  In the earliest phases of their evolution, stars gain mass through the
acquisition of matter from their birth clouds. The widely accepted classical
concept of early stellar evolution neglects the details of this accretion phase
and assumes the formation of stars with large initial radii that contract
gravitationally. In this picture, the common idea is that once the stars begin
their fusion processes, they have forgotten their past. By analysing stellar
oscillations in recently born stars, we show that the accretion history leaves
a potentially detectable imprint on the stars' interior structures. Currently
available data from space would allow discriminating between these more
realistic accretion scenarios and the classical early stellar evolution models.
This opens a window to investigate the interior structures of young pulsating
stars that will also be of relevance for related fields, such as stellar
oscillations in general and exoplanet studies.
