Lee Hartmann

TL;DR: In this paper, the authors present two-dimensional hydrodynamic simulations of self-gravitating protostellar disks subject to axisymmetric infall from envelopes and irradiation from the central star, to explore disk fragmentation due to gravitational instability and the fragmented clump evolution.

TL;DR: In this paper, a simplified analysis of the effects of disk accretion on the early evolution of fully convective, low-mass pre-main-sequence stars is presented, but it differs in that the accretion of material occurs over a small area of the stellar surface, such as through a disk or magnetospheric accretion column.

TL;DR: In this paper, the authors use 2D hydrodynamic simulations of viscous disks to examine whether dynamically interacting multiple giant planets can explain the large gaps (spanning over one order of magnitude in radius) inferred for the transitional and pre-transitional disks around T Tauri stars.

TL;DR: In this paper, the authors present two-dimensional simulations of finite, self-gravitating gaseous sheets and suggest that these simple calculations have interesting implications for the gravitational evolution of overall molecular cloud structure, envisioning that such clouds might originate as roughly sheetlike sections of gas accumulated as a result of large-scale flows in the local interstellar medium.