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dc.contributor.authorKharchenko, V.
dc.contributor.authorDalgarno, A.
dc.date.accessioned2019-09-24T17:25:49Z
dc.date.issued2001
dc.identifier.citationKharchenko, V., and A. Dalgarno. 2001. “Variability of Cometary X-Ray Emission Induced by Solar Wind Ions.” The Astrophysical Journal 554 (1): L99–102. https://doi.org/10.1086/320929.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41397461*
dc.description.abstractX-ray emission spectra induced by the interaction of the slow and fast solar wind components with cometary gas are calculated for typical solar wind compositions. The emission spectra arising from the charge transfer mechanism are shown to be in good agreement with observational data. The identities and intensities of the brightest spectral lines that include forbidden transitions are obtained for the slow and fast solar winds. Differences in emission spectra of individual comets occur because of variations in the solar wind composition. Comparisons with observational data for comets Levy and Hale-Bopp indicate that they were subjected to the slow solar wind. The spectra at photon energies above 500 eV fluctuate with the solar wind composition because of the varying presence of fully stripped oxygen ions. Mechanisms of X-ray photon emission at energies above 0.9 keV are discussed.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleVariability of Cometary X-Ray Emission Induced by Solar Wind Ions
dc.typeJournal Article
dc.description.versionVersion of Record
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorDalgarno, Alexander::501fae4cfad8b04754ee2838c45fc5d0::600
dc.date.available2019-09-24T17:25:49Z
dash.workflow.comments1Science Serial ID 96147
dc.identifier.doi10.1086/320929
dash.source.volume554;1
dash.source.pageL99-L102


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