The Accretion Process in the DQ Tau Binary System

Abstract Mass accretion from the circumstellar disk onto protostar is a fundamental process during star formation. Measuring mass rate particularly challenging for stars belonging to binary systems, because it often difficult discriminate which component accreting. DQ Tau an almost equal-mass spectroscopic system where components orbit each other every 15.8 days. The known display pulsed accretion, i.e., periodic modulation of by on eccentric orbit. We present multi-epoch ESO/Very Large Telescope X-Shooter observations Tau, with aim determining this main accreting source. use absorption lines in spectra determine radial velocity two components, and measure continuum veiling as function wavelength time. fit observed nonaccreting templates correct photospheric chromospheric contribution. In corrected spectra, we study detail profiles emission calculate rates orbital phase. accordance previous findings, detect elevated close periastron. varying between 10 ?8.5 ?7.3 M ? yr ?1 . line suggest that both are actively accreting, dominant accretor not always same component, few orbits.