A β Cephei pulsator and a changing orbital inclination in the high-mass eclipsing binary system VV Orionis (CROSBI ID 288591)
Prilog u časopisu | Pismo (znanstveno) | međunarodna recenzija
Podaci o odgovornosti
Southworth, J. ; Bowman, D. M. ; Pavlovski, Krešimir
engleski
A β Cephei pulsator and a changing orbital inclination in the high-mass eclipsing binary system VV Orionis
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.
binary stars, eclipsing binaries, fundamental parameters, stellar oscillations
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Podaci o izdanju
501
2021.
L65-L70
objavljeno
1745-3933
10.1093/mnrasl/slaa197