Gap formation in gaseous and planetesimal disks
Roman Rafikov (Princeton University) - 14 Nov at 12:00 noon
Gravitational interaction between astrophysical disks and massive
perturbers embedded in them tends to affect disk surface density
structure, leading in some cases to gap formation. This phenomenon can
occur both in gaseous and planetesimal protoplanetary disks. In the first
case density wave damping is responsible for transfer of the angular
momentum to the disk material and subsequent disk evolution. Using
realistic nonlocal damping prescription it is possible to derive
a limit on a mass of gap forming planet in gaseous protoplanetary disks,
including planetary migration into account. In planetesimal disks
gravitational scattering by planet tries to repel planetesimals away.
This tendency is opposed by planetesimal-planetesimal interactions
giving rise to "viscous" spreading of the disk. There exists a single
parameter characterizing competiton between these processes and
determining critical gap opening mass for planetesimal disks. These gap
clearing phenomena are important for our understanding of planetary
migration and can be the mechanism determining final masses of
terrestrial and giant planets.
The seminar will be held in 501 Campbell Hall.
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