Period study of the binary star SW Cygni

dc.contributor.author	Chaubey, U. S.
dc.date.accessioned	2011-01-11T06:34:13Z
dc.date.available	2011-01-11T06:34:13Z
dc.date.issued	1980
dc.identifier.citation	This article is taken from ADS database	en_US
dc.identifier.uri	http://hdl.handle.net/123456789/778
dc.description.abstract	The O-C curve of SW Cyg between 1880 and 1977 is presented and discussed. It is found that the orbital period undergoes a systematic change, becoming greater with time. In addition, a periodic oscillation of amplitude 0ᵈ.015 with period of 43.8 years is superimposed on this general trend. It is concluded that the increase int he period is due to a transfer of mass from the secondary star to the primary and the periodic oscillation is due to the light time effect of the third body of mass function f(m) = 0.006M☉.	en_US
dc.language.iso	en_US	en_US
dc.relation.ispartofseries	ass67-129
dc.subject	SW Cygni - Binary star	en_US
dc.title	Period study of the binary star SW Cygni	en_US
dc.type	Article	en_US