Do all gaps in protoplanetary discs host planets?

Abstract

Following the assumption that the disc substructures observed in protoplanetary discs originate from the interaction between the disc and the forming planets embedded therein, we aim to test if these putative planets could represent the progenitors of the currently observed giant exoplanets. We performed N-body simulations assuming initially three, four, five or seven planets. Our model includes pebble and gas accretion, migration, damping of eccentricities and inclinations, disc-planet interaction and disc evolution. We locate the planets in the positions where the gaps in protoplanetary discs have been observed and we evolve the systems for 100Myr including a few Myr of gas disc evolution, while also testing three values of $\alpha$ viscosity. For planetary systems with initially three and four planets we find that most of the growing planets lie beyond the RV detection limit of 5AU and only a small fraction of them migrate into the inner region. We also find that these systems have too low final eccentricities to be in agreement with the observed giant planet population. Systems initially consisting of five or seven planets become unstable after $\approx$40Kyr of integration time. This clearly shows that not every gap can host a planet. The general outcome of our simulations - too low eccentricities - is independent of the disc's viscosity and surface density. Further observations could either confirm the existence of an undetected population of wide-orbit giants or exclude the presence of such undetected population to constrain how many planets hide in gaps even further.

arXiv commentAccepted for publication in A&A

References in corpus (49)

• Spectral Energy Distributions of T Tauri Stars With Passive Circumstellar Disks
• Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70
• On the width and shape of gaps in protoplanetary disks
• Ringed Substructure and a Gap at 1 AU in the Nearest Protoplanetary Disk
• Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region
• A torque formula for non-isothermal Type I planetary migration - II. Effects of diffusion
• The Disk Substructures at High Angular Resolution Project (DSHARP): II. Characteristics of Annular Substructures
• Separating gas-giant and ice-giant planets by halting pebble accretion
• The effect of dust settling on the appearance of protoplanetary disks
• Ring shaped dust accumulation in transition disks
• Breaking the Chains: Hot Super-Earth systems from migration and disruption of compact resonant chains
• Gaps, Rings, and Non-Axisymmetric Structures in Protoplanetary Disks - From Simulations to ALMA Observations
• Evidence of fast pebble growth near condensation fronts in the HL Tau protoplanetary disk
• A Kinematical Detection of Two Embedded Jupiter Mass Planets in HD 163296
• Pebble isolation mass --- scaling law and implications for the formation of super-Earths and gas giants
• Kinematic evidence for an embedded protoplanet in a circumstellar disc
• Dynamical Evolution of the Early Solar System
• The structure of protoplanetary discs around evolving young stars
• How to form planetesimals from mm-sized chondrules and chondrule aggregates
• Orbital and atmospheric characterization of the planet within the gap of the PDS 70 transition disk
• A Circumplanetary Disk Around PDS70c
• Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc
• Radial migration of gap-opening planets in protoplanetary disks. I. The case of a single planet
• How Empty are Disk Gaps Opened by Giant Planets?
• On the Minimum Core Mass for Giant Planet Formation at Wide Separations
• Accelerated planetesimal growth in self-gravitating protoplanetary discs
• Multiple Disk Gaps and Rings Generated by a Single Super-Earth
• Gap Opening by Extremely Low Mass Planets in a Viscous Disk
• Formation of planetary systems by pebble accretion and migration: Growth of gas giants
• Stellar irradiated discs and implications on migration of embedded planets I: equilibrium discs
• Orbital evolution of eccentric planets in radiative discs
• Thresholds for Particle Clumping by the Streaming Instability
• Formation of a disc gap induced by a planet: Effect of the deviation from Keplerian disc rotation
• The newborn planet population emerging from ring-like structures in discs
• On the formation of multiple concentric rings and gaps in protoplanetary disks
• The formation of rings and gaps in magnetically coupled disk-wind systems: ambipolar diffusion and reconnection
• Evolution of Migrating Planets Undergoing Gas Accretion
• Radiation Hydrodynamical Turbulence In Protoplanetary Disks: Numerical Models and Observational Constraints
• Zombie Vortex Instability I: A Purely Hydrodynamic Instability to Resurrect the Dead Zones of Protoplanetary Disks
• Multiple Disk Gaps and Rings Generated by a Single Super-Earth: II. Spacings, Depths, and Number of Gaps, with Application to Real Systems
• Planet-planet scattering in planetesimal disks
• An Origin of Multiple Ring Structure and Hidden Planets in HL Tau: A Unified Picture by Secular Gravitational Instability
• Anisotropic Infall and Substructure formation in Embedded Disks
• Evolution of inclined planets in three-dimensional radiative discs
• Early Dynamical Instabilities in the Giant Planet Systems
• The eccentricity distribution of giant planets and their relation to super-Earths in the pebble accretion scenario
• Giants are bullies: how their growth influences systems of inner sub-Neptunes and super-Earths
• Are the observed gaps in protoplanetary discs caused by growing planets?
• Emerging population of gap-opening planets around type-A stars -- Long-term evolution of the forming planets around HD 163296

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• Hidden under a warm blanket: If planets existed in protostellar disks, they would hardly produce observable substructures
• Dust ring and gap formation by gas flow induced by low-mass planets embedded in protoplanetary disks $\mathrm{II}$. Time-dependent model
• Timescales diagnostics for saving viscous and MHD-driven dusty discs from external photoevaporation