Protoplanetary disk evolution in nearby star-forming regions

Résumé

Earlier Works in the field of protoplanetary disk evolution were primarily based on samples of a few hundred objects at much. They presented conclusive evidences on the overall time-scale for disk dissipation and for the fact that most protoplanetary disks seem to be massive enough in the early years to allow for the formation of a multiple planetary system like our own. The details of the disk dissipation process as a function of basic physical stellar parameters or how it would map to the actual population of known exoplanets were however less coherent, possibly produced by strong selection biases in the relatively small samples. The goal of this work was therefore to perform a statistical and homogeneous treatment of all observations from a larger simple of 2,500 young stars in the Solar Neighborhood to clarify the dependence of the disk dissipation process on the stellar parameters and to try to provide a statistic link between the population of disks and those of known exoplanets a later ages, taking into account the observation biases in both samples (extracto del informe del Dr. Don Bruno Merín Martín).