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Southworth, J, Bowman, DM and Pavlovski, K (2021) A β Cephei pulsator and a changing orbital inclination in the high-mass eclipsing binary system VV Orionis. Monthly Notices of the Royal Astronomical Society: Letters, 501 (1). L65 - L70. ISSN 1745-3925

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Abstract

We present an analysis of the high-mass eclipsing binary system VV Ori based on photometry from the TESS satellite. The primary star (B1 V, 9.5 M⊙⁠) shows β Cephei pulsations and the secondary (B7 V, 3.8 M⊙⁠) is possibly a slowly pulsating B star. We detect 51 significant oscillation frequencies, including two multiplets with separations equal to the orbital frequency, indicating that the pulsations are tidally perturbed. We analyse the TESS light curve and published radial velocities to determine the physical properties of the system. Both stars are only the second of their pulsation type with a precisely measured mass. The orbital inclination is also currently decreasing, likely due to gravitational interactions with a third body.

Item Type: Article
Additional Information: This is the final published version of the article (version of record). It first appeared online via Oxford University Press at https://doi.org/10.1093/mnrasl/slaa197 - please refer to any applicable terms of use of the publisher.
Uncontrolled Keywords: stars, binaries, eclipsing, fundamental parameters, oscillations
Subjects: Q Science > QB Astronomy > QB799 Stars
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 22 Apr 2021 11:04
Last Modified: 11 Aug 2021 10:26
URI: https://eprints.keele.ac.uk/id/eprint/9423

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