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DC Field | Value | Language |
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dc.citation.number | 1 | - |
dc.citation.startPage | 41 | - |
dc.citation.title | ASTROPHYSICAL JOURNAL | - |
dc.citation.volume | 791 | - |
dc.contributor.author | Henley, David B. | - |
dc.contributor.author | Shelton, Robin L. | - |
dc.contributor.author | Kwak, Kyujin | - |
dc.date.accessioned | 2023-12-22T02:16:51Z | - |
dc.date.available | 2023-12-22T02:16:51Z | - |
dc.date.created | 2014-09-15 | - |
dc.date.issued | 2014-08 | - |
dc.description.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. | - |
dc.identifier.bibliographicCitation | ASTROPHYSICAL JOURNAL, v.791, no.1, pp.41 | - |
dc.identifier.doi | 10.1088/0004-637X/791/1/41 | - |
dc.identifier.issn | 0004-637X | - |
dc.identifier.scopusid | 2-s2.0-84905258909 | - |
dc.identifier.uri | https://scholarworks.unist.ac.kr/handle/201301/5961 | - |
dc.identifier.url | http://www.scopus.com/inward/record.url?partnerID=HzOxMe3b&scp=84905258909 | - |
dc.identifier.wosid | 000339657700041 | - |
dc.language | 영어 | - |
dc.publisher | IOP PUBLISHING LTD | - |
dc.title | The origin of the x-ray emission from the high-velocity cloud MS30.7-81.4-118 | - |
dc.type | Article | - |
dc.description.isOpenAccess | FALSE | - |
dc.relation.journalWebOfScienceCategory | Astronomy & Astrophysics | - |
dc.relation.journalResearchArea | Astronomy & Astrophysics | - |
dc.description.journalRegisteredClass | scie | - |
dc.description.journalRegisteredClass | scopus | - |
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