Kinematical and Dynamical Approaches to Gravitational Instability

Details Kinematical and Dynamical Approaches to Gravitational Instability Kinematical and Dynamical Approaches to Gravitational Instability

1993-09-16

arxiv.org/abs/astro-ph/9309024v1

Astronomy and Astrophysics

Astrophysics

10 pages, uuencoded compressed postscript, 1 figure included, preprint numbers IASSNS-AST 93/57 and MIT-CSR-93-21

Scientific paper

This paper reviews the essential physics of gravitational instability in a Robertson-Walker background spacetime. Three approaches are presented in a pedagogical manner, based on (1) the Eulerian fluid equations, (2) the Lagrangian description of trajectories, and (3) the Lagrangian fluid equations. Linear and nonlinear limits are discussed for each case. Shear and tides are shown to play a key role in nonlinear gravitational instability. The Lagrangian fluid approach is used to show that several widely held beliefs about gravitational instability are false. The following collapse theorem is proven: for a given initial density fluctuation and growth rate, the spherical tophat perturbation collapses more slowly than any other configuration. We also show that density maxima are not the first points to collapse and that underdense regions may collapse if their initial shear is sufficiently high. The Lagrangian fluid approach leads to an almost closed set of local evolution equations for individual mass elements. The magnetic part of the Weyl tensor, which may be present even in the nonrelativistic (Newtonian) limit, may prevent a purely local description. However, neglecting the magnetic part of the Weyl tensor, we obtain predictions for high-redshift collapse that are in good agreement with a high-resolution cold dark matter N-body simulation.

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