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곽규진

Kwak, Kyujin
Computational Astrophysics Lab.
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dc.citation.endPage 14 -
dc.citation.number 2 -
dc.citation.startPage 1 -
dc.citation.title ASTROPHYSICAL JOURNAL -
dc.citation.volume 751 -
dc.contributor.author Shelton, R. L. -
dc.contributor.author Kwak, Kyujin -
dc.contributor.author Henley, D. B. -
dc.date.accessioned 2023-12-22T05:07:52Z -
dc.date.available 2023-12-22T05:07:52Z -
dc.date.created 2014-11-12 -
dc.date.issued 2012-06 -
dc.description.abstract With the goal of understanding why X-rays have been reported near some high-velocity clouds, we perform detailed three-dimensional hydrodynamic and magnetohydrodynamic simulations of clouds interacting with environmental gas like that in the Galaxy's thick disk/halo or the Magellanic Stream. We examine two scenarios. In the first, clouds travel fast enough to shock heat warm environmental gas. In this scenario, the X-ray productivity depends strongly on the speed of the cloud and the radiative cooling rate. In order to shock heat environmental gas to temperatures of ≥106K, cloud speeds of ≥300 kms-1 are required. If cooling is quenched, then the shock-heated ambient gas is X-ray emissive, producing bright X-rays in the 1/4keV band and some X-rays in the 3/4keV band due to O VII and other ions. If, in contrast, the radiative cooling rate is similar to that of collisional ionizational equilibrium plasma with solar abundances, then the shocked gas is only mildly bright and for only about 1Myr. The predicted count rates for the non-radiative case are bright enough to explain the count rate observed with XMM-Newton toward a Magellanic Stream cloud and some enhancement in the ROSAT 1/4keV count rate toward Complex C, while the predicted count rates for the fully radiative case are not. In the second scenario, the clouds travel through and mix with hot ambient gas. The mixed zone can contain hot gas, but the hot portion of the mixed gas is not as bright as those from the shock-heating scenario. -
dc.identifier.bibliographicCitation ASTROPHYSICAL JOURNAL, v.751, no.2, pp.1 - 14 -
dc.identifier.doi 10.1088/0004-637X/751/2/120 -
dc.identifier.issn 0004-637X -
dc.identifier.scopusid 2-s2.0-84861144773 -
dc.identifier.uri https://scholarworks.unist.ac.kr/handle/201301/8683 -
dc.identifier.url http://www.scopus.com/inward/record.url?partnerID=HzOxMe3b&scp=84861144773 -
dc.identifier.wosid 000304204600041 -
dc.language 영어 -
dc.publisher IOP PUBLISHING LTD -
dc.title MODELING THE X-RAYS RESULTING FROM HIGH-VELOCITY CLOUDS -
dc.type Article -
dc.description.journalRegisteredClass scie -
dc.description.journalRegisteredClass scopus -
dc.subject.keywordAuthor galaxies: ISM -
dc.subject.keywordAuthor Galaxy: halo -
dc.subject.keywordAuthor ISM: clouds -
dc.subject.keywordAuthor ISM: kinematics and dynamics -
dc.subject.keywordAuthor methods: numerical -
dc.subject.keywordAuthor X-rays: ISM -
dc.subject.keywordPlus TURBULENT MIXING LAYERS -
dc.subject.keywordPlus GALACTIC HALO -
dc.subject.keywordPlus COMPLEX-C -
dc.subject.keywordPlus MAGELLANIC STREAM -
dc.subject.keywordPlus INTERSTELLAR-MEDIUM -
dc.subject.keywordPlus IONIZED-GAS -
dc.subject.keywordPlus HOT PLASMA -
dc.subject.keywordPlus MILKY-WAY -
dc.subject.keywordPlus IONIZATION -
dc.subject.keywordPlus ORIGIN -

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