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Astrophysics of Planet Formation
Preface 1. Observations of planetary systems 2. Protoplanetary disk structure 3. Protoplanetary disk evolution 4. Planetesimal formation 5. Terrestrial planet formation 6. Giant planet formation 7.Expand
Investigating fragmentation conditions in self-gravitating accretion discs
The issue of fragmentation in self-gravitating gaseous accretion discs has implications both for the formation of stars in discs in the nuclei of active galaxies, and for the formation of gaseousExpand
Massive black hole binary mergers within subparsec scale gas discs
We study the efficiency and dynamics of supermassive black hole binary mergers driven by angular momentum loss to small-scale gas discs. Such binaries form after major galaxy mergers, but their fateExpand
Dynamics of Protoplanetary Disks
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 its connectionExpand
Accretion during the Merger of Supermassive Black Holes
We study the evolution of disk accretion during the merger of supermassive black hole binaries in galactic nuclei. In hierarchical galaxy formation models, the most common binaries are likely toExpand
Episodic accretion in magnetically layered protoplanetary discs
We study protoplanetary disc evolution assuming that angular momentum transport is driven by gravitational instability at large radii, and magnetohydrodynamic (MHD) turbulence in the hot innerExpand
Turbulence and Angular Momentum Transport in a Global Accretion Disk Simulation
The global development of magnetohydrodynamic turbulence in an accretion disk is studied within a simplified disk model that omits vertical stratification. Starting with a weak vertical seed field, aExpand
The effect of cooling on the global stability of self-gravitating protoplanetary discs
Using a local model, Gammie has shown that accretion discs with cooling times tcool ≤ 3Ω−1 fragment into gravitationally bound objects, while those with cooling times tcool > 3Ω−1 evolve into aExpand
Emergent mesoscale phenomena in magnetized accretion disc turbulence
We study how the structure and variability of magnetohydrodynamic (MHD) turbulence in accretion discs converge with domain size. Our results are based on a series of vertically stratified localExpand
A Three-Dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk using DCO$^+$
Gas kinematics are an important part of the planet formation process. Turbulence influences planetesimal growth and migration from the scale of sub-micron dust grains through gas-giant planets. RadioExpand
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