Is HR 2947 a variable?

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DC Field	Value	Language
dc.contributor.author	Kameswara Rao, N	-
dc.contributor.author	Ashok, N. M	-
dc.contributor.author	Kulkarni, P. V	-
dc.date.accessioned	2005-02-04T16:21:03Z	-
dc.date.available	2005-02-04T16:21:03Z	-
dc.date.issued	1981-06	-
dc.identifier.citation	BASI, Vol. 9, No. 2, pp. 144-150	en
dc.identifier.uri	http://hdl.handle.net/2248/312	-
dc.description.abstract	Observations of HR 2947 show that it is fainter by 0.3 mag in V compared to the magnitude listed by Cowley et al. (1969). The energy distribution from 1565 Armstrong to 1.25 micro is similar to that of a B5 III star and does not indicate presence of any companion. Teff ~ 13500 plus or minus 500 K and log g= 3.5 plus or minus 0.5 are obtained by comparison with the theoretical energy distribution. It is suggested that the light variability, if real, could be due to the formation of a thin gas shell around the star.	en
dc.format.extent	475881 bytes	-
dc.format.mimetype	application/pdf	-
dc.language.iso	en	-
dc.publisher	Astronomical Society of India	en
dc.subject	variable stars	en
dc.title	Is HR 2947 a variable?	en
dc.type	Article	en
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