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Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains

dc.contributor.authorIZIDORO, André
hal.structure.identifierLund Observatory
dc.contributor.authorBITSCH, Bertram
hal.structure.identifierECLIPSE 2019
dc.contributor.authorRAYMOND, Sean N.
hal.structure.identifierNiels Bohr Institute [Copenhagen] [NBI]
dc.contributor.authorJOHANSEN, Anders
hal.structure.identifierJoseph Louis LAGRANGE [LAGRANGE]
dc.contributor.authorMORBIDELLI, Alessandro
dc.contributor.authorLAMBRECHTS, Michiel
hal.structure.identifierDepartment of Astrophysical and Planetary Sciences [Boulder]
dc.contributor.authorJACOBSON, Seth A.
dc.date.issued2019
dc.identifier.issn0004-6361
dc.description.abstractEnAt least 30% of main sequence stars host planets with sizes between 1 and 4 Earth radii and orbital periods of less than 100 days. We use N-body simulations including a model for gas-assisted pebble accretion and disk-planet tidal interaction to study the formation of super-Earth systems. We show that the integrated pebble mass reservoir creates a bifurcation between hot super-Earths or hot-Neptunes ($\lesssim15M_{\oplus}$) and super-massive planetary cores potentially able to become gas giant planets ($\gtrsim15M_{\oplus}$). Simulations with moderate pebble fluxes grow multiple super-Earth-mass planets that migrate inwards and pile up at the disk's inner edge forming long resonant chains. We follow the long-term dynamical evolution of these systems and use the period ratio distribution of observed planet-pairs to constrain our model. Up to $\sim$95% of resonant chains become dynamically unstable after the gas disk dispersal, leading to a phase of late collisions that breaks the resonant configuration. Our simulations match observations if we combine a dominant fraction ($\gtrsim95\%$) of unstable systems with a sprinkling ($\lesssim5\%$) of stable resonant chains (the Trappist-1 system represents one such example). Our results demonstrate that super-Earth systems are inherently multiple (${\rm N\geq2}$) and that the observed excess of single-planet transits is a consequence of the mutual inclinations excited by the planet-planet instability. In simulations in which planetary seeds are initially distributed in the inner and outer disk, close-in super-Earths are systematically ice-rich. This contrasts with the interpretation that most super-Earths are rocky based on bulk density measurements of super-Earths and photo-evaporation modeling of their bimodal radius distribution. We investigate the conditions needed to form rocky super-Earths. The formation of rocky super-Earths (abridged)
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics - Earth and Planetary Astrophysics
dc.title.enFormation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains
dc.typeArticle de revue
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv1902.08772
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pagesubmitted A&A.
bordeaux.peerReviewedoui
hal.identifierhal-02051777
hal.version1
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-02051777v1
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