Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 467, Issue 4, Pages 4577-4590Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx426
Keywords
accretion, accretion discs; hydrodynamics; celestial mechanics; planet-disc interactions
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Funding
- STFC [ST/L000636/1]
- Science and Technology Facilities Council [ST/P000673/1, ST/L000636/1] Funding Source: researchfish
- STFC [ST/L000636/1, ST/P000673/1] Funding Source: UKRI
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We explore the evolution of the eccentricity of an accretion disc perturbed by an embedded planet whose mass is sufficient to open a large gap in the disc. Various methods for representing the orbit-averaged motion of an eccentric disc are discussed. We characterize the linear instability that leads to the growth of eccentricity by means of hydrodynamical simulations. We numerically recover the known result that eccentricity growth in the disc is possible when the planet-to-star mass ratio exceeds 3 x 10(-3). For mass ratios larger than this threshold, the precession rates and growth rates derived from simulations, as well as the shape of the eccentric mode, compare well with the predictions of a linear theory of eccentric discs. We study mechanisms by which the eccentricity growth eventually saturates into a non-linear regime.
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