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Photometric characteristics of the Be stars: almost twenty years of UBV monitoring at the Hvar observatory

Published online by Cambridge University Press:  26 May 2016

K. Pavlovski ,
H. Božić ,
Ž. Ružić ,
P. Harmanec ,
J. Horn ,
P. Koubský ,
K. Juza ,
P. Hadrava ,
S. Kříž  and
S. Štefl
...Show all authors
K. Pavlovski
Affiliation:
Hvar Observatory, Zagreb University, 41000 Zagreb, Croatia
H. Božić
Affiliation:
Hvar Observatory, Zagreb University, 41000 Zagreb, Croatia
Ž. Ružić
Affiliation:
Hvar Observatory, Zagreb University, 41000 Zagreb, Croatia
P. Harmanec
Affiliation:
Astronomical Institute, 251 65 Ondřejov, Czech Republic
J. Horn
Affiliation:
Astronomical Institute, 251 65 Ondřejov, Czech Republic
P. Koubský
Affiliation:
Astronomical Institute, 251 65 Ondřejov, Czech Republic
K. Juza
Affiliation:
Astronomical Institute, 251 65 Ondřejov, Czech Republic
P. Hadrava
Affiliation:
Astronomical Institute, 251 65 Ondřejov, Czech Republic
S. Kříž
Affiliation:
Astronomical Institute, 251 65 Ondřejov, Czech Republic
S. Štefl
Affiliation:
Astronomical Institute, 251 65 Ondřejov, Czech Republic
F. Žďársky
Affiliation:
Astronomical Institute, 251 65 Ondřejov, Czech Republic

Extract

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Since their discovery (by Father Secchi in 1866) until the end of sixties, Be stars were not a subject of any systematic studies of their possible light and colour variations. Already at that time, the astronomical literature contained ample evidence showing that a number of Be stars were light variables. However, almost all such findings resulted as by-products of studies of different or wider groups of objects. Feinstein (1968) was probably the first who pointed out explicitly that many Be stars are light variables. A pioneering study which was aimed at the detection of light variations of a large group of Be stars by means of differential photoelectric photometry was carried out by Haupt & Schroll (1974).

Type
5. Be Stars: Spectroscopy and Photometry
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 301 - 302
Copyright
Copyright © Kluwer 1994 

References

Feinstein, A.: 1968, Z. Astrophys. 68, 29 Google Scholar
Harmanec, P., Hadrava, P., Ružić, Ž., Pavlovski, K., Božić, H., Horn, J., Koubský, P.: 1988, IBVS, No. 3263 ,Google Scholar
Harmanec, P., Horn, J., Juza, K.: 1993, A&AS, in press,Google Scholar
Haupt, H., Schroll, A.: 1974, A&AS 15, 311 Google Scholar
Pavlovski, K., Ružić, Ž.: 1991, in Rapid Variability of OB-stars: Nature and Diagnostic Value , Ed. Baade, D., ESO Conf. Proc. No. 36, 191 Google Scholar
Percy, J.R., Jakate, S.M., Matthews, J.M.: 1981, AJ 86, 53 Google Scholar