E. Moravveji

Tight asteroseismic constraints on core overshooting and diffusive mixing in the slowly rotating pulsating B8.3V star KIC 10526294

KIC 10526294 is a very slowly rotating and slowly pulsating late B-type star. Its 19 consecutive dipole gravity modes constitute a series with almost constant period spacing. This unique collection of identified modes probes the near-core environment of this star and holds the potential to reveal the size and structure of the overshooting zone on top of the convective core, as well as the mixing properties of the star. We pursue forward seismic modelling based on adiabatic eigenfrequencies of equilibrium models for eight extensive evolutionary grids tuned to KIC 10526294, by varying the initial mass, metallicity, chemical mixture, and the extent of the overshooting layer on top of the convective core. We examine models for both OP and OPAL opacities and test the occurrence of extra diffusive mixing. We find a tight mass, metallicity relation within the ranges

THE INTERNAL ROTATION PROFILE OF THE B-TYPE STAR KIC 10526294 FROM FREQUENCY INVERSION OF ITS DIPOLE GRAVITY MODES

M

SUB-INERTIAL GRAVITY MODES IN THE B8V STAR KIC 7760680 REVEAL MODERATE CORE OVERSHOOTING AND LOW VERTICAL DIFFUSIVE MIXING

~ 3.13 to 3.25 Msun and

KIC 10526294: a slowly rotating B star with rotationally split, quasi-equally spaced gravity modes

Z

The eccentric massive binary V380 Cyg: revised orbital elements and interpretation of the intrinsic variability of the primary component

~ 0.014 to 0.028. We deduce that an exponentially decaying diffusive core overshooting prescription describes the seismic data better than a step function formulation and derive a value of

ASTEROSEISMIC FINGERPRINTS OF ROTATION AND MIXING IN THE SLOWLY PULSATING B8 V STAR KIC 7760680

f_{ov}

Signatures of internal rotation discovered in the Kepler data of five slowly pulsating B stars

between 0.017 and 0.018. Moreover, the inclusion of extra diffusive mixing with a value of

Detection of solar-like oscillations in the bright red giant stars γ Piscium and θ1 Tauri from a 190-day high-precision spectroscopic multi-site campaign⋆

\log D_{\rm mix}

Kepler sheds new and unprecedented light on the variability of a blue supergiant: Gravity waves in the O9.5Iab star HD 188209

between 1.75 and 2.00 dex (with

Modelling of σ Scorpii, a high-mass binary with a β Cep variable primary component

D_{\rm mix}