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A ß?Cephei pulsator and a changing orbital inclination in the high-mass eclipsing binary system VV?Orionis

Southworth, John; Bowman, D M; Pavlovski, K

A ß?Cephei pulsator and a changing orbital inclination in the high-mass eclipsing binary system VV?Orionis Thumbnail


Authors

D M Bowman

K Pavlovski



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 ß?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.

Journal Article Type Article
Acceptance Date Dec 7, 2020
Online Publication Date Dec 16, 2020
Publication Date Feb 1, 2021
Publicly Available Date May 30, 2023
Journal Monthly Notices of the Royal Astronomical Society: Letters
Publisher Oxford University Press
Peer Reviewed Peer Reviewed
Volume 501
Issue 1
Pages L65 - L70
DOI https://doi.org/10.1093/mnrasl/slaa197
Keywords stars, binaries, eclipsing, fundamental parameters, oscillations
Publisher URL https://doi.org/10.1093/mnrasl/slaa197

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