Unexplained phenomena related to the spin rates of young low mass stars still remain. Half of the young solar mass stars rotate very slow (<10km/s) and this is a contradiction because they are still in the process of contracting and are accreting material with high angular momentum from the circumstellar disk. Two explanations have been proposed: Magnetic connection between star and disk and stellar winds powered by accretion. High resolution optical spectra can help to distinguish among these scenarios and in particular to determine the disk accretion, outflow and equatorial projected velocities. We propose to conduct observations with the optical spectrograph ESPADOSN at the 3.5m CFHT Telescope of 6 T Tauri stars in MBM12 (~2Myr), the nearest molecular cloud in Northern Hemisphere. With these data we will able to determine under what conditions a spin-down torque from stellar winds may significantly affect the spin evolution at the earliest ages.