HD 142527 is a young pre-main sequence star with properties indicative of the presence of a giant planet or/and a low-mass stellar companion .
We have analyzed an X-Shooter/Very Large Telescope spectrum to provide accurate stellar parameters and accretion rate .
The analysis of the spectrum , together with constraints provided by the SED fitting , the distance to the star ( 140 \pm 20 pc ) and the use of evolutionary tracks and isochrones , lead to the following set of parameters T _ { eff } = 6550 \pm 100 K , \log g = 3.75 \pm 0.10 , L _ { * } / L _ { \odot } = 16.3 \pm 4.5 , M _ { * } / M _ { \odot } = 2.0 \pm 0.3 and an age of 5.0 \pm 1.5 Myr .
This stellar age provides further constrains to the mass of the possible companion estimated by Biller et al .
( 2012 ) , being in-between 0.20 and 0.35 M _ { \odot } .
Stellar accretion rates obtained from UV Balmer excess modelling , optical photospheric line veiling , and from the correlations with several emission lines spanning from the UV to the near-IR , are consistent to each other .
The mean value from all previous tracers is 2 ( \pm 1 ) \times 10 ^ { -7 } M _ { \odot } yr ^ { -1 } , which is within the upper limit gas flow rate from the outer to the inner disk recently provided by Cassasus et al .
( 2013 ) .
This suggests that almost all gas transferred between both components of the disk is not trapped by the possible planet ( s ) in-between but fall onto the central star , although it is discussed how the gap flow rate could be larger than previously suggested .
In addition , we provide evidence showing that the stellar accretion rate of HD 142527 has increased by a factor \sim 7 on a timescale of 2-5 years .