Formation of close-in super-Earths in evolving protoplanetary disks due to disk winds

Abstract

Planets with masses larger than about 0.1 Earth-masses undergo rapid inward migration (type I migration) in a standard protoplanetary disk. Recent magnetohydrodynamical simulations revealed the presence of magnetically driven disk winds, which would alter the disk profile and the type I migration in the close-in region. We investigate orbital evolution of planetary embryos in disks that viscously evolve under the effects of disk winds. The aim is to discuss effects of altered disk profiles on type I migration. In addition, we aim to examine whether observed distributions of close-in super-Earths can be reproduced by simulations that include effects of disk winds. We perform N-body simulations of super-Earth formation from planetary embryos, in which a recent model for disk evolution is used. We explore a wide range of parameters and draw general trends. We also carry out N-body simulations of close-in super-Earth formation from embryos in such disks under various conditions. We find that the type I migration is significantly suppressed in many cases. Even in cases in which inward migration occurs, the migration timescale is lengthened to 1 Myr, which mitigates the type I migration problem. This is because the gas surface density is decreased and has a flatter profile in the close-in region due to disk winds. We find that when the type I migration is significantly suppressed, planets undergo late orbital instability during the gas depletion, leading to a non-resonant configuration. We also find that observed distributions of close-in super-Earths (e.g., period ratio, mass ratio) can be reproduced. In addition, we show that in some results of simulations, systems with a chain of resonant planets, like the TRAPPIST-1 system, form.

arXiv comment18 pages, 19 figures, accepted for publication in A&A

References in corpus (35)

• The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets
• Planet Occurrence within 0.25 AU of Solar-type Stars from Kepler
• A torque formula for non-isothermal Type I planetary migration - II. Effects of diffusion
• Wind-driven Accretion in Protoplanetary Disks. I: Suppression of the Magnetorotational Instability and Launching of the Magnetocentrifugal Wind
• A torque formula for non-isothermal Type I planetary migration - I. Unsaturated horseshoe drag
• Toward a Deterministic Model of Planetary Formation V. Accumulation Near the Ice Line
• Breaking the Chains: Hot Super-Earth systems from migration and disruption of compact resonant chains
• The California-Kepler Survey V. Peas in a Pod: Planets in a Kepler Multi-planet System are Similar in Size and Regularly Spaced
• Formation of the Terrestrial Planets from a Narrow Annulus
• Migration then assembly: Formation of Neptune mass planets inside 1 AU
• Global simulations of protoplanetary disks with ohmic resistivity and ambipolar diffusion
• Disk Winds Driven by Magnetorotational Instability and Dispersal of Proto-Planetary Disks
• Global simulations of protoplanetary disks with net magnetic flux: I. Non-ideal MHD case
• Testing In Situ Assembly with the Kepler Planet Candidate Sample
• Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc
• Evolution of Protoplanetary Discs with Magnetically Driven Disc Winds
• N-body simulations of planetary accretion around M dwarf stars
• Protoplanetary Disk Winds by Magnetorotational Instability : Formation of an Inner Hole and a Crucial Assist for Planet Formation
• Magnetically driven accretion in protoplanetary discs
• Local outflows from turbulent accretion disks
• Hot super-Earths and giant planet cores from different migration histories
• Wind-driven Accretion in Protoplanetary Disks --- II: Radial Dependence and Global Picture
• MHD Simulations of Global Accretion Disks with Vertical Magnetic Fields
• Dynamical corotation torques on low-mass planets
• Migration of Earth-size planets in 3D radiative discs
• A reassessment of the in situ formation of close-in super-Earths
• Accretion of Terrestrial Planets from Oligarchs in a Turbulent Disk
• The Orbital Stability of Planets Trapped in the First-Order Mean-Motion Resonances
• Condition for Capture into First-order Mean Motion Resonances and Application to Constraints on Origin of Resonant Systems
• Suppression of type I migration by disk winds
• Low mass planet migration in magnetically torqued dead zones - I. Static migration torque
• Formation of the terrestrial planets in the solar system around 1 au via radial concentration of planetesimals
• Formation of terrestrial planets in disks evolving via disk winds and implications for the origin of the solar system's terrestrial planets
• Planetary Torque in 3D Isentropic Disks
• Effects of global gas flows on type I migration

Cited by in corpus (57)

• Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
• The Nature of the Radius Valley: Hints from Formation and Evolution Models
• The New Generation Planetary Population Synthesis (NGPPS). IV. Planetary systems around low-mass stars
• The New Generation Planetary Population Synthesis (NGPPS). I. Bern global model of planet formation and evolution, model tests, and emerging planetary systems
• Influence of sub- and super-solar metallicities on the compositions of solid planetary building blocks
• The Exoplanet Radius Valley from Gas-driven Planet Migration and Breaking of Resonant Chains
• The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines
• A Tale of Planet Formation: From Dust to Planets
• Giant planet formation at the pressure maxima of protoplanetary disks II. A hybrid accretion scenario
• Constraining MHD disk winds with ALMA. Apparent rotation signatures and application to HH212
• Most super-Earths formed by dry pebble accretion are less massive than 5 Earth masses
• A Balanced Budget View on Forming Giant Planets by Pebble Accretion
• HD219666b: A hot-Neptune from TESS Sector 1
• Three-dimensional Global Simulations of Type-II Planet-disk Interaction with a Magnetized Disk Wind: I. Magnetic Flux Concentration and Gap Properties
• Giants are bullies: how their growth influences systems of inner sub-Neptunes and super-Earths
• Molecules with ALMA at Planet-forming Scales (MAPS) XVI: Characterizing the impact of the molecular wind on the evolution of the HD 163296 system
• Sub-Neptune Formation: The View from Resonant Planets
• Formation of the terrestrial planets in the solar system around 1 au via radial concentration of planetesimals
• Breaking Resonant Chains: Destabilization of Resonant Planets due to Long-term Mass Evolution
• Setting the Stage: Planet formation and Volatile Delivery
• A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130)
• The effect of a strong pressure bump in the Sun's natal disk: Terrestrial planet formation via planetesimal accretion rather than pebble accretion
• Do the TRAPPIST-1 Planets Have Hydrogen-rich Atmospheres?
• How to make giant planets via pebble accretion
• N-body simulations of planet formation via pebble accretion II. How various giant planets form
• Unified simulations of planetary formation and atmospheric evolution: Effects of pebble accretion, giant impacts, and stellar irradiations on super-Earth formation
• The "Breaking The Chains" migration model for super-Earths formation: the effect of collisional fragmentation
• When, where, and how many planets end up in first-order resonances?
• Inner rocky super-Earth formation: distinguishing the formation pathways in viscously heated and passive discs
• Habitable planet formation around low-mass stars: Rapid accretion, rapid debris removal and the essential contribution of external giants
• Close-in Super-Earths: The first and the last stages of planet formation in an MRI-accreting disc
• Unified simulations of planetary formation and atmospheric evolution II: Rapid disk clearing by photoevaporation yields low-mass super-Earth atmospheres
• Formation of giant planets with large metal masses and metal fractions via giant impacts in a rapidly dissipating disk
• TRAPPIST-1: Dynamical analysis of the transit-timing variations and origin of the resonant chain
• Radial migration of gap-opening planets in protoplanetary disks. II. The case of a planet pair
• Promoted Mass Growth of Multiple, Distant Giant Planets through Pebble Accretion and Planet-Planet Collision
• Ejection of close-in super-Earths around low-mass stars in the giant impact stage
• Formation of Planetary Populations II: Effects of Initial Disk Size & Radial Dust Drift
• Effects of Planetesimal Scattering: Explaining the Observed Offsets from Period Ratios 3:2 and 2:1
• Size evolution of close-in super-Earths through giant impacts and photoevaporation
• The growth of super-Earths: the importance of a self-consistent treatment of disc structures and pebble accretion
• Departure from the Exact Location of Mean Motion Resonances Induced by the Gas Disk in the Systems Observed by Kepler
• Near Mean Motion Resonance of Terrestrial Planet Pair Induced by Giant Planet: Application to Kepler-68 System
• Combined Effects of Disk Winds and Turbulence-Driven Accretion on Planet Populations
• A limit on gas accretion onto close-in super-Earth cores from disk accretion
• Rapid-then-slow migration reproduces mass distribution of TRAPPIST-1 system
• How Flow Isolation May Set the Mass Scale for Super-Earth Planets
• The New Generation Planetary Population Synthesis (NGPPS). VII. Statistical comparison with the HARPS/Coralie survey
• Forming rocky exoplanets around K-dwarf stars
• Time-dependent evolution of the protoplanetary discs with magnetic winds
• Diversity of disc viscosities can explain the period ratios of resonant and non-resonant systems of hot super-Earths and mini-Neptunes
• Can Planets Exist in the Habitable Zone of 55~Cancri?
• The stability of unevenly spaced planetary systems
• Higher-Order Mean-Motion Resonances Can Form in Type-I Disk Migration
• Predicting the Dominant Formation Mechanism of Multi-Planetary Systems
• Forming Earth-like and Low-Mass Rocky Exoplanets Through Pebble and Planetesimal Accretion
• Early Initiation of Inner Solar System Formation at Dead-Zone Inner Edge