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Ryu, Dongsu
Astrophysics Lab
Research Interests
  • Shock waves and turbulence in clusters of galaxies
  • Origin and evolution of magnetic fields and cosmic rays in the universe
  • Plasma astrophysical phenomena in the large-scale structure of the universe

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Faraday dispersion functions of galaxies

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dc.contributor.author Ideguchi, Shinsuke ko
dc.contributor.author Tashiro, Yuichi ko
dc.contributor.author Akahori, Takuya ko
dc.contributor.author Takahashi, Keitaro ko
dc.contributor.author Ryu, Dongsu ko
dc.date.available 2014-09-04T00:38:53Z -
dc.date.created 2014-09-02 ko
dc.date.issued 2014-09 ko
dc.identifier.citation ASTROPHYSICAL JOURNAL, v.792, no.1, pp.1 - 10 ko
dc.identifier.issn 0004-637X ko
dc.identifier.uri https://scholarworks.unist.ac.kr/handle/201301/5601 -
dc.description.abstract The Faraday dispersion function (FDF), which can be derived from an observed polarization spectrum by Faraday rotation measure synthesis, is a profile of polarized emissions as a function of Faraday depth. We study intrinsic FDFs along sight lines through face-on Milky Way like galaxies by means of a sophisticated galactic model incorporating three-dimensional MHD turbulence, and investigate how much information the FDF intrinsically contains. Since the FDF reflects distributions of thermal and cosmic-ray electrons as well as magnetic fields, it has been expected that the FDF could be a new probe to examine internal structures of galaxies. We, however, find that an intrinsic FDF along a sight line through a galaxy is very complicated, depending significantly on actual configurations of turbulence. We perform 800 realizations of turbulence and find no universal shape of the FDF even if we fix the global parameters of the model. We calculate the probability distribution functions of the standard deviation, skewness, and kurtosis of FDFs and compare them for models with different global parameters. Our models predict that the presence of vertical magnetic fields and the large-scale height of cosmic-ray electrons tend to make the standard deviation relatively large. In contrast, the differences in skewness and kurtosis are relatively less significant. ko
dc.description.statementofresponsibility open -
dc.language 영어 ko
dc.publisher IOP PUBLISHING LTD ko
dc.title Faraday dispersion functions of galaxies ko
dc.type ARTICLE ko
dc.identifier.scopusid 2-s2.0-84906233259 ko
dc.identifier.wosid 000341172100051 ko
dc.type.rims ART ko
dc.description.wostc 0 *
dc.description.scopustc 0 *
dc.date.tcdate 2015-05-06 *
dc.date.scptcdate 2014-09-26 *
dc.identifier.doi 10.1088/0004-637X/792/1/51 ko
dc.identifier.url http://www.scopus.com/inward/record.url?partnerID=HzOxMe3b&scp=84906233259 ko
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