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dc.contributor.authorPepino, R.
dc.contributor.authorKharchenko, V.
dc.contributor.authorDalgarno, A.
dc.contributor.authorLallement, R.
dc.date.accessioned2019-09-24T17:26:15Z
dc.date.issued2004
dc.identifier.citationPepino, R., V. Kharchenko, A. Dalgarno, and R. Lallement. 2004. “Spectra of the X‐Ray Emission Induced in the Interaction between the Solar Wind and the Heliospheric Gas.” The Astrophysical Journal 617 (2): 1347–52. https://doi.org/10.1086/425682.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41397493*
dc.description.abstractSpectra of the heliospheric EUV and X-ray emission induced in the charge transfer collisions of the highly charged solar wind ions with the interstellar gas have been calculated. Cascading photon spectra of individual Oq+, Cq+, Nq+, and Neq+ ions have been constructed using recent data on ion radiative transition probabilities and the state-selective population cross sections for charge transfer collisions of the most abundant heavy solar wind ions with H and He atoms. Emission spectra have been calculated for slow and fast solar winds interacting with the heliospheric H and He gas. Relative intensities of the brightest lines have been predicted. The volume power distribution of the charge transfer EUV and X-ray emission has been computed for simplified models of the solar winds and the interstellar gas. X-ray images of the heliosphere have been composed for the region inside 10 AU from the Sun.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleSpectra of the X‐Ray Emission Induced in the Interaction between the Solar Wind and the Heliospheric Gas
dc.typeJournal Article
dc.description.versionVersion of Record
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorDalgarno, Alexander::501fae4cfad8b04754ee2838c45fc5d0::600
dc.date.available2019-09-24T17:26:15Z
dash.workflow.comments1Science Serial ID 96810
dc.identifier.doi10.1086/425682
dash.source.volume617;2
dash.source.page1347-1352


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