The Pre-main Sequence: Challenges and Prospects for Asteroseismology

Stars do not simply pop up on the main sequence. Before stars arrive zero-age sequence, they form in collapses of molecular clouds, gain matter through accretion processes, and compress their cores until hydrogen can burn full equilibrium. Although this evolutionary phase lasts a relatively short time, it is imprint these important physical processes that often ignored by simplified assumptions. While asteroseismology offers great tool to investigate studying pre-MS oscillations turn has potential further advance field. Asteroseismology pre-main sequence faces observational theoretical challenges. The remnants birth environment which still surrounding young causes variability interfere with signal pulsations. lack long time-base satellite observations addition limits applications method. Theoretical models include several assumptions simplifications influence calculation pulsation frequencies excitation properties modes. Keeping all mind, prospects for are manifold. An improved understanding structure stellar objects answer some open questions evolution, including angular momentum transport formation magnetic fields. gyrochronology, example, struggles determine ages youngest clusters, pulsations function as an independent age indicator yielding higher precision single stars. increasing interest astrophysics general early evolution planets illustrates growing importance asteroseismology.