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Gas Flow across Gaps in Protoplanetary Disks

Open access
Lubow, S. H., D’Angelo, G.·2006·The Astrophysical Journal

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 ~1 M J 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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Metadata

Authors
Lubow, S. H., & D’Angelo, G.
Venue
The Astrophysical Journal
Published
2006-04-10
Volume
641
Issue
1
Pages
526-533
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
OpenAlex
W2038574798
Cited by
272
References
24
FWCI
7.52
Type
journal article
Language
en
Open access
bronze

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CoChat. (2026). Citation check: Gas Flow across Gaps in Protoplanetary Disks. https://app.cochat.ai/papers/10.1086/500356
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Lubow, S. H., & D’Angelo, G. (2006). Gas Flow across Gaps in Protoplanetary Disks. The Astrophysical Journal. https://doi.org/10.1086/500356

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Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).

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