Analysing interior characteristics of pulsating hot subdwarf B stars

Hot subdwarf B (sdB) stars are evolved, subluminous, helium-burning stars, most likely formed when red-giant stars lose their hydrogen envelope via interactions with close companions. They play an important role in our understanding of binary evolution, stellar atmospheres, and interiors. Among sdBs, only a small fraction pulsate. Recent space missions, notably Kepler, then K2, and now TESS, have revolutionized our comprehension of sdBs and have provided unprecedented access to asteroseismic measurements and tools for pulsating sdB stars. In this poster, we present a study that delves into convective boundary treatment during the helium-burning phase, with a particular focus on the convective premixing method and its impact on the evolution of the convective core in the pulsating sdB star KIC 10001893, which was extensively observed by the Kepler spacecraft. We identify three distinct stages in the convective premixing approach, and our analysis of asteroseismic characteristics and modelling of period spacings reveal the mode trapping due to compositional changes near the core. Our research explores various parameters related to period spacings across different stages of helium burning and suggests that using the distance parameter, which represents the average distances between deep trapped modes during the second stage of sdB evolutionary models, is a viable approach for describing the core helium-burning phase.