Protoplanetary disks are quasi-steady structures whose evolution and dispersal determine
the environment for planet formation. I review the theory of protoplanetary disk evolution and …

Thin, Keplerian accretion disks generically become gravitationally unstable at large radii. I
investigate the nonlinear outcome of such instability in cool disks using razor-thin, local …

We study protoplanetary disc evolution assuming that angular momentum transport is driven
by gravitational instability at large radii, and magnetohydrodynamic (MHD) turbulence in the …

In this paper, we examine the issue of characterizing the transport associated with
gravitational instabilities in relatively cold discs, discussing in particular the conditions under …

The evolution of gravitationally unstable protoplanetary gaseous disks has been studied
with the use of three-dimensional smoothed particle hydrodynamics simulations with …

Gas giant planets have been detected in orbit around an increasing number of nearby stars.
Two theories have been advanced for the formation of such planets: core accretion and disk …

I review the basic physical processes that determine the evolution of accretion discs. I first
introduce the main properties of discs observed around young stars across the mass …

ABSTRACT I argue for two modes of gas giant planet formation and discuss the conditions
under which each mode operates. Gas giant planets at disk radii r> 100 AU are likely to form …

In this paper we consider the evolution of small planetesimals (radii∼ 1–10 m) in marginally
stable, self-gravitating protoplanetary discs. The drag force between the disc gas and the …

Submillimetre images of transition discs are expected to reflect the distribution of the
optically thin dust. Former observation of three transition discs LkHα 330, SR 21N and HD …