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Title:
Asteroseismology of the β Cephei star ν Eridani - I. Photometric observations and pulsational frequency analysis
Authors:
Handler, G.; Shobbrook, R. R.; Jerzykiewicz, M.; Krisciunas, K.; Tshenye, T.; Rodríguez, E.; Costa, V.; Zhou, A.-Y.; Medupe, R.; Phorah, W. M.; Garrido, R.; Amado, P. J.; Paparó, M.; Zsuffa, D.; Ramokgali, L.; Crowe, R.; Purves, N.; Avila, R.; Knight, R.; Brassfield, E.; Kilmartin, P. M.; Cottrell, P. L.
Affiliation:
AA(Institut für Astronomie, Universität Wien, Türkenschanzstrasse 17, A-1180 Wien, Austria), AB(Australian National University, Canberra, ACT, Australia), AC(Wroclaw University Observatory, ul. Kopernika 11, 51-622 Wroclaw, Poland), AD(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile; Las Campanas Observatory, Casilla 601, La Serena, Chile), AE(Theoretical Astrophysics Programme, University of the North-West, Private Bag X2046, Mmabatho 2735, South Africa), AF(Instituto de Astrofisica de Andalucia, C.S.I.C., Apdo. 3004, 18080 Granada, Spain), AG(Instituto de Astrofisica de Andalucia, C.S.I.C., Apdo. 3004, 18080 Granada, Spain), AH(National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China), AI(Theoretical Astrophysics Programme, University of the North-West, Private Bag X2046, Mmabatho 2735, South Africa; South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa), AJ(Theoretical Astrophysics Programme, University of the North-West, Private Bag X2046, Mmabatho 2735, South Africa), AK(Instituto de Astrofisica de Andalucia, C.S.I.C., Apdo. 3004, 18080 Granada, Spain), AL(Instituto de Astrofisica de Andalucia, C.S.I.C., Apdo. 3004, 18080 Granada, Spain), AM(Konkoly Observatory, Box 67, H-1525 Budapest XII, Hungary), AN(Konkoly Observatory, Box 67, H-1525 Budapest XII, Hungary), AO(Theoretical Astrophysics Programme, University of the North-West, Private Bag X2046, Mmabatho 2735, South Africa), AP(Department of Physics and Astronomy, University of Hawaii - Hilo, 200 West Kawili Street, Hilo, Hawaii, 96720-4091, USA), AQ(Department of Physics and Astronomy, University of Hawaii - Hilo, 200 West Kawili Street, Hilo, Hawaii, 96720-4091, USA), AR(Department of Physics and Astronomy, University of Hawaii - Hilo, 200 West Kawili Street, Hilo, Hawaii, 96720-4091, USA), AS(Department of Physics and Astronomy, University of Hawaii - Hilo, 200 West Kawili Street, Hilo, Hawaii, 96720-4091, USA), AT(Department of Physics and Astronomy, University of Hawaii - Hilo, 200 West Kawili Street, Hilo, Hawaii, 96720-4091, USA), AU(Department of Physics and Astronomy, University of Canterbury, Christchurch, New Zealand), AV(Department of Physics and Astronomy, University of Canterbury, Christchurch, New Zealand)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 347, Issue 2, pp. 454-462. (MNRAS Homepage)
Publication Date:
01/2004
Origin:
MNRAS
MNRAS Keywords:
techniques: photometric, stars: early-type, stars: individual: μ Eridani, stars: individual: ν Eridani, stars: oscillations, stars: variables: other
DOI:
10.1111/j.1365-2966.2004.07214.x
Bibliographic Code:
2004MNRAS.347..454H

Abstract

We undertook a multisite photometric campaign for the β Cephei star ν Eridani. More than 600 h of differential photoelectric uvyV photometry were obtained with 11 telescopes during 148 clear nights.

The frequency analysis of our measurements shows that the variability of ν Eri can be decomposed into 23 sinusoidal components, eight of which correspond to independent pulsation frequencies between 5 and 8 cd-1. Some of these are arranged in multiplets, which suggests rotational m-mode splitting of non-radial pulsation modes as the cause. If so, the rotation period of the star must be between 30 and 60 d.

One of the signals in the light curves of ν Eri has a very low frequency of 0.432 cd-1. It can be a high-order combination frequency or, more likely, an independent pulsation mode. In the latter case, ν Eri would be both a β Cephei star and a slowly pulsating B (SPB) star.

The photometric amplitudes of the individual pulsation modes of ν Eri appear to have increased by about 20 per cent over the last 40 years. So have the amplitudes of the dominant combination frequencies of the star. Among the latter, we could only identify sum frequencies with certainty, not difference frequencies, which suggests that neither light-curve distortion in its simplest form nor resonant mode coupling is their single cause.

One of our comparison stars, μ Eridani, turned out to be variable with a dominant time-scale of 1.62 d. We believe either that it is an SPB star just leaving its instability strip or that its variations are of rotational origin.


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