MHD disc winds can reproduce fast disc dispersal and the correlation
  between accretion rate and disc mass in Lupus
  The final architecture of planetary systems depends on the extraction of
angular momentum and mass-loss processes of the discs in which they form.
Theoretical studies proposed that magnetized winds launched from the discs (MHD
disc winds) could govern accretion and disc dispersal. In this work, we revisit
the observed disc demographics in the framework of MHD disc winds, combining
analytical solutions of disc evolution and a disc population synthesis
approach. We show that MHD disc winds alone can account for both disc dispersal
and accretion properties. The decline of disc fraction over time is reproduced
by assuming that the initial accretion timescale (a generalization of the
viscous timescale) varies from disc to disc and that the decline of the
magnetic field strength is slower than that of the gas. The correlation between
accretion rate and disc mass, and the dispersion of the data around the mean
trend as observed in Lupus is then naturally reproduced. The model also
accounts for the rapidity of the disc dispersal. This paves the way for planet
formation models in the paradigm of wind-driven accretion.
