TOWARD A DETERMINISTIC MODEL OF PLANETARY FORMATION. VI. DYNAMICAL INTERACTION AND COAGULATION OF MULTIPLE ROCKY EMBRYOS AND SUPER-EARTH SYSTEMS AROUND SOLAR-TYPE STARS

By Shigeru Ida, D. Lin. 2010

161 citations recorded by the source corpus.

Radial velocity and transit surveys indicate that solar-type stars bear super-Earths, with masses up to ∼20 M⊕ and periods up to a few months, that are more common than those with Jupiter-mass gas giants. In many cases, these super-Earths are members of multiple-planet systems in which their mutual dynamical interaction has influenced their formation and evolution. In this paper, we modify an existing numerical population synthesis scheme to take into account protoplanetary embryos’ interaction with their evolving natal gaseous disks, as well as their close scatterings and resonant interaction with each other. We show that it is possible for a group of compact embryos to emerge interior to the ice line, grow, migrate, and congregate into closely packed convoys which stall in the proximity of their host stars. After the disk–gas depletion, they undergo orbit crossing, close scattering, and giant impacts to form multiple rocky Earths or super-Earths in non-resonant orbits around ∼0.1 AU with moderate eccentricities of ∼0.01–0.1. We suggest that most refractory super-Earths with periods in the range of a few days to weeks may have formed through this process. These super-Earths differ from Neptune-like ice giants by their compact sizes and lack of a substantial gaseous envelope.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d253d71962a633e6686465f55cdff88038a381e3

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In Astronomy and Astrophysics

1. Jon Fortney
2. D. Charbonneau
3. Timothy Morton
4. G. Marcy
5. J. Johnson
6. C. Mordasini
7. J. Winn
8. Andrew W. Howard

Citations in the corpus

• Spacing of Kepler Planets: Sculpting by Dynamical Instability (2015, background): “Dynamical Scuplting The formation of Kepler planets themselves is not yet understood and different theories have been proposed (Terquem & Papaloizou 2007; Ida & Lin 2010; Hansen & Murray 2012; Chiang & Laughlin 2013; Chatterjee & Tan 2014).”
• Planet-Disk Interaction and Orbital Evolution (2012, background): “Ida & Lin (2010) recently considered the formation of super-Earths using population synthesis.”
• Breaking the chains: hot super-Earth systems from migration and disruption of compact resonant chains (2017, background): “…Ogihara, Morbidelli & Guillot 2015a,b) or (2) assembly of planets at moderate or larger distances from the star followed by inward gas-driven migration (Terquem & Papaloizou 2007; Ida & Lin 2008, 2010; McNeil & Nelson 2010; Hellary & Nelson 2012; Cossou et al. 2014; Coleman & Nelson 2014, 2016).”
• The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths (2012, background): “50 days (Ida & Lin 2010; Howard et al. 2010; Howard et al. 2012, and references therein).”
• TESTING IN SITU ASSEMBLY WITH THE KEPLER PLANET CANDIDATE SAMPLE (2013, background): “…due to large-scale, post-assembly planetary migration in this calculation, it could potentially be the alternative contributing process we seek, especially if the late-time instability of resonant chains (Terquem & Papaloizou 2007; Ida & Lin 2010) produces primarily systems of low multiplicity.”
• HOW THERMAL EVOLUTION AND MASS-LOSS SCULPT POPULATIONS OF SUPER-EARTHS AND SUB-NEPTUNES: APPLICATION TO THE KEPLER-11 SYSTEM AND BEYOND (2012, background): “Furthermore, the co-planar, tightly packed, circular orbits in the system strongly suggest that it could have undergone Type 1 migration (Ida & Lin 2010).”
• COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. I. OUTCOME REGIMES AND SCALING LAWS (2011, background): “Recently, the distribution of stable planets has been investigated in population synthesis models (e.g., Mordasini et al. 2009; Ida & Lin 2010; Schlaufman et al. 2010; Alibert et al. 2011).”
• Compositional Imprints in Density–Distance–Time: A Rocky Composition for Close-in Low-mass Exoplanets from the Location of the Valley of Evaporation (2017, background): “These cases represent limiting cases of the different theories for the formation of the numerous class of close-in, low-mass planets (e.g., Ida & Lin 2010; Chiang & Laughlin 2013; Raymond & Cossou 2014; Baruteau et al. 2016).”
• COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. II. THE DIVERSITY OF IMPACT OUTCOMES DURING THE END STAGE OF PLANET FORMATION (2011, methodology): “…purpose of this Monte Carlo simulation is to investigate the effects of the collision physics model and is not meant to replace full N -body planet formation models or more sophisticated statistical population synthesis models (e.g., Alibert et al. 2011; Mordasini et al. 2009a,b; Ida & Lin 2010).”
• PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER (2011, background): “The relevant processes, including inward migration, have been simulated numerically both for individual planet growth and for entire populations of planets (Ida & Lin 2004, 2008b; Mordasini et al. 2009a; Schlaufman et al. 2010; Ida & Lin 2010; Alibert et al. 2011).”
• TRANSIT TIMING OBSERVATIONS FROM KEPLER. IV. CONFIRMATION OF FOUR MULTIPLE-PLANET SYSTEMS BY SIMPLE PHYSICAL MODELS (2012, background): “Previously for systems of super-Earths, theorists (Terquem & Papaloizou 2007; McNeil & Nelson 2010; Ida & Lin 2010; Liu et al. 2011; Pierens et al. 2011) have suggested planets could be about this close to one another and trapped in resonances, but they have always focused on first-order resonances.”
• Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, background): “The effects induced by the concurrent formation of many protoplanets (see Thommes et al. 2008; Ida & Lin 2010; Hellary & Nelson 2012) like for example capture into meanmotion resonances, competition for gas and solids, or effects of the eccentricity onto the migration, cannot be described in the…”
• The habitability of Proxima Centauri b. I. Irradiation, rotation and volatile inventory from formation to the present (2016, background): “…can be explained if planetary embryos formed at several AU, migrated inward to the inner edge of the protoplanetary disk and underwent a late phase of collisions (Terquem & Papaloizou 2007; Ida & Lin 2010; McNeil & Nelson 2010; Swift et al. 2013; Cossou et al. 2014; Izidoro & et al. 2016).”
• IN SITU FORMATION AND DYNAMICAL EVOLUTION OF HOT JUPITER SYSTEMS (2015, methodology): “Here, we make no attempt at a population synthesis-type study (see e.g. Ida and Lin 2005), and instead aim to elucidate a single, fundamental process that acts to sculpt the final architectures of the observed planetary systems.”
• A PLATEAU IN THE PLANET POPULATION BELOW TWICE THE SIZE OF EARTH (2013, methodology): “The population synthesis models of Ida & Lin (2010) and Mordasini et al. (2012) suggest that they form near or beyond the ice line and then migrate quiescently in the protoplanetary disk.”
• Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, background): “Further growth from these masses to the final masses by giant impacts (e.g. Marcus et al. 2010) will then only occur after the damping influence of the gas disk is gone (Ida & Lin 2010), a phase which is however not included in our model at the moment.”