HR 7275: A new variable star

Three years of photometry in V and B of the UBV system are presented to confirm the suspicion of Herbst (1973) that HR 7275 is a variable star. The photometry is used to derive the photometric period, which proves to be about 3% shorter than the spectroscopically determined optical period of 28.59 d...

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Published in:Astrophysics and space science 1982-04, Vol.83 (1-2), p.181-188
Main Authors: Fried, R. E., Eaton, Joel A., Hall, D. S., Henry, G. W., Lovell, L. P., Krisciunas, K., Chambliss, C. R., Detterline, P. K., Landis, H. J., Louth, H., Skillman, D. R.
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container_end_page 188
container_issue 1-2
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container_title Astrophysics and space science
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creator Fried, R. E.
Eaton, Joel A.
Hall, D. S.
Henry, G. W.
Lovell, L. P.
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Detterline, P. K.
Landis, H. J.
Louth, H.
Skillman, D. R.
description Three years of photometry in V and B of the UBV system are presented to confirm the suspicion of Herbst (1973) that HR 7275 is a variable star. The photometry is used to derive the photometric period, which proves to be about 3% shorter than the spectroscopically determined optical period of 28.59 d. Total variation observed during the three years was 0.22 m in the V, and the light curve was always asymmetrical.
doi_str_mv 10.1007/BF00648550
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title HR 7275: A new variable star
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