Abstract
We present the analysis of KIC 7760680, the rotating Slowly Pulsating B-type star identified in the Kepler photometry. The oscillation spectrum of the star exhibits a series of 36 frequencies which are quasi-equally spaced in period. We confirm that this series can be associated with prograde dipole modes of consecutive radial orders. In our studies, the effects of rotation were included in the MESA equilibrium models as well as in the puslational calculations in the framework of the traditional approximation. We find that pulsational models computed with the OPLIB opacities best reproduce the observed frequency range. The modified opacity data with an enhancement of the opacity at $\log T=5.3$, 5.46 and 5.06 were tested as well. Increasing the OPLIB opacities by about 50% at $\log T=5.3$ is sufficient to excite modes in the whole range of 36 frequency peaks of KIC 7760680.
Highlights
KIC 7760680 was classified as the Slowly Pulsating Btype star by Pápics et al [1] who found a series of 36 frequencies quasi- spaced in period from the Kepler photometry
Moravveji et al [2] made a detailed seismic modelling of the star taking into account effects of rotation in the framework of the traditional approximation [e. g., 3–9] applied to the non-rotating MESA [10,11,12] evolutionary models
The reason is that we used rotating evolutionary models which give lower effective temperature for the same mass
Summary
KIC 7760680 was classified as the Slowly Pulsating Btype star by Pápics et al [1] who found a series of 36 frequencies quasi- spaced in period from the Kepler photometry. Moravveji et al [2] made a detailed seismic modelling of the star taking into account effects of rotation in the framework of the traditional approximation [e. The authors found that KIC 7760680 is a moderately rotating star with the rotational frequency amounting to 26% of its Roche break up frequency (0.4805 d−1) and with a mass ∼ 3.25M. They constrained the exponentially decaying convective core overshooting parameter to fov ≈ 0.024 ± 0.001. Their best seismic models employed extra diffusive mixing in the radiative envelope.
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