On the detection of oscillations in pre-Main Sequence low mass stars

On their evolution to the Main-Sequence (HS), young low mass stars do not cross the instability strip. However; due to the presence of convection in their envelopes, these stars are expected to display solar like oscillations. The potential of rising seismology for constraining the pre-main sequence evolution (PMS) of low mass stars makes them very, interesting seismic targets. We present a series of simulations aiming at estimating the viability of detecting oscillations in these highly active stars. We do so by simulating periodic signals; covering a representative range of frequencies; amplitudes and time samplings, superimposed on data based on observations of T Tauri stars (TTS). In doing so we try to establish under what conditions the oscillations can be extracted from the strongly variable photometric light curves of these stars.