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DC Field | Value | Language |
---|---|---|
dc.citation.number | 2 | - |
dc.citation.startPage | 50 | - |
dc.citation.title | ASTROPHYSICAL JOURNAL | - |
dc.citation.volume | 949 | - |
dc.contributor.author | Raymond, John C. | - |
dc.contributor.author | Ghavamian, Parviz | - |
dc.contributor.author | Bohdan, Artem | - |
dc.contributor.author | Ryu, Dongsu | - |
dc.contributor.author | Niemiec, Jacek | - |
dc.contributor.author | Sironi, Lorenzo | - |
dc.contributor.author | Tran, Aaron | - |
dc.contributor.author | Amato, Elena | - |
dc.contributor.author | Hoshino, Masahiro | - |
dc.contributor.author | Pohl, Martin | - |
dc.contributor.author | Amano, Takanobu | - |
dc.contributor.author | Fiuza, Frederico | - |
dc.date.accessioned | 2023-12-21T12:36:56Z | - |
dc.date.available | 2023-12-21T12:36:56Z | - |
dc.date.created | 2023-07-07 | - |
dc.date.issued | 2023-06 | - |
dc.description.abstract | Collisionless shock waves in supernova remnants and the solar wind heat electrons less effectively than they heat ions, as is predicted by kinetic simulations. However, the values of T ( e )/T ( p ) inferred from the H alpha profiles of supernova remnant shocks behave differently as a function of Mach number or Alfven Mach number than what is measured in the solar wind or predicted by simulations. Here we determine T ( e )/T ( p ) for supernova remnant shocks using H alpha profiles, shock speeds from proper motions, and electron temperatures from X-ray spectra. We also improve the estimates of sound speed and Alfven speed used to determine Mach numbers. We find that the H alpha determinations are robust and that the discrepancies among supernova remnant shocks, solar wind shocks, and computer-simulated shocks remain. We discuss some possible contributing factors, including shock precursors, turbulence, and varying preshock conditions. | - |
dc.identifier.bibliographicCitation | ASTROPHYSICAL JOURNAL, v.949, no.2, pp.50 | - |
dc.identifier.doi | 10.3847/1538-4357/acc528 | - |
dc.identifier.issn | 0004-637X | - |
dc.identifier.scopusid | 2-s2.0-85160914481 | - |
dc.identifier.uri | https://scholarworks.unist.ac.kr/handle/201301/64835 | - |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/acc528 | - |
dc.identifier.wosid | 000997730200001 | - |
dc.language | 영어 | - |
dc.publisher | IOP Publishing Ltd | - |
dc.title | Electron-Ion Temperature Ratio in Astrophysical Shocks | - |
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 | BALMER-DOMINATED SHOCKS | - |
dc.subject.keywordPlus | TYCHOS SUPERNOVA REMNANT | - |
dc.subject.keywordPlus | COSMIC-RAY ACCELERATION | - |
dc.subject.keywordPlus | LARGE-MAGELLANIC-CLOUD | - |
dc.subject.keywordPlus | HIGH-RESOLUTION SPECTROSCOPY | - |
dc.subject.keywordPlus | CYGNUS LOOP | - |
dc.subject.keywordPlus | MAGNETIC-FIELD | - |
dc.subject.keywordPlus | X-RAY | - |
dc.subject.keywordPlus | KEPLERS SUPERNOVA | - |
dc.subject.keywordPlus | MACH-NUMBER | - |
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