The PDS 70 system has been subject to many studies in the past year following the discovery of two accreting planets in the gap of its circumstellar disk . Nevertheless , the mass accretion rate onto the star is still not well known . Here we determined the stellar mass accretion rate and its variability based on TESS and HARPS observations . The stellar light curve shows a strong signal with a 3.03 \pm 0.06 days period , which we attribute to stellar rotation . Our analysis of the HARPS spectra shows a rotational velocity of v \sin i = 16.0 \pm 0.5 { km s ^ { -1 } } , indicating that the inclination of the rotation axis is 50 \pm 8 degrees . This implies that the rotation axes of the star and its circumstellar disk are parallel within the measurement error . We apply magnetospheric accretion models to fit the profiles of the H \alpha line and derive mass accretion rates onto the star in the range of 0.6 - 2.2 \times 10 ^ { -10 } { M _ { \odot } yr ^ { -1 } } , varying over the rotation phase . The measured accretion rates are in agreement with those estimated from NUV fluxes using accretion shock models . The derived accretion rates are higher than expected from the disk mass and planets properties for the low values of the viscous parameter \alpha suggested by recent studies , potentially pointing to an additional mass reservoir in the inner disk to feed the accretion , such as a dead zone . We find that the He I \lambda 10830 line shows a blueshifted absorption feature , indicative of a wind . The mass-loss rate estimated from the line depth is consistent with an accretion-driven inner disk MHD wind .