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Kwak, Kyujin
Computational Astrophysics Lab
Research Interests
  • Computational Fluid Dynamics

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The origin of the x-ray emission from the high-velocity cloud MS30.7-81.4-118

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Title
The origin of the x-ray emission from the high-velocity cloud MS30.7-81.4-118
Author
Henley, David B.Shelton, Robin L.Kwak, Kyujin
Keywords
Galaxy: halo; ISM: clouds; ISM: individual objects (MS30.7?81.4?118); X-rays: ISM
Issue Date
201408
Publisher
IOP PUBLISHING LTD
Citation
ASTROPHYSICAL JOURNAL, v.791, no.1, pp.1 - 16
Abstract
A soft X-ray enhancement has recently been reported toward the high-velocity cloud MS30.7-81.4-118 (MS30.7), a constituent of the Magellanic Stream. In order to investigate the origin of this enhancement, we have analyzed two overlapping XMM-Newton observations of this cloud. We find that the X-ray enhancement is 6′ or 100 pc across, and is concentrated to the north and west of the densest part of the cloud. We modeled the X-ray enhancement with a variety of spectral models. A single-temperature equilibrium plasma model yields a temperature of and a 0.4-2.0 keV luminosity of 7.9 × 1033 erg s-1. However, this model underpredicts the on-enhancement emission around 1 keV, which may indicate the additional presence of hotter plasma (T ≳ 107 K), or that recombination emission is important. We examined several different physical models for the origin of the X-ray enhancement. We find that turbulent mixing of cold cloud material with hot ambient material, compression or shock heating of a hot ambient medium, and charge exchange reactions between cloud atoms and ions in a hot ambient medium all lead to emission that is too faint. In addition, shock heating in a cool or warm medium leads to emission that is too soft (for reasonable cloud speeds). We find that magnetic reconnection could plausibly power the observed X-ray emission, but resistive magnetohydrodynamical simulations are needed to test this hypothesis. If magnetic reconnection is responsible for the X-ray enhancement, the observed spectral properties could potentially constrain the magnetic field in the vicinity of the Magellanic Stream.
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DOI
http://dx.doi.org/10.1088/0004-637X/791/1/41
ISSN
0004-637X
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SNS_Journal Papers
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