Orbit of the spectroscopic binary B Persei

dc.contributor.author	Rajamohan, R
dc.contributor.author	Parthasarathy, M
dc.date.accessioned	2009-03-25T10:34:57Z
dc.date.available	2009-03-25T10:34:57Z
dc.date.issued	1975-04
dc.identifier.citation	Pramana - Journal of Physics, Vol. 4, No. 4, pp. 153 - 159	en
dc.identifier.issn	0304-4289
dc.identifier.uri	http://hdl.handle.net/2248/4411
dc.description.abstract	Spectroscopic 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.iso	en	en
dc.publisher	Indian Academy of Sciences	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1975Prama...4..153R	en
dc.relation.uri	http://www.ias.ac.in/j_archive/pramana/4/vol4contents.html	en
dc.subject	Binary Stars	en
dc.subject	Orbital Elements	en
dc.subject	Stellar Motions	en
dc.subject	Stellar Spectrophotometry	en
dc.subject	Apsides	en
dc.subject	Emission Spectra	en
dc.subject	Mass Transfer	en
dc.subject	Radial Velocity	en
dc.subject	Radio Sources (Astronomy)	en
dc.title	Orbit of the spectroscopic binary B Persei	en
dc.type	Article	en