Internal rotation and mixing in the massive star HD192575
- 1. Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
- 2. Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain & Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain
- 3. Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium & Department of Astrophysics, IMAPP, Radboud University Nijmegen, 6500 GL Nijmegen, The Netherlands & Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
Description
The evolution of high mass stars (>8M_sun) is strongly dictated by their interior structure, specifically the mixing processes near the core and in the surrounding envelope. Asteroseismology can open up these stellar interiors but unfortunately Kepler did not provide any high-mass stars with identified modes for this endeavour. The TESS space mission is remedying this by observing a large number of high-mass stars allowing us to construct an asteroseismic sample of OB pulsators and open up the way to their asteroseismic sounding.
In this poster we present a detailed analysis of the high-mass pulsator HD192575 (B0.5 V) using its 1-year TESS light curve. HD192575 is among the first of its variability class to be observed uninterruptedly during such a long time and the resulting high frequency precision of the measured pulsations allows for in-depth modelling. In our novel modelling strategy we use a maximum likelihood estimator which incorporates correlations among the parameters and theoretical uncertainties due to unknown input physics of stellar models. This allows us to derive a precise mass, internal mixing, and age from zonal modes, as well as its interior rotation from detected rotationally split multiplets of low-degree modes.
