Detection of new short period oscillations in PG 1711+336 (V795 HER)

dc.contributor.author	Ashoka, B. N.
dc.contributor.author	Seetha, S.
dc.contributor.author	Marar, T. M. K.
dc.contributor.author	Padmini, V. N.
dc.contributor.author	Kasturirangan, K.
dc.contributor.author	Rao, U. R.
dc.contributor.author	Pande, M. C.
dc.contributor.author	Mahra, H. S.
dc.date.accessioned	2010-02-15T05:56:39Z
dc.date.available	2010-02-15T05:56:39Z
dc.date.issued	1989
dc.identifier.citation	This article downloded from ADS Free Online Journal	en_US
dc.identifier.uri	http://hdl.handle.net/123456789/512
dc.description.abstract	Long period light variations of the cataclysmic variables PG 1711+336 (V795 Her) were first noticed by Mironov et al. (1983 a,b) who reported a photometric period of 0.115883 day for the system. Baidak et al., (1985) improved the ephemer is and refined the period to 0.114488 day (2.75 hour). If this period is interpreted as the orbital period, then the system is unique in that its orbital period falls within the period gap in the distribution of cataclysmic variables versus their orbital periods.	en_US
dc.language.iso	en_US	en_US
dc.relation.ispartofseries	ibvs3352
dc.subject	Cataclysmic variables PG 1711+336 (V795 Her)	en_US
dc.title	Detection of new short period oscillations in PG 1711+336 (V795 HER)	en_US
dc.type	Article	en_US