Please use this identifier to cite or link to this item: http://hdl.handle.net/10773/14996
Title: Stability of resonant configurations during the migration of planets and constraints on disk-planet interactions
Author: Delisle, J. -B.
Correia, A. C. M.
Laskar, J.
Keywords: Celestial mechanics
Pllanets and satellites - dynamical evolution and stability
Planet-disk interactions
Issue Date: Jul-2015
Publisher: EDP Sciences
Abstract: We study the stability of mean-motion resonances (MMR) between two planets during their migration in a protoplanetary disk. We use an analytical model of resonances and describe the effect of the disk by a migration timescale (T-m,T-i) and an eccentricity damping timescale (T-e,T-i) for each planet (i = 1; 2 for the inner and outer planets, respectively). We show that the resonant configuration is stable if T-e,T-1/T-e,T-2 > (e(1)/e(2))(2). This general result can be used to put constraints on specific models of disk-planet interactions. For instance, using classical prescriptions for type-I migration, we show that when the angular momentum deficit (AMD) of the inner orbit is greater than the outer's orbit AMD, resonant systems must have a locally inverted disk density profile to stay locked in resonance during the migration. This inversion is very atypical of type-I migration and our criterion can thus provide an evidence against classical type-I migration. That is indeed the case for the Jupiter-mass resonant systems HD 60532b, c (3: 1 MMR), GJ 876b, c (2: 1 MMR), and HD 45364b, c (3: 2 MMR). This result may be evidence of type-II migration (gap-opening planets), which is compatible with the high masses of these planets.
Peer review: yes
URI: http://hdl.handle.net/10773/14996
DOI: 10.1051/0004-6361/201526285
ISSN: 0004-6361
Appears in Collections:CIDMA - Artigos
DFis - Artigos
GGDG - Artigos

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