Analysis of Hydrodynamic Instabilities at Photoevaporation Fronts in Astrophysical Settings*

Details Analysis of Hydrodynamic Instabilities at Photoevaporation Fronts in Astrophysical Settings* Analysis of Hydrodynamic Instabilities at Photoevaporation Fronts in Astrophysical Settings*

Nov 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aps..dpp.r8q09r&link_type=abstract

American Physical Society, Division of Plasma Physics Meeting, November 16-20, 1998 New Orleans, LA, abstract #R8Q.09

Physics

Plasma Physics

Scientific paper

Molecular clouds situated near bright newborn stars are exposed to intense fluxes of ionizing radiation. In particular, the spectacular Eagle Nebula belongs to this class of objects. Photoionization of the gas produces an intense ablative flow from the surface of the cloud and the acceleration of the cloud material in the opposite direction, a situation where hydrodynamic instabilities such as the Rayleigh-Taylor (RT) and Richtmyer-Meshkov (RM) instabilities may develop.[L. Spitzer. ApJ 120, 1 (1954).]. New observational data from the Hubble Space Telescope warrants revisiting the question of whether features in the Eagle nebule might be caused by hydrodynamic instabilities.[ J.J. Hester et al. AJ 111, 2348 (1996); M.W. Pound. ApJ 493, L113 (1998); J.M. Stone, J. Xu, and L.G. Mundy, Nature 377, 315 (1995).] We will discuss the effects of initial density non-uniformities, compressibility, shocks, variations of the ionizing flux in time and space, ablative stabilization, and possible ``fire-polishing". *Work performed under the auspices of the U.S. Department of Energy by the Lawrence Livermore National Laboratory under Contract W-7405-ENG-48.

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