Dr John Taylor j.k.taylor@keele.ac.uk
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
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 |
Files
2012.03947.pdf
(1 Mb)
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