2023
DOI: 10.3847/2041-8213/acc015
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Dissipative Capture of Planets into First-order Mean-motion Resonances

Abstract: The emergence of orbital resonances among planets is a natural consequence of the early dynamical evolution of planetary systems. While it is well established that convergent migration is necessary for mean-motion commensurabilities to emerge, recent numerical experiments have shown that the existing adiabatic theory of resonant capture provides an incomplete description of the relevant physics, leading to an erroneous mass scaling in the regime of strong dissipation. In this work, we develop a new model for r… Show more

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Cited by 7 publications
(6 citation statements)
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“…Resonances are naturally associated with convergent migration (when two planets orbit the same star embedded in the same protoplanetary disk and the sizes of their orbits change in such a way that the orbits get closer to each other, Terquem & Papaloizou 2007;Cresswell & Nelson 2008;Morbidelli et al 2008). This process is well understood on theoretical grounds (e.g., Batygin & Morbidelli 2013;Batygin 2015), and in particular, it is known that which mean motion resonances are skipped and which ones are successfully established depends on the orbital damping timescales (Batygin 2015;Deck & Batygin 2015;Xu et al 2018;Batygin & Petit 2023), and so do the final eccentricities after successfully capturing in a given mean motion resonance (Papaloizou & Szuszkiewicz 2005;Crida et al 2008;Goldreich & Schlichting 2014;Deck & Batygin 2015;Pichierri et al 2018). We show simple examples in which our modified formulas for orbital damping timescales for partial-gap opening planets yield dynamically different results than the prescriptions used so far in the literature, and we stress in what way this would impact the orbital states obtained at the end of population synthesis models.…”
Section: Discussionmentioning
confidence: 99%
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“…Resonances are naturally associated with convergent migration (when two planets orbit the same star embedded in the same protoplanetary disk and the sizes of their orbits change in such a way that the orbits get closer to each other, Terquem & Papaloizou 2007;Cresswell & Nelson 2008;Morbidelli et al 2008). This process is well understood on theoretical grounds (e.g., Batygin & Morbidelli 2013;Batygin 2015), and in particular, it is known that which mean motion resonances are skipped and which ones are successfully established depends on the orbital damping timescales (Batygin 2015;Deck & Batygin 2015;Xu et al 2018;Batygin & Petit 2023), and so do the final eccentricities after successfully capturing in a given mean motion resonance (Papaloizou & Szuszkiewicz 2005;Crida et al 2008;Goldreich & Schlichting 2014;Deck & Batygin 2015;Pichierri et al 2018). We show simple examples in which our modified formulas for orbital damping timescales for partial-gap opening planets yield dynamically different results than the prescriptions used so far in the literature, and we stress in what way this would impact the orbital states obtained at the end of population synthesis models.…”
Section: Discussionmentioning
confidence: 99%
“…The processes of resonant capture and which resonances will be built under which conditions are fairly well understood (Batygin 2015;Deck & Batygin 2015;Pichierri et al 2018;Batygin & Petit 2023). A mean motion resonance can be skipped if the resonance crossing time for the two planets is comparable to or shorter than the period of the planets' resonant interaction (the so-called adiabatic limit, which is a condition on the torque), or if the dissipative torque is simply stronger than the resonant torque (which is a condition on the relative diskdriven e-damping onto the planets; Batygin 2015; Batygin & Petit 2023).…”
Section: Application To N-body Integrationsmentioning
confidence: 99%
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“…We stress again that convergent migration is only a necessary condition to maintain MMR. The capture probability also depends on the eccentricities and the migration and eccentricity damping rates (Mustill & Wyatt 2011;Goldreich & Schlichting 2014;Batygin & Petit 2023;Huang & Ormel 2023;Kajtazi et al 2023).…”
Section: Conditions For Convergent Migration Of Two Planetsmentioning
confidence: 99%
“…For example, a variable mass budget available in pebbles could regulate the formation and migration of either Earth-like or super-Earth-like planets in the terrestrial zone (Lambrechts et al, 2019b). Disc evolution in turn regulates migration rates and resonant-trapping of planet systems (Kajtazi et al, 2023;Batygin and Petit, 2023;Huang and Ormel, 2023). Finally, the composition of planets is a complex product of the full planetary growth process, starting from the growth and drift of primordial dust grains (e.g.…”
Section: Constraints On Planet Formation and Evolutionmentioning
confidence: 99%