The mass-radius relation of intermediate-mass planets outlined by hydrodynamic escape and thermal evolution

Abstract

We employ planetary evolution modeling to reproduce the MR distribution of the 198 so far detected planets with mass and radius measured to the <45% and <15% level, respectively, and less massive than 108Me. We simultaneously account for atmospheric escape, based on the results of hydrodynamic models, and thermal evolution, based on planetary structure evolution models. Since high-energy stellar radiation affects atmospheric evolution, we account for the entire range of possible stellar rotation histories. To set the planetary parameters at formation, we use analytical approximations based on formation models. Finally, we build a grid of synthetic planets with parameters reflecting those of the observed distribution. The predicted radius spread reproduces well the observed MR distribution, except for two distinct groups of outliers (~20% of the population). The first one consists of close-in Saturn-mass planets with Jupiter-like radii for which we underpredict the radius likely because it lacks additional heating similar to that responsible for inflation in hot Jupiters. The second group consists of warm sub-Neptunes, which should host massive primordial H-dominated atmospheres, but instead present high densities indicative of small gaseous envelopes. This suggests that their formation, internal structure, and evolution are different from that of atmospheric evolution through the escape of H-dominated envelopes accreted onto rocky cores. The observed characteristics of low-mass planets (<10-15Me) strongly depend on the impact of atmospheric escape, and thus on the evolution of the host star, while primordial parameters are less relevant. Instead, for more massive planets, the parameters at formation play the dominant role in shaping the final MR distribution.

arXiv comment14 pages + 8 pages Appendix, 8+4 Figures; Accepted for publication in A&A

References in corpus (80)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars
• Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions
• Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 20945
• The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets
• The Revised TESS Input Catalog and Candidate Target List
• Using FU Orionis Outbursts to Constrain Self-Regulated Protostellar Disk Models
• Kepler planets: a tale of evaporation
• The evaporation valley in the Kepler planets
• Atmospheric Circulation and Tides of "51Peg b-like" Planets
• The Mass-Radius Relation for 65 Exoplanets Smaller than 4 Earth Radii
• The California Kepler Survey VII. Precise Planet Radii Leveraging Gaia DR2 Reveal the Stellar Mass Dependence of the Planet Radius Gap
• Core-powered mass loss and the radius distribution of small exoplanets
• False positive probabilties for all Kepler Objects of Interest: 1284 newly validated planets and 428 likely false positives
• Sculpting the Valley in the Radius Distribution of Small Exoplanets as a by-product of Planet Formation: The Core-Powered Mass-Loss Mechanism
• Evolution of "51Peg b-like" Planets
• Gaseous Mean Opacities for Giant Planet and Ultracool Dwarf Atmospheres over a Range of Metallicities and Temperatures
• A Framework for Quantifying the Degeneracies of Exoplanet Interior Compositions
• Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2
• Inflating Hot Jupiters With Ohmic Dissipation
• Initial Conditions of Planet Formation: Lifetimes of Primordial Disks
• Compositional imprints in density-distance-time: a rocky composition for close-in low-mass exoplanets from the location of the valley of evaporation
• Lack of Inflated Radii for Kepler Giant Planet Candidates Receiving Modest Stellar Irradiation
• The active lives of stars: a complete description of rotation and XUV evolution of F, G, K, and M dwarfs
• The Extreme Ultraviolet and X-Ray Sun in Time: High-Energy Evolutionary Tracks of a Solar-Like Star
• Densities and Eccentricities of 139 Kepler Planets from Transit Time Variations
• Evolutionary Analysis of Gaseous Sub-Neptune-Mass Planets with MESA
• The Nature of the Radius Valley: Hints from Formation and Evolution Models
• A generalized bayesian inference method for constraining the interiors of super Earths and sub-Neptunes
• Formation of Jupiter using opacities based on detailed grain physics
• On the Anomalous Radii of the Transiting Extrasolar Planets
• TESS Discovery of a Transiting Super-Earth in the $\pi$ Mensae System
• The radius discrepancy in low mass stars: single vs. binaries
• Kepler 18-b, c, and d: A System Of Three Planets Confirmed by Transit Timing Variations, Lightcurve Validation, Spitzer Photometry and Radial Velocity Measurements
• Challenges in Planet Formation
• Advection of potential temperature in the atmosphere of irradiated exoplanets: a robust mechanism to explain radius inflation
• Ohmic Dissipation in the Atmospheres of Hot Jupiters
• A grid of upper atmosphere models for 1--40 MEARTH planets: application to CoRoT-7 b and HD219134 b,c
• Magnetospheric Truncation, Tidal Inspiral, and the Creation of Short and Ultra-Short Period Planets
• Thermal Tides in Fluid Extrasolar Planets
• The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age
• TESS's first planet: a super-Earth transiting the naked-eye star $\pi$ Mensae
• Planetary evolution with atmospheric photoevaporation I. Analytical derivation and numerical study of the evaporation valley and transition from super-Earths to sub-Neptunes
• Mass and Mass Scalings of Super-Earths
• A remnant planetary core in the hot-Neptune desert
• Hot Jupiters: Origins, Structure, Atmospheres
• The Mechanical Greenhouse: Burial of Heat by Turbulence in Hot Jupiter Atmospheres
• A Definition for Giant Planets Based on the Mass-Density Relationship
• Grain opacity and the bulk composition of extrasolar planets. II. An analytical model for the grain opacity in protoplanetary atmospheres
• WASP-107b's density is even lower: a case study for the physics of planetary gas envelope accretion and orbital migration
• Grain opacity and the bulk composition of extrasolar planets. I. Results from scaling the ISM opacity
• WASP-South transiting exoplanets: WASP-130b, WASP-131b, WASP-132b, WASP-139b, WASP-140b, WASP-141b & WASP-142b
• Planet formation by pebble accretion in ringed disks
• Deflating Super-Puffs: Impact of Photochemical Hazes on the Observed Mass-Radius Relationship of Low Mass Planets
• TESS delivers its first Earth-sized planet and a warm sub-Neptune
• Extended Heat Deposition in Hot Jupiters: Application to Ohmic Heating
• Idealised simulations of the deep atmosphere of hot jupiters: Deep, hot, adiabats as a robust solution to the radius inflation problem
• Identifying the "true" radius of the hot sub-Neptune CoRoT-24b by mass loss modelling
• Ohmic Heating Suspends, not Reverses, the Cooling Contraction of Hot Jupiters
• The Oblique Orbit of WASP-107b from K2 Photometry
• Evolution of the Exoplanet Size Distribution: Forming Large Super-Earths Over Billions of Years
• HARPS-N radial velocities confirm the low densities of the Kepler-9 planets
• Coupling thermal evolution of planets and hydrodynamic atmospheric escape in MESA
• Starspots on WASP-107 and pulsations of WASP-118
• Constraining the entropy of formation from young transiting planets
• Effective induction heating around strongly magnetized stars
• Close-in sub-Neptunes reveal the past rotation history of their host stars: atmospheric evolution of planets in the HD3167 and K2-32 planetary systems
• The Kepler-11 system: evolution of the stellar high-energy emission and {initial planetary} atmospheric mass fractions
• New Perspectives on the Exoplanet Radius Gap from a Mathematica Tool and Visualized Water Equation of State
• How does the mass and activity history of the host star affect the population of low-mass planets?
• The Influence of Age on the Relative Frequency of Super-Earths and Sub-Neptunes
• Beyond the exoplanet mass-radius relation
• Sculpting the sub-Saturn Occurrence Rate via Atmospheric Mass Loss
• The Magellan/PFS Exoplanet Search: A 55-day period dense Neptune transiting the bright ($V=8.6$) star HD 95338
• The Bimodal Distribution in Exoplanet Radii: Considering Varying Core Compositions and ${\mathrm{H}}_2$ Envelope's Sizes
• Detection and characterization of an ultra-dense sub-Neptune planet orbiting the Sun-like star HD 119130
• A hot mini-Neptune in the radius valley orbiting solar analogue HD 110113
• Shallowness of circulation in hot Jupiters -- Advancing the Ohmic dissipation model
• The key impact of the host star's rotational history on the evolution of TOI-849b
• Atmospheric mass loss and stellar wind effects in young and old systems II: Is TOI-942 the past of TOI-421 system?

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