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Title:
Gas Flow across Gaps in Protoplanetary Disks
Authors:
Lubow, S. H.; D'Angelo, G.
Affiliation:
AA(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218; Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. ), AB(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL, UK )
Publication:
The Astrophysical Journal, Volume 641, Issue 1, pp. 526-533. (ApJ Homepage)
Publication Date:
04/2006
Origin:
UCP
Astronomy Keywords:
Accretion, Accretion Disks, Hydrodynamics, Stars: Planetary Systems: Protoplanetary Disks, Planets and Satellites: General
DOI:
10.1086/500356
Bibliographic Code:
2006ApJ...641..526L

Abstract

We analyze the gas accretion flow through a planet-produced gap in a protoplanetary disk. We adopt the α-disk model and ignore effects of planetary migration. We develop a semianalytic, one-dimensional model that accounts for the effects of the planet as a mass sink and also carry out two-dimensional hydrodynamic simulations of a planet embedded in a disk. The predictions of the mass flow rate through the gap based on the semianalytic model generally agree with the hydrodynamic simulations at the 25% level. Through these models, we are able to explore steady state disk structures and over large spatial ranges. The presence of an accreting ~1MJ planet significantly lowers the density of the disk within a region of several times the planet's orbital radius. The mass flow rate across the gap (and onto the central star) is typically 10%-25% of the mass accretion rate outside the orbit of the planet, for planet-to-star mass ratios that range from 5×10-5 to 1×10-3.
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