Asteroseismology of Kepler SPB stars using TESS

The slowly pulsating B stars (SPBs) are main sequence stars pulsating in g-modes. The sensitivity of g-modes to the near-core structure allows these stars to be used as probes of important uncertainties in stellar astrophysics, such as convective boundary mixing and rotation. Some of the most well-studied SPBs were observed by Kepler, which allowed precise frequency extraction from four years of continuous observation. These stars continue to be observed with TESS, typically in spans of two sectors at a time. This presents an opportunity to explore to what extent the non-continuous TESS light curves can reproduce the results of the Kepler light curves. I will present our TESS reanalysis of a sample of SPBs previously observed by Kepler. I will explain our light curve extraction method, based on optimising the signal to noise of pulsation frequencies. I will then compare the extracted frequencies and the forward modelling results between TESS and Kepler. This work provides a benchmark for the performance of TESS light curves in asteroseismic forward modelling of g-mode pulsators. It also demonstrates the variation in performance between stars, highlighting the difficulties of ensemble analyses.