DC Field | Value | Language |
---|---|---|
dc.contributor.author | Jo, Young-Soo | ko |
dc.contributor.author | Seon, Kwang-il | ko |
dc.contributor.author | Min, Kyoung-Wook | ko |
dc.contributor.author | Edelstein, Jerry | ko |
dc.contributor.author | Wonyoung, Han | ko |
dc.contributor.author | Korpela, Eric J. | ko |
dc.contributor.author | Sirk, Martin M. | ko |
dc.date.accessioned | 2019-07-23T06:20:32Z | - |
dc.date.available | 2019-07-23T06:20:32Z | - |
dc.date.created | 2019-07-23 | - |
dc.date.created | 2019-07-23 | - |
dc.date.created | 2019-07-23 | - |
dc.date.issued | 2019-07 | - |
dc.identifier.citation | ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, v.243, no.1, pp.9 | - |
dc.identifier.issn | 0067-0049 | - |
dc.identifier.uri | http://hdl.handle.net/10203/263736 | - |
dc.description.abstract | We present all-sky maps of two major far-ultraviolet cooling lines, C IV and O VI, of highly ionized gas to investigate the nature of the transition-temperature gas. From the extinction-corrected line intensities of C IV and O VI, we calculated the gas temperature and the emission measure of the transition-temperature gas assuming isothermal plasma in the collisional ionization equilibrium. The gas temperature was found to be more or less uniform throughout the Galaxy with a value of (1.89 +/- 0.06) x 10(5) K. The emission measure of the transition-temperature gas is described well by a disk-like model in which the scale height of the electron density is z(0) = 6(-2)(+3) kpc. The total mass of the transition-temperature gas is estimated to be approximately 6.4(-2.8)(+5.2) x 10(9)M(circle dot). We also calculated the volume-filling fraction of the transition-temperature gas, which was estimated to be f = 0.26 +/- 0.09, and it varies from f similar to 0.37 in the inner Galaxy to f similar to 0.18 in the outer Galaxy. The spatial distribution of C IV and O VI cannot be explained by a simple supernova remnant model or a three-phase model. The combined effects of supernova remnants and turbulent mixing layers can explain the intensity ratio of C IV and O VI. Thermal conduction front models and high-velocity cloud models are also consistent with our observation. | - |
dc.language | English | - |
dc.publisher | IOP PUBLISHING LTD | - |
dc.title | Global Distribution of Far-ultraviolet Emissions from Highly Ionized Gas in the Milky Way | - |
dc.type | Article | - |
dc.identifier.wosid | 000473818500002 | - |
dc.type.rims | ART | - |
dc.citation.volume | 243 | - |
dc.citation.issue | 1 | - |
dc.citation.beginningpage | 9 | - |
dc.citation.publicationname | ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | - |
dc.identifier.doi | 10.3847/1538-4365/ab22ae | - |
dc.contributor.localauthor | Min, Kyoung-Wook | - |
dc.contributor.nonIdAuthor | Jo, Young-Soo | - |
dc.contributor.nonIdAuthor | Seon, Kwang-il | - |
dc.contributor.nonIdAuthor | Edelstein, Jerry | - |
dc.contributor.nonIdAuthor | Wonyoung, Han | - |
dc.contributor.nonIdAuthor | Korpela, Eric J. | - |
dc.contributor.nonIdAuthor | Sirk, Martin M. | - |
dc.description.isOpenAccess | N | - |
dc.type.journalArticle | Article | - |
dc.subject.keywordAuthor | dust, extinction | - |
dc.subject.keywordAuthor | Galaxy: evolution | - |
dc.subject.keywordAuthor | Galaxy: halo | - |
dc.subject.keywordAuthor | ISM: structure | - |
dc.subject.keywordAuthor | line: formation | - |
dc.subject.keywordAuthor | ultraviolet: ISM | - |
dc.subject.keywordPlus | LARGE-MAGELLANIC-CLOUD | - |
dc.subject.keywordPlus | X-RAY | - |
dc.subject.keywordPlus | INTERSTELLAR-MEDIUM | - |
dc.subject.keywordPlus | SUPERNOVA-REMNANTS | - |
dc.subject.keywordPlus | O-VI | - |
dc.subject.keywordPlus | ABSORPTION | - |
dc.subject.keywordPlus | HALO | - |
dc.subject.keywordPlus | EXTINCTION | - |
dc.subject.keywordPlus | EVOLUTION | - |
dc.subject.keywordPlus | IMPACT | - |
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