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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/1757
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dc.contributor.authorRamesh, K. B-
dc.contributor.authorRohini, V. S-
dc.date.accessioned2007-07-27T08:53:20Z-
dc.date.available2007-07-27T08:53:20Z-
dc.date.issued2008-10-10-
dc.identifier.citationThe Astrophysical Journal Letters, Vol. 686, pp. L41 – L44en
dc.identifier.urihttp://hdl.handle.net/2248/1757-
dc.description.abstractConsistent correlations between X-ray background flux (XBF) and sunspot area over three solar cycles suggest a strong relationship between the flux emergence at the locations of strong field regions, sunspots, and the coronal heating processes that ultimately result in coronal X-ray emission. We find that the pattern of variation of sunspot numbers shows noticeable deviations from the pattern depicted by the sunspot areas when compared to XBF. A weight factor, such as , assigned to individual spot groups in may provide better estimation of the true strength of solar cyclesen
dc.format.extent633480 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherThe American Astronomical Societyen
dc.relation.urihttp://www.journals.uchicago.edu/doi/abs/10.1086/592774en
dc.rights© The American Astronomical Society. All rights reserved-
dc.subjectSunen
dc.subjectcorona—Sunen
dc.subjectX-rays-
dc.subjectgamma rays—sunspots-
dc.title1–8 Å Coronal Background X-Ray Emission and the Associated Indicators of Photospheric Magnetic Activityen
dc.typeArticleen
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