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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/1639
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dc.contributor.authorGhosh, K. K-
dc.contributor.authorJayakumar, K-
dc.date.accessioned2007-06-15T10:49:22Z-
dc.date.available2007-06-15T10:49:22Z-
dc.date.issued1988-02-
dc.identifier.citationAstrophysics and Space Science, Vol. 141, No. 2, pp. 293 – 301en
dc.identifier.issn0004-640X-
dc.identifier.urihttp://hdl.handle.net/2248/1639-
dc.description.abstractSudden brightening of Fe II and Balmer (Hβ and Hα) lines of X Oph was observed on 28 - 29 May, 1986. Equivalent width of Fe II and Hβ lines increased by a factor of two and that for Hα line by a factor of four, during the brightening phase of the star. This brightening phenomenon has been explained in the framework of "Coronal Radiative Instability".en
dc.format.extent176190 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherD. Reidel Publishing Co.en
dc.relation.urihttp://adsabs.harvard.edu/abs/1988Ap%26SS.141..293Gen
dc.relation.urihttp://dx.doi.org/10.1007/BF00639496-
dc.subjectEarly Starsen
dc.subjectBalmer Seriesen
dc.subjectH Alpha Line-
dc.subjectH Beta Line-
dc.subjectStellar Spectra-
dc.subjectB Stars-
dc.subjectIron-
dc.subjectO Stars-
dc.subjectStellar Atmospheres-
dc.titleRapid simultaneous observations of Fe II and Balmer emission lines of X OPHen
dc.typeArticleen
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