DIRECT NUMERICAL SIMULATION OF RADIATION PRESSURE-DRIVEN TURBULENCE AND WINDS IN STAR CLUSTERS AND GALACTIC DISKS

The pressure exerted by the radiation of young stars may be an important feedback mechanism that drives turbulence and winds in forming star clusters and the disks of starburst galaxies. In this paper, we report a series of two-dimensional flux-limited diffusion radiation-hydrodynamics calculations...

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Bibliographic Details
Published in:The Astrophysical journal 2012-12, Vol.760 (2), p.1-20
Main Authors: KRUMHOLZ, Mark R, THOMPSON, Todd A
Format: Article
Language:English
Subjects:
APPROXIMATIONS
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COMPUTERIZED SIMULATION
COSMIC DUST
DIFFUSION
Disks
Earth, ocean, space
Exact sciences and technology
Fluid flow
Fluxes
GALAXIES
HYDRODYNAMICS
INFRARED RADIATION
Mathematical analysis
Mathematical models
RADIANT HEAT TRANSFER
RADIATION FLUX
RADIATION PRESSURE
RAYLEIGH-TAYLOR INSTABILITY
STAR CLUSTERS
STARS
STELLAR ATMOSPHERES
STELLAR WINDS
TURBULENCE
Turbulent flow
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Summary:The pressure exerted by the radiation of young stars may be an important feedback mechanism that drives turbulence and winds in forming star clusters and the disks of starburst galaxies. In this paper, we report a series of two-dimensional flux-limited diffusion radiation-hydrodynamics calculations performed with the code orion in which we drive strong radiation fluxes through columns of dusty matter confined by gravity in order to answer these questions. We consider both systems where the radiation flux is sub-Eddington throughout the gas column, and those where it is super-Eddington at the midplane but sub-Eddington in the atmosphere. However, the instability also produces a channel structure in which the radiation-matter interaction is reduced compared to time-steady analytic models because the radiation field is not fully trapped. We provide an approximation formula, appropriate for implementation in analytic models and non-radiative simulations, for the force exerted by the infrared radiation field in this regime.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637x/760/2/155