On the detection of oscillations in pre-main sequence low mass stars

Details On the detection of oscillations in pre-main sequence low mass stars On the detection of oscillations in pre-main sequence low mass stars

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.538..385p&link_type=abstract

In: Second Eddington Workshop: Stellar structure and habitable planet finding, 9 - 11 April 2003, Palermo, Italy. Edited by F. F

Physics

Stars: Evolution, Stars: Oscillations, Stars: Pre-Main Sequence

Scientific paper

On their evolution to the Main-Sequence (MS), 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 using 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.

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