Full metadata record
DC Field | Value | Language |
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dc.citation.number | 2 | - |
dc.citation.startPage | 183 | - |
dc.citation.title | ASTROPHYSICAL JOURNAL | - |
dc.citation.volume | 926 | - |
dc.contributor.author | Cho, Hyunjin | - |
dc.contributor.author | Ryu, Dongsu | - |
dc.contributor.author | Kang, Heysung | - |
dc.date.accessioned | 2023-12-21T14:37:57Z | - |
dc.date.available | 2023-12-21T14:37:57Z | - |
dc.date.created | 2022-03-18 | - |
dc.date.issued | 2022-02 | - |
dc.description.abstract | Observations indicate that turbulence in the interstellar medium (ISM) is supersonic (M (turb) >> 1) and strongly magnetized (beta similar to 0.01-1), while in the intracluster medium (ICM) it is subsonic (M (turb) less than or similar to 1) and weakly magnetized (beta similar to 100). Here, M (turb) is the turbulent Mach number and beta is the plasma beta. We study the properties of shocks induced in these disparate environments, including the distribution of the shock Mach number, M (s) , and the dissipation of the turbulent energy at shocks, through numerical simulations using a high-order, accurate code based on the weighted essentially nonoscillatory scheme. In particular, we investigate the effects of different modes of the forcing that drives turbulence: solenoidal, compressive, and a mixture of the two. In ISM turbulence, while the density distribution looks different with different forcings, the velocity power spectrum, P (v) , on small scales exhibits only weak dependence. Hence, the statistics of shocks depend weakly on forcing either. In the ISM models with M (turb) approximate to 10 and beta similar to 0.1, the fraction of the turbulent energy dissipated at shocks is estimated to be similar to 15%, not sensitive to the forcing mode. In contrast, in ICM turbulence, P (v) as well as the density distribution show strong dependence on forcing. The frequency and average Mach number of shocks are greater for compressive forcing than for solenoidal forcing; so is the energy dissipation. The fraction of the ensuing shock dissipation is in the range of similar to 10%-35% in the ICM models with M (turb) approximate to 0.5 and beta similar to 10(6). The rest of the turbulent energy should be dissipated through turbulent cascade. | - |
dc.identifier.bibliographicCitation | ASTROPHYSICAL JOURNAL, v.926, no.2, pp.183 | - |
dc.identifier.doi | 10.3847/1538-4357/ac41cc | - |
dc.identifier.issn | 0004-637X | - |
dc.identifier.scopusid | 2-s2.0-85126124762 | - |
dc.identifier.uri | https://scholarworks.unist.ac.kr/handle/201301/57676 | - |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/ac41cc | - |
dc.identifier.wosid | 000763082900001 | - |
dc.language | 영어 | - |
dc.publisher | IOP PUBLISHING LTD | - |
dc.title | Effects of Forcing on Shocks and Energy Dissipation in Interstellar and Intracluster Turbulences | - |
dc.type | Article | - |
dc.description.isOpenAccess | TRUE | - |
dc.relation.journalWebOfScienceCategory | Astronomy & Astrophysics | - |
dc.relation.journalResearchArea | Astronomy & Astrophysics | - |
dc.type.docType | Article | - |
dc.description.journalRegisteredClass | scie | - |
dc.description.journalRegisteredClass | scopus | - |
dc.subject.keywordPlus | EFFICIENT IMPLEMENTATION | - |
dc.subject.keywordPlus | DENSITY PROBABILITY-DISTRIBUTION | - |
dc.subject.keywordPlus | LARGE-SCALE STRUCTURE | - |
dc.subject.keywordPlus | MAGNETIC-FIELDS | - |
dc.subject.keywordPlus | GALAXY CLUSTERS | - |
dc.subject.keywordPlus | STAR-FORMATION | - |
dc.subject.keywordPlus | UNIVERSALITY | - |
dc.subject.keywordPlus | WAVES | - |
dc.subject.keywordPlus | GAS | - |
dc.subject.keywordPlus | FLUCTUATIONS | - |
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