Imprint of planet formation in the deep interior of the Sun

Abstract

Stars grow by accreting gas that has an evolving composition owing to the growth and inward drift of dust (pebble wave), the formation of planetesimals and planets, and the selective removal of hydrogen and helium by disk winds. We investigated how the formation of the Solar System may have affected the composition and structure of the Sun, and whether it plays any role in solving the solar abundance problem. We simulated the evolution of the Sun from the protostellar phase to the present age and attempted to reproduce spectroscopic and helioseismic constraints. We performed chi-squared tests to optimize our input parameters. We confirmed that, for realistic models, planet formation occurs when the solar convective zone is still massive; thus, the overall changes due to planet formation are too small to significantly improve the chi-square fits. We found that solar models with up-to-date abundances require an opacity increase of 12% to 18% centered at $T=10^{6.4}$ K to reproduce the available observational constraints. This is slightly higher than, but is qualitatively in good agreement with, recent measurements of higher iron opacities. These models result in better fits to the observations than those using old abundances; therefore, they are a promising solution to the solar abundance problem. Using these improved models, we found that planet formation processes leave a small imprint in the solar core, whose metallicity is enhanced by up to 5%. This result can be tested by accurately measuring the solar neutrino flux. In the improved models, the protosolar molecular cloud core is characterized by a primordial metallicity in the range 0.0127-0.0157 and a helium mass fraction in the range 0.268-0.274. (abridged)

arXiv commentAccepted for publication in A&A. 24 pages, 17 figures

References in corpus (82)

• SciPy 1.0--Fundamental Algorithms for Scientific Computing in Python
• The NumPy array: a structure for efficient numerical computation
• The chemical composition of the Sun
• 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): Binaries, Pulsations, and Explosions
• Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions
• Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation
• Disk Frequencies and Lifetimes in Young Clusters
• Low Temperature Opacities
• Protoplanetary Disks and Their Evolution
• Solar Chemical Abundances Determined with a CO5BOLD 3D Model Atmosphere
• The chemical make-up of the Sun: A 2020 vision
• Dust coagulation in protoplanetary disks: a rapid depletion of small grains
• Element Diffusion in the Solar Interior
• New Mass Loss Measurements from Astrospheric Lyman-alpha Absorption
• The peculiar solar composition and its possible relation to planet formation
• Timescale of Mass Accretion in Pre-Main-Sequence Stars
• A new Generation of Standard Solar Models
• New Solar Composition: The Problem With Solar Models Revisited
• Evolution of protoplanetary disks: Constraints from DM Tauri and GM Aurigae
• Helioseismological Implications of Recent Solar Abundance Determinations
• Constraining solar abundances using helioseismology
• Disk Winds Driven by Magnetorotational Instability and Dispersal of Proto-Planetary Disks
• Episodic accretion at early stages of evolution of low mass stars and brown dwarfs: a solution for the observed luminosity spread in HR diagrams?
• Solar models with accretion. I. Application to the solar abundance problem
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Protostellar Core Formation
• Experimental evidence of neutrinos produced in the CNO fusion cycle in the Sun
• Why do protoplanetary disks appear not massive enough to form the known exoplanet population?
• Dust masses of young disks: constraining the initial solid reservoir for planet formation
• Formation Process of the Circumstellar Disk: Long-term Simulations in the Main Accretion Phase of Star Formation
• Fresh insights on the structure of the solar core
• The Impact of Dust Evolution and Photoevaporation on Disk Dispersal
• Observed luminosity spread in young clusters and Fu Ori stars: a unified picture
• Jupiter's composition: sign of a (relatively) late formation in a chemically evolved protosolar disk
• On the Reliability of Stellar Ages and Age Spreads Inferred from Pre-Main Sequence Evolutionary Models
• Global Seismology of the Sun
• Measuring the extent of convective cores in low-mass stars using Kepler data: towards a calibration of core overshooting
• Fingerprints of giant planets in the photospheres of Herbig stars
• On the opacity change required to compensate for the revised solar composition
• Stellar Mass Dependent Disk Dispersal
• Can Enhanced Diffusion Improve Helioseismic Agreement for Solar Models with Revised Abundances?
• Episodic accretion: the interplay of infall and disc instabilities
• The chemical composition of the Sun from helioseismic and solar neutrino data
• Exploring mass loss, low-Z accretion, and convective overshoot in solar models to mitigate the solar abundance problem
• The photospheric solar oxygen project: IV. 3D-NLTE investigation of the 777 nm triplet lines
• Viscous Evolution and Photoevaporation of Circumstellar Disks due to External FUV Radiation Fields
• Determining the initial helium abundance of the Sun
• Growth and migration of solids in evolving protostellar disks I: Methods and Analytical tests
• Saturation of Stellar Winds from Young Suns
• Giant Planets
• Evidence for a Dichotomy in the Interior Structures of Jupiter and Saturn from Helium Phase Separation
• Low abundances of heavy elements in the solar outer layers: comparisons of solar models with helioseismic inversions
• Dispersal of protoplanetary disks by the combination of magnetically driven and photoevaporative winds
• Alive and well: a short review about standard solar models
• Revisiting the pre-main-sequence evolution of stars I. Importance of accretion efficiency and deuterium abundance
• Fingerprints of giant planets in the composition of solar twins
• Element abundance ratios in the quiet Sun transition region
• Apparent disk-mass reduction and planetesimal formation in gravitationally unstable disks in Class 0/I YSOs
• Solar models with convective overshoot, the solar-wind mass loss, and a PMS disk accretion: helioseismic quantities, Li depletion and neutrino fluxes
• Prospects for asteroseismology
• Jupiter's formation in the vicinity of the amorphous ice snowline
• On the filtering and processing of dust by planetesimals 1. Derivation of collision probabilities for non-drifting planetesimals
• Constraints on the opacity profile of the sun from helioseismic observables and solar neutrino flux measurements
• A grid of 1D low-mass star formation collapse models
• Dust Dynamics in Protoplanetary Disk Winds Driven by Magneto-Rotational Turbulence: A Mechanism for Floating Dust Grains with Characteristic Sizes
• Revisiting the pre-main-sequence evolution of stars II. Consequences of planet formation on stellar surface composition
• Convective overshooting and penetration in a Boussinesq spherical shell
• Combining multiple structural inversions to constrain the Solar modelling problem
• Solar Elemental Abundances
• Calibrating Core Overshooting Parameters With Two-dimensional Hydrodynamical Simulations
• Dust clearing by radial drift in evolving protoplanetary discs
• Gravitoviscous protoplanetary disks with a dust component. III. Evolution of gas, dust, and pebbles
• On the hydrostatic stratification of the solar tachocline
• First solar models with OPAS opacity tables
• On Stellar Evolution In A Neutrino Hertzsprung-Russell Diagram
• Pebble accretion in class 0/I YSOs as a possible pathway for early planet formation
• Accreting pre-main sequence models and abundance anomalies in globular clusters
• Rotating Solar Models with Low Metal Abundances as Good as Those with High Metal Abundances
• Standard solar models: a perspective from updated solar neutrino fluxes and the gravity-mode period spacing
• The solar abundance problem and eMSTOs in clusters
• History of the Solar Nebula from Meteorite Paleomagnetism

Cited by in corpus (14)

• Higher metal abundances do not solve the solar problem
• Evidence of a signature of planet formation processes from solar neutrino fluxes
• An Expanded Set of Los Alamos OPLIB Tables in MESA: Type-1 Rosseland-mean Opacities and Solar Models
• Constraints on the properties of macroscopic transport in the Sun from combined lithium and beryllium depletion
• Helioseismic inference of the solar radiative opacity
• The Pre-main Sequence: Challenges and Prospects for Asteroseismology
• Local heating due to convective overshooting and the solar modelling problem
• Using Molecular Lines to Determine Carbon and Nitrogen Abundances in the Atmospheres of Cool Stars
• Solar Models and Astrophysical S-factors Constrained by Helioseismic Results and Updated Neutrino Fluxes
• Solar models with protosolar accretion and turbulent mixing
• The impact of the transport of chemicals and electronic screening on helioseismic and neutrino observations in solar models
• Using Lithium and Beryllium to Study Structure and Evolution of Rotating Stars
• Investigating the impact of Solar Fusion III reaction rates on helioseismic constraints and solar neutrino fluxes
• A data-driven estimate of the protosolar helium mass fraction