An empirically-derived formula for the shape of planet-induced gaps in protoplanetary disks. (arXiv:1906.11256v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Duffell_P/0/1/0/all/0/1">Paul C. Duffell</a>
This study uses numerical hydrodynamics calculations and a novel method for
densely sampling parameter space to measure the precise shape of a gap opened
by a planet in a gaseous disk, as a function of planet-to-star mass ratio, disk
Mach number, and disk viscosity. Formulas for gap depth and width are
determined, which are combined to form a complete formula for surface density
as a function of radius in the disk. This new analytical formula is compared
with numerically-derived gaps opened by planets ranging from very low masses up
to a few times Jupiter’s mass, and excellent agreement is found over a wide
range of parameter space relevant to planet-disk interactions. A simple-to-use
code is presented to rapidly generate synthetic disk profiles.
This study uses numerical hydrodynamics calculations and a novel method for
densely sampling parameter space to measure the precise shape of a gap opened
by a planet in a gaseous disk, as a function of planet-to-star mass ratio, disk
Mach number, and disk viscosity. Formulas for gap depth and width are
determined, which are combined to form a complete formula for surface density
as a function of radius in the disk. This new analytical formula is compared
with numerically-derived gaps opened by planets ranging from very low masses up
to a few times Jupiter’s mass, and excellent agreement is found over a wide
range of parameter space relevant to planet-disk interactions. A simple-to-use
code is presented to rapidly generate synthetic disk profiles.
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