An asteroseismic and spectroscopic pipeline for the analysis of structures and rotation profiles of rapidly-rotating main sequence stars

In intermediate- to high-mass main sequence stars, fast rotation distorts the stellar surface and scrambles the oscillation spectra. Through the use of 2D models, 2D oscillation calculations and machine learning algorithms, we were able to develop fast and automated techniques to highlight patterns in the spectra. From those we derive stellar mean densities and internal differential rotation, paving the way for mode identification and inversion techniques for these stars. I also introduce a novel pipeline for the spectroscopy of flattened stars, that use these new asteroseismic diagnostics, allowing us to estimate the fundamental parameters and inclination of rotating stars. The future extensions of both techniques are discussed, to predict how we can couple them to reach a complete description of rotating pulsators on the upper main sequence.
{"references":["Reese, D. R. 2021, A&A, 645, A46"]}