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 |
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dc.format.mimetype |
application/pdf |
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dc.language.iso |
en |
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dc.publisher |
Astronomical Society of India |
en |
dc.subject |
variable stars |
en |
dc.title |
Is HR 2947 a variable? |
en |
dc.type |
Article |
en |