University of Cambridge > > DAMTP Astro Lunch > Massive Planets (and Other Bodies) in Steady-State Accretion Disks

Massive Planets (and Other Bodies) in Steady-State Accretion Disks

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We describe how massive planets (and binary stars and supermassive black hole binaries) interact with viscous accretion disks. For a sufficiently massive planet (or binary star or SMBH binary), the planet acts as a leaky dam to the accreting material. We quantify the strength of the dam as a function of planet mass, and show how the pileup of material behind the dam could explain transitional disks. We then investigate a massive planet’s migration rate, and explain why the old paradigm (i.e., Type-II) was fundamentally flawed. We also show that planets more massive than a few Jupiter masses (as well as binary stars and SMBH binaries) migrate outwards in viscous accretion disks, a result which could have a range of observational implications.

This talk is part of the DAMTP Astro Lunch series.

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