Formation of Pillars at the Boundaries between H II Regions and Molecular Clouds

Details Formation of Pillars at the Boundaries between H II Regions and Molecular Clouds Formation of Pillars at the Boundaries between H II Regions and Molecular Clouds

2006-04-26

arxiv.org/abs/astro-ph/0604545v1

Astrophys.J. 647 (2006) 1151-1158

Astronomy and Astrophysics

Astrophysics

21 pages, 8 figures, accepted for publication in ApJ. high resolution figures available upon request

Scientific paper

10.1086/505458

We investigate numerically the hydrodynamic instability of an ionization front (IF) accelerating into a molecular cloud, with imposed initial perturbations of different amplitudes. When the initial amplitude is small, the imposed perturbation is completely stabilized and does not grow. When the initial perturbation amplitude is large enough, roughly the ratio of the initial amplitude to wavelength is greater than 0.02, portions of the IF temporarily separate from the molecular cloud surface, locally decreasing the ablation pressure. This causes the appearance of a large, warm HI region and triggers nonlinear dynamics of the IF. The local difference of the ablation pressure and acceleration enhances the appearance and growth of a multimode perturbation. The stabilization usually seen at the IF in the linear regimes does not work due to the mismatch of the modes of the perturbations at the cloud surface and in density in HII region above the cloud surface. Molecular pillars are observed in the late stages of the large amplitude perturbation case. The velocity gradient in the pillars is in reasonably good agreement with that observed in the Eagle Nebula. The initial perturbation is imposed in three different ways: in density, in incident photon number flux, and in the surface shape. All cases show both stabilization for a small initial perturbation and large growth of the second harmonic by increasing amplitude of the initial perturbation above a critical value.

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