  In the poster presented in Cool Star 15, we analyzed the effect of disk
accretion on the evolution of very low mass pre-main sequence stars and young
brown dwarfs and the resulting uncertainties on the determination of masses and
ages. We use the Lyon evolutionary 1-D code assuming a magnetospheric accretion
process, i.e., the material falls covering a small area of the radiative
surface, and we take into account the internal energy added from the accreted
material as a free parameter $\epsilon$. Even if the approach to this problem
is phenomenological, our formalism provides important hints about
characteristics of disk accretion, which are useful for improved stellar
interior calculations. Using the accretion rates derived from observations our
results show that accretion does not affect considerably the position of
theoretical isochrones as well as the luminosity compared with standard
non-accreting models. See more discussions in a forthcoming paper by Gallardo,
Baraffe and Chabrier (2008).
