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Title:
Asteroseismology of the β Cephei star ν Eridani - II. Spectroscopic observations and pulsational frequency analysis
Authors:
Aerts, C.; De Cat, P.; Handler, G.; Heiter, U.; Balona, L. A.; Krzesinski, J.; Mathias, P.; Lehmann, H.; Ilyin, I.; De Ridder, J.; Dreizler, S.; Bruch, A.; Traulsen, I.; Hoffmann, A.; James, D.; Romero-Colmenero, E.; Maas, T.; Groenewegen, M. A. T.; Telting, J. H.; Uytterhoeven, K.; Koen, C.; Cottrell, P. L.; Bentley, J.; Wright, D. J.; Cuypers, J.
Affiliation:
AA(Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium), AB(Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium), AC(Institut für Astronomie, Universität Wien, Türkenschanzstrasse 17, A-1180 Wien, Austria), AD(Department of Astronomy, Case Western Reserve University 10900 Euclid Ave Cleveland, OH 44106-7215, USA), AE(South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa), AF(Apache Point Observatory 2001 Apache Point Road PO Box 59, Sunspot, NM 88349-0059, USA; Mt. Suhora Observatory, Cracow, Pedagogical University, ul. Podchorǎżych 2, 30-084, Poland), AG(Observatoire de la Côte d'Azur, BP 4229, F-06304 Nice Cedex 04, France), AH(Thüringer Landessternwarte, D-07778 Tautenburg, Germany), AI(Astronomy Division, PO Box 3000, 90014 University of Oulu, Finland), AJ(Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium), AK(Institut für Astronomie und Astrophysik, Abt. Astronomie, Sand 1, 72076 Tübingen, Germany), AL(Laboratório Nacional de Astrofísica, Rua Estados Unidos, 154 - Bairro das Nacões, 37504-364 Itajubá, Brazil), AM(Institut für Astronomie und Astrophysik, Abt. Astronomie, Sand 1, 72076 Tübingen, Germany), AN(Institut für Astronomie und Astrophysik, Abt. Astronomie, Sand 1, 72076 Tübingen, Germany), AO(Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, F-38041 Grenoble Cedex 9, France), AP(South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa), AQ(Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium), AR(Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium), AS(Nordic Optical Telescope, Apartado 474, E-38700 Santa Cruz de La Palma, Spain), AT(Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Leuven, Belgium), AU(South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa), AV(Department of Physics and Astronomy, University of Canterbury, Christchurch, New Zealand), AW(Department of Physics and Astronomy, University of Canterbury, Christchurch, New Zealand), AX(Department of Physics and Astronomy, University of Canterbury, Christchurch, New Zealand), AY(Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussels, Belgium)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 347, Issue 2, pp. 463-470. (MNRAS Homepage)
Publication Date:
01/2004
Origin:
MNRAS
Astronomy Keywords:
techniques: spectroscopic, stars: early-type, stars: individual: ν Eridani, stars: oscillations, stars: variables: other
DOI:
10.1111/j.1365-2966.2004.07215.x
Bibliographic Code:
2004MNRAS.347..463A

Abstract

We undertook a multisite spectroscopic campaign for the β Cephei star ν Eridani. A total of 2294 high-resolution spectra were obtained from telescopes at 11 different observatories around the world. The time base of dedicated multisite observations is 88 d. To this data set we have added 148 older, previously unpublished spectra, such that the overall time-span of the 2442 spectra is 430 d. The analysis of the radial velocity variations derived from the SiIII triplet centred on 4560Å leads to 19 significant frequencies, of which seven correspond to independent pulsation frequencies. Five of these are members of multiplets with an average spacing of 0.018 +/- 0.002 cd-1. Our spectroscopic results agree well with those derived from a simultaneous multisite photometric campaign of the star, albeit that we do not recover their low frequency at 0.43218 cd-1. We find three different candidate frequencies below 1 cd-1 instead. We also find that the radial velocity amplitude of the main mode has increased by some 30 per cent over the last 15 years, which is consistent with the photometry data. We derive a relative equivalent width variation of 6.5 per cent, which is completely dominated by the main radial mode. The phase difference between the radial velocity and light variations for the main frequency is , which is clearly deviant from the adiabatic value and confirms the radial nature of the dominant mode. The spectral line broadening leads to an upper limit of 20 km s-1 for vsini, which is consistent with the long rotation period derived from the frequency splittings.

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