Self-consistent dynamical and thermodynamical evolutions of protoplanetary disks

Astronomical observations reveal the diversity of protoplanetary disk evolutions. In order to understand the global evolution of these disks from their birth, during the collapse of the molecular cloud, to their evaporation because of the stellar radiation, many processes with different timescales must be coupled: stellar evolution, thermodynamical evolution, photoevaporation, cloud collapse, viscous spreading... By modeling the results of large scale simulations and coupling them with models of viscous evolution, we have designed a one dimension full model of disk evolution for which most parameters are self-consistently calculated at each time step. We integrate the Hueso and Guillot, 2005 model of disk evolution and couple the radiative transfer description of Calvet et al, 1991 allowing us to handle a non-isothermal disk. We also take into account the collapse of the molecular cloud that feeds the disk. Using the same temperature model in the vertical direction, we estimate 2D thermal maps of the disk. The central star itself is modeled using recent stellar evolution code described in Piau et al, 2011. We first test our model in the case of an already formed Minimum Mass solar Nebula, trying to match the observational constraints on the radial surface density gradients and photosphere height profiles of the Taurus-Auriga or Ophiucus disks for instance. We then follow the full long-term evolution of a disk fed by the collapse of the molecular cloud. We estimate disk temperatures and accretion rates and try to constrain the favourable zone for the formation of the first solids. This will help targeting future JWST observations.