When one examines the dynamic stability of a cold cloud in diffuse warm (or hot) phase gas, Kelvin-Helmholtz instability (KHI) is always considerable when there is relative motion between the two components. In this paper I discuss a stability condition of KHI on the boundary between the components, where we always expect evaporation of the cold, denser component (cloud) and/or condensation of the more diffuse component (diffuse warm or hot phase gas). I define a phase transition layer that occurs under these conditions, the thickness of which is estimated from the balance between the thermal conduction and the radiative cooling. That is, the thickness is defined as the Field length. At the phase transition layer, both the components exchange momentum with each other and the velocity field becomes continuous. When these events occur, KHIs with a wavelength shorter than the width of the layer are stabilized. Our two key findings are that (1) the Field length corresponds to the size of the phase transition layer and (2) that it is impossible for a typical proto-globular cluster cloud to be affected by small-scale KHI since its Field length is comparable to the cloud's size.

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