2020
DOI: 10.1093/mnras/staa2112
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The origins of nearly coplanar, non-resonant systems of close-in super-Earths

Abstract: Some systems of close-in “super-Earths” contain five or more planets on non-resonant but compact and nearly coplanar orbits. The Kepler-11 system is an iconic representative of this class of system. It is challenging to explain their origins given that planet-disk interactions are thought to be essential to maintain such a high degree of coplanarity, yet these same interactions invariably cause planets to migrate into chains of mean motion resonances. Here we mine a large dataset of dynamical simulations of su… Show more

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Cited by 21 publications
(20 citation statements)
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“…In the instability scenario, these may be the systems that remained stable and did not experience growth in eccentricity. Or, if they did encounter an instability, they may have experienced a smaller degree of scattering that left them unusually coplanar and circular (Esteves et al 2020).…”
Section: Discussionmentioning
confidence: 99%
“…In the instability scenario, these may be the systems that remained stable and did not experience growth in eccentricity. Or, if they did encounter an instability, they may have experienced a smaller degree of scattering that left them unusually coplanar and circular (Esteves et al 2020).…”
Section: Discussionmentioning
confidence: 99%
“…The answer to this apparent contradiction is not immediately clear. Perhaps impacts often occur before the full dissipation of the gaseous disk (Esteves et al., 2020) such that a thin atmosphere can still be accreted (Lee & Chiang, 2015). Or perhaps resonant chains of planets are spread out by a different mechanism, such as by the magnetospheric rebound migration torque from the expanding disk cavity (Liu et al., 2017).…”
Section: Implied Formation Pathwaysmentioning
confidence: 99%
“…Within the context of "classical" models of planet formation, the present-day architecture of planetary systems was assumed to be inherited from the detailed structure of the protoplanetary disk from which the planets emerged (Cameron 1988). Recent theoretical progress on the origin of the exoplanetary period distribution, as well as the early evolution of the Solar System itself, however, indicates that violent, post-nebular dynamical instabilities may play an important role in sculpting the terminal outcome of the planet formation process (Tsiganis et al 2005;Morbidelli 2010;Izidoro et al 2017;Esteves et al 2020). Unfortunately, this markedly chaotic evolutionary framework renders a deterministic model that unambiguously connects the properties of the planets natal disk with their present-day (observable) attributes an impossibility.…”
Section: Introductionmentioning
confidence: 99%