Gravitational Fragmentation of Expanding Shells. II. Three-dimensional Simulations

Abstract

We investigate the gravitational fragmentation of expanding shells driven by HII regions using the three-dimensional Lagrangian simulation codes based on the Riemann solver, called Godunov smoothed particle hydrodynamics. The ambient gas is assumed to be uniform. In order to attain high resolution to resolve the geometrically thin dense shell, we calculate not the whole but a part of the shell. We find that perturbations begin to grow earlier than the prediction of the linear analysis under the thin-shell approximation. The wavenumber of the most unstable mode is larger than that in the thin-shell linear analysis. The development of the gravitational instability is accompanied by the significant deformation of the contact discontinuity. These results are consistent with a linear analysis presented by Iwasaki et al. (2011) that have taken into account the density profile across the thickness and approximate shock and contact discontinuity boundary conditions. We derive useful analytic formulae for the fragment scale and the epoch when the gravitational instability begins to grow.

12 pages, 14 figures, to be published in the Astrophysical Journal

References in corpus (4)

• Ionisation-induced star formation I: The collect and collapse model
• The fragmentation of expanding shells II: Thickness matters
• Gravitational Fragmentation of Expanding Shells. II. Three-dimensional Simulations
• Trapping of the HII and Photodissociation Region in a Radially Stratified Molecular Cloud

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