Reference : Photoelectric photometry of the peculiar emission-line star GG Carinae
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/17774
Photoelectric photometry of the peculiar emission-line star GG Carinae
English
Gosset, Eric mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Surdej, Jean mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
Swings, J.-P. [Liege, Universite, Cointe-Ougree, Belgium]
1984
Astronomy and Astrophysics. Supplement Series
EDP Sciences
55
411-424
Yes (verified by ORBi)
International
0365-0138
Les Ulis
France
[en] LIGHT CURVE ; PECULIAR STARS ; STELLAR SPECTROPHOTOMETRY ; UBV SPECTRA ; VARIABLE STARS ; ELECTROPHOTOMETRY ; EMISSION SPECTRA ; FOURIER ANALYSIS ; STELLAR COLOR ; ECLIPSING BINARY STARS
[en] The first extensive sets of photoelectric observations of the peculiar emission-line star GG Carinae were obtained from 1977 to 1981, in both the standard UBV and Strömgren systems. A Fourier analysis of 767 independent measurements leads to the determination of a period P = 31[SUP]d[/SUP].020 for the light variations. Different physical arguments based on the analysis of the present photoelectric - as well as previous photographic - data clearly indicate, however, that the true period is P = 62[SUP]d[/SUP].039. The resulting composite lightcurve displays two distinct maxima and minima with a total light amplitude Deltam â ¡ 0.5 mag. Additional interesting features are noticed in the mean lightcurve. Although it is not possible to classify GG Carinae among any known type of variable stars, the light variations of this object are similar to those observed for beta Lyrae-type systems.
Researchers ; Professionals
http://hdl.handle.net/2268/17774
http://esoads.eso.org/abs/1984A%26AS...55..411G
The authors thank EDP Sciences for their deposit authorization

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