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Kwak, Kyujin
Computational Astrophysics Lab
Research Interests
  • Computational Fluid Dynamics
  • Astrophysical and Laboratory Plasma
  • Hydrodynamics with Radiation
  • Nuclear, Atomic, and Molecular Reactions

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SIMULATIONS OF HIGH-VELOCITY CLOUDS. II. ABLATION FROM HIGH-VELOCITY CLOUDS AS A SOURCE OF LOW-VELOCITY HIGH IONS

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Title
SIMULATIONS OF HIGH-VELOCITY CLOUDS. II. ABLATION FROM HIGH-VELOCITY CLOUDS AS A SOURCE OF LOW-VELOCITY HIGH IONS
Author
Henley, David B.Kwak, KyujinShelton, Robin L.
Keywords
Galaxy: halo; hydrodynamics; ISM: clouds; methods: numerical; ultraviolet: ISM
Issue Date
2012-07
Publisher
IOP PUBLISHING LTD
Citation
ASTROPHYSICAL JOURNAL, v.753, no.1, pp.1 - 16
Abstract
In order to determine if the material ablated from high-velocity clouds (HVCs) is a significant source of low-velocity high ions (C IV, N V, and O VI) such as those found in the Galactic halo, we simulate the hydrodynamics of the gas and the time-dependent ionization evolution of its carbon, nitrogen, and oxygen ions. Our suite of simulations examines the ablation of warm material from clouds of various sizes, densities, and velocities as they pass through the hot Galactic halo. The ablated material mixes with the environmental gas, producing an intermediate-temperature mixture that is rich in high ions and that slows to the speed of the surrounding gas. We find that the slow mixed material is a significant source of the low-velocity O VI that is observed in the halo, as it can account for at least 1/3 of the observed O VI column density. Hence, any complete model of the high ions in the halo should include the contribution to the O VI from ablated HVC material. However, such material is unlikely to be a major source of the observed C IV, presumably because the observed C IV is affected by photoionization, which our models do not include. We discuss a composite model that includes contributions from HVCs, supernova remnants, a cooling Galactic fountain, and photoionization by an external radiation field. By design, this model matches the observed O VI column density. This model can also account for most or all of the observed C IV, but only half of the observed N V.
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DOI
10.1088/0004-637X/753/1/58
ISSN
0004-637X
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PHY_Journal Papers
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