SIMBAD references

We present new evolutionary sequences for long lasting accreting low-mass (0.1M_☉≤M≤2.5M_☉) pre-main sequence stars. The calculations, performed for two different mass accretion rates, show that accretion accelerates the evolution of the star. The star has a smaller radius and goes down its convective track faster than in a standard scheme. Consequently, the age of a star, as given by its location on the Hertzsprung-Russell diagram, is lower than that of a non-accreting star. We discuss ²H and ⁷Li burning and show how accretion affects the surface abundance of these elements. Notably, we point out that deuterium must be present at the surface of accreting intermediate-mass stars. Finally, we estimate the age, mass and radius of a sample of T Tauri stars located in the Taurus Auriga star forming region.