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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4411
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dc.contributor.authorRajamohan, R-
dc.contributor.authorParthasarathy, M-
dc.date.accessioned2009-03-25T10:34:57Z-
dc.date.available2009-03-25T10:34:57Z-
dc.date.issued1975-04-
dc.identifier.citationPramana - Journal of Physics, Vol. 4, No. 4, pp. 153 - 159en
dc.identifier.issn0304-4289-
dc.identifier.urihttp://hdl.handle.net/2248/4411-
dc.description.abstractSpectroscopic orbital elements are derived for the close binary system b Persei on the basis of forty spectrograms. The period is redetermined as 1.527360 days, and variations in the orbital elements are confirmed by reanalyzing previous observations. It is shown that variations in some of these elements may result from distortion of the radial-velocity curve by gas streams in the system. It is suggested that b Persei is in an active mass-transfer stage.en
dc.language.isoenen
dc.publisherIndian Academy of Sciencesen
dc.relation.urihttp://adsabs.harvard.edu/abs/1975Prama...4..153Ren
dc.relation.urihttp://www.ias.ac.in/j_archive/pramana/4/vol4contents.htmlen
dc.subjectBinary Starsen
dc.subjectOrbital Elementsen
dc.subjectStellar Motionsen
dc.subjectStellar Spectrophotometryen
dc.subjectApsidesen
dc.subjectEmission Spectraen
dc.subjectMass Transferen
dc.subjectRadial Velocityen
dc.subjectRadio Sources (Astronomy)en
dc.titleOrbit of the spectroscopic binary B Perseien
dc.typeArticleen
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