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An improved model of the B0.5e + Be binary system φ Per

Published online by Cambridge University Press:  26 May 2016

P. Harmanec ,
J. Horn ,
P. Koubský ,
K. Juza ,
H. Božić ,
K. Pavlovski ,
A.-M Hubert  and
H. Hubert
P. Harmanec
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic 251 65 Ondřejov, Czech Republic
J. Horn
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic 251 65 Ondřejov, Czech Republic
P. Koubský
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic 251 65 Ondřejov, Czech Republic
K. Juza
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic 251 65 Ondřejov, Czech Republic
H. Božić
Affiliation:
Hvar Observatory, Faculty of Geodesy, Zagreb University, Kačićeva 26, 41000 Zagreb, Croatia
K. Pavlovski
Affiliation:
Hvar Observatory, Faculty of Geodesy, Zagreb University, Kačićeva 26, 41000 Zagreb, Croatia
A.-M Hubert
Affiliation:
Observatoire de Paris, Section d'Astrophysique de Meudon, URA 335 du CNRS, F-92195 Meudon Cedex, France
H. Hubert
Affiliation:
Observatoire de Paris, Section d'Astrophysique de Meudon, URA 335 du CNRS, F-92195 Meudon Cedex, France

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φ Per (HD 10516) is a spectroscopic binary with a 126.699-day period (Ludendorff 1910, Cannon 1910, Harmanec 1985). However, most of the published RV curves of the primary are based on H I shell lines and exhibit a typical distortion with a sharp maximum, shallow minimum and a bump at 0.P4 after the RV maximum (c.f., e.g., Harmanec 1985). There has been controversy on the nature of the secondary. Hynek (1940) and Hendry (1976) concluded that the binary was composed of two B stars. Peters (1976) suggested that the secondary of φ Per is a Roche-lobe filling K giant. Poeckert (1981) reported the discovery of a weak He II 4686 emission which moved in antiphase to the Be primary and suggested that it originated in the disk around the secondary. In his interpretation, the secondary is a helium star, a remnant of an originally more massive star which in the past transferred its mass to the present Be star. There is now no mass tranfer in the system according to Poeckert. Using RVs of the broad absorptions for primary, and of the He II 4686 emission for the secondary, Poeckert obtained two roughly sinusoidal RV curves and M1sin3i = 21.1 m⊙ and M2sin3i = 3.4 m⊙.

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. 327 - 328
Copyright
Copyright © Kluwer 1994 

References

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