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Towards an understanding of the Of?p star HD 191612: optical spectroscopy
Howarth, Ian D.; Walborn, Nolan R.; Lennon, Danny J.; Puls, Joachim; Nazé, Yaël; Annuk, K.; Antokhin, I.; Bohlender, D.; Bond, H.; Donati, J.-F.; Georgiev, L.; Gies, D.; Harmer, D.; Herrero, A.; Kolka, I.; McDavid, D.; Morel, T.; Negueruela, I.; Rauw, G.; Reig, P.
AA(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT), AB(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA), AC(The Isaac Newton Group of Telescopes, Apartado de Correos 321, 38700 Santa Cruz de La Palma, Canary Islands, Spain), AD(Universitäts-Sternwarte München, Scheinerstr. 1, 81679 München, Germany), AE(FNRS Institut d'Astrophysique et de Géophysique, Université de Liège, Bât. B5c, Allée du VI Août 17, B-4000 Liège, Belgium), AF(Tartu Observatory, 61602 Tõravere, Estonia), AG(Sternberg Astronomical Institute, Moscow University, Universitetskij Prospect 13, Moscow 119992, Russia), AH(National Research Council of Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada), AI(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA), AJ(Laboratoire d'Astrophysique, Observatoire Midi-Pyrénées, 14 Av. E. Belin, F-31400 Toulouse, France), AK(Instituto de Astronomía, UNAM, Apartado Postal 70-254, CD Universitaria, CP 04510 México DF, Mexico), AL(Department of Physics and Astronomy, Georgia State University, PO Box 4106, Atlanta, GA 30302-4106, USA), AM(Kitt Peak National Observatory, NOAO, PO Box 26732, Tucson, AZ 85719, USA), AN(Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain), AO(Tartu Observatory, 61602 Tõravere, Estonia), AP(Department of Astronomy, University of Virginia, PO Box 400325, Charlottesville, VA 22904-4325, USA), AQ(Katholieke Universiteit Leuven, Departement Natuurkunde en Sterrenkunde, Instituut voor Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium), AR(Departamento de Fisica, Ingeniería de Sistemas y Teoría de la Señal, Escuela Politécnica Superior, Universidad de Alicante, Ap. 99, 03080 Alicante, Spain), AS(FNRS Institut d'Astrophysique et de Géophysique, Université de Liège, Bât. B5c, Allée du VI Août 17, B-4000 Liège, Belgium), AT(IESL, Foundation for Research and Technology, 71110 Heraklion, Greece)
Monthly Notices of the Royal Astronomical Society, Volume 381, Issue 2, pp. 433-446. (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
stars: binaries: spectroscopic, stars: early-type, stars: individual: HD 191612, stars: magnetic fields, stars: rotation
Bibliographic Code:


We present extensive optical spectroscopy of the early-type magnetic star HD 191612 (O6.5f?pe-O8fp). The Balmer and HeI lines show strongly variable emission which is highly reproducible on a well-determined 538-d period. HeII absorptions and metal lines (including many selective emission lines but excluding HeII lambda4686 Å emission) are essentially constant in line strength, but are variable in velocity, establishing a double-lined binary orbit with Porb = 1542d, e = 0.45. We conduct a model-atmosphere analysis of the spectrum, and find that the system is consistent with a ~O8 giant with a ~B1 main-sequence secondary. Since the periodic 538-d changes are unrelated to orbital motion, rotational modulation of a magnetically constrained plasma is strongly favoured as the most likely underlying `clock'. An upper limit on the equatorial rotation is consistent with this hypothesis, but is too weak to provide a strong constraint.

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