The gravitational stability of a compressed slab of gas

Abstract

We consider the linear stability of an isothermal, pressure-bounded, self-gravitating gas slab. such a configuration if unstable at sufficiently long wavelengths and grows at rate ~ squre root G*rho, where rho is the density of the gas slab, but at high external pressure the nature of this instability is quite different from that of the usual Jeans instability. We develop an analytical model that reproduces the behaviour of the instability found numerically by Elmegreen & Elmegreen. They found, surprisingly, that the critical wavenumber for the onset of the instability is always of the order of the layer thickness, independently of the level of self-gravity and the external pressure. For high external pressure, the instability is due to a neutral mode that exists bucause external pressure can hold the layer, which attains nearly constant density pressure, to any distorted shape. In this case, the unstable mode is neither a p-mode nor a g-mode, and has a curl-free and divergence-free velocity field. In the linear regime, the main effect of the instability is to distort the shape of the stability of the shocked gas layer that results from the supersonic head-on collision of identical clouds. We conclude that dynamical instabilities within the shocked layer do not substantially enhance star formation when the layer is (ram) pressure-confined.