Hostname: page-component-cd9895bd7-dk4vv Total loading time: 0 Render date: 2024-12-18T05:30:17.576Z Has data issue: false hasContentIssue false
  • English
  • Français

Multiperiodicity in light variations of 53 Persei: results from optical photometry in 1990 October–1991 January

Published online by Cambridge University Press:  26 May 2016

L. Huang ,
Z. Guo ,
J. Hao ,
J.R. Percy ,
M.S. Fieldus ,
R. Fried ,
R. K. Palovski ,
H. Božić ,
Ž. Ružić  and
M. Paparó
...Show all authors
L. Huang
Affiliation:
Beijing Astronomical Observatory, Beijing, China
Z. Guo
Affiliation:
Beijing Astronomical Observatory, Beijing, China
J. Hao
Affiliation:
Beijing Astronomical Observatory, Beijing, China
J.R. Percy
Affiliation:
Erindale Campus, The University of Toronto, Mississauga, Canada
M.S. Fieldus
Affiliation:
Department of Astronomy, The University of Toronto, Toronto, Canada
R. Fried
Affiliation:
Braeside Observatory, Flagstaff, U.S.A.
R. K. Palovski
Affiliation:
Hvar Observatory, Zagreb University, Zagreb, Croatia
H. Božić
Affiliation:
Hvar Observatory, Zagreb University, Zagreb, Croatia
Ž. Ružić
Affiliation:
Hvar Observatory, Zagreb University, Zagreb, Croatia
M. Paparó
Affiliation:
Konkoly Observatory, Budapest, Hungary
B. Vetö
Affiliation:
Konkoly Observatory, Budapest, Hungary
R. Dukes
Affiliation:
Physics Department, The College of Charleston, Charleston, U.S.A.

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The B type star 53 Persei was discovered in 1977 by Smith (1977) as the prototype of a separate group of B-type variables showing light and line profile variability. The physical cause of the variability was thought to be nonradial pulsation (NRP) (see, e.g. Smith et al. 1984). However, the NRP model for this star has been questioned by Balona (1986) who suggested the rotational modulation (RM) model to explain the variability. In order to resolve the long lasting debate about 53 Persei, a campaign was initiated to organize coordinated optical photometry and spectroscopy from the ground, and Far-UV photometry from Voyager in 1991 January. This paper presents the results of period analysis on the groundbased UBV data. In another paper, Smith & Huang (1994) report the new identification of pulsation modes using Voyager Far-UV photometry combined with the results from optical observations. Some preliminary results from APT uvby observations taken at a single site are also cited for comparison.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 33 - 36
Copyright
Copyright © Kluwer 1994 

References

Balona, L.A.: 1986, ‘Stellar Pulsation’ in Cox, A.N. et al., ed(s)., Berlin: Springer , 83.Google Scholar
Breger, M.: 1990, Comm. Asteroseismology 20, 1 Google Scholar
Buta, R.J., Smith, M.A.: 1979, Astrophysical Journal 232, 213 CrossRefGoogle Scholar
Roberts, D.H., Lehár, J, Dreher, J.W.: 1987, Astronomical Journal 93, 968 CrossRefGoogle Scholar
Smith, M.A.: 1977, Astrophysical Journal 215, 574 Google Scholar
Smith, M.A., Buta, R.J.: 1979, Astrophysical Journal 232, L193 Google Scholar
Smith, M.A. et al.: 1984, Astrophysical Journal 282, 226 Google Scholar
Smith, M.A., McCall, M.L.: 1978, Astrophysical Journal 223, 221 Google Scholar
Smith, M.A., Huang, L. 1994, this Proceedings Google Scholar