Study of Jupiter's Interior with Quadratic Monte Carlo Simulations

Abstract

We construct models for Jupiter's interior that match the gravity data obtained by the Juno and Galileo spacecrafts. To generate ensembles of models, we introduce a novel quadratic Monte Carlo technique that is more efficient in confining fitness landscapes than affine invariant method that relies on linear stretch moves. We compare how long it takes the ensembles of walkers in both methods to travel to the most relevant parameter region. Once there, we compare the autocorrelation time and error bars of the two methods. For a ring potential and the 2d Rosenbrock function, we find that our quadratic Monte Carlo technique is significantly more efficient. Furthermore we modified the walk moves by adding a scaling factor. We provide the source code and examples so that this method can be applied elsewhere. Here we employ our method to generate five-layer models for Jupiter's interior that include winds and a prominent dilute core, which allows us to match the planet's even and odd gravity harmonics. We compare predictions from the different model ensembles and analyze how much an increase of the temperature at 1 bar and ad hoc change to the equation of state affects the inferred amount of heavy elements in atmosphere and in the planet overall.

arXiv comment27 pages, 9 figures, 2 tables

References in corpus (44)

• Binary companions of evolved stars in APOGEE DR14: Search method and catalog of ~5,000 companions
• The mass distribution and gravitational potential of the Milky Way
• The Mass Dependence Between Protoplanetary Disks and their Stellar Hosts
• The trouble with $H_0$
• How to Constrain Your M Dwarf: measuring effective temperature, bolometric luminosity, mass, and radius
• The Gemini Planet Imager: First Light
• Tidal Deformabilities and Radii of Neutron Stars from the Observation of GW170817
• A Technique for Extracting Highly Precise Photometry for the Two-Wheeled Kepler Mission
• Beasts of the Southern Wild: Discovery of nine Ultra Faint satellites in the vicinity of the Magellanic Clouds
• Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core
• A Massive Core in Jupiter Predicted From First-Principles Simulations
• FPEOS: A First-Principles Equation of State Table of Deuterium for Inertial Confinement Fusion Applications
• Hydrogen-Helium Mixtures in the Interiors of Giant Planets
• Jupiter models with improved ab initio hydrogen EOS (H-REOS.2)
• Nuclear Quantum Effects and Nonlocal Exchange-Correlation Functionals Applied to Liquid Hydrogen at High Pressure
• Ab Initio Equation of State for Hydrogen-Helium Mixtures with Recalibration of the Giant-Planet Mass-Radius Relation
• The water abundance in Jupiter's equatorial zone
• Rocky core solubility in Jupiter and giant exoplanets
• Sequestration of noble gases in giant planet interiors
• Phase separation in hydrogen-helium mixtures at Mbar pressures
• Concentric Maclaurin spheroid models of rotating liquid planets
• First-Principles Equation of State Database for Warm Dense Matter Computation
• A Preliminary Jupiter Model
• Path Integral Monte Carlo and Density Functional Molecular Dynamics Simulations of Hot, Dense Helium
• The Formation of Jupiter's Diluted Core by a Giant Impact
• Phase diagram of hydrogen and a hydrogen-helium mixture at planetary conditions by Quantum Monte Carlo simulations
• Jupiter internal structure: the effect of different equations of state
• Analysis of laser shock experiments on precompressed samples using a quartz reference and application to warm dense hydrogen and helium
• Jupiter's inhomogeneous envelope
• The Challenge of Forming a Fuzzy Core in Jupiter
• Revelations on Jupiter's Formation, Evolution and Interior: Challenges from Juno Results
• Understanding Jupiter's Interior
• Solubility of Iron in Metallic Hydrogen and Stability of Dense Cores in Giant Planets
• Models of Saturn's Interior Constructed with Accelerated Concentric Maclaurin Spheroid Method
• Measuring Jupiter's water abundance by Juno: the link between interior and formation models
• Double-diffusive erosion of the core of Jupiter
• Combined magnetic and gravity measurements probe the deep zonal flows of the gas giants
• Benchmarking Hydrogen-Helium Mixtures with QMC: Energetics, Pressures, and Forces
• Gravity and Zonal Flows of Giant Planets: From the Euler Equation to the Thermal Wind Equation
• A subsolar oxygen abundance or a radiative region deep in Jupiter revealed by thermochemical modelling
• Comparison of Jupiter Interior Models Derived from First-Principles Simulations
• Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
• Linking Zonal Winds and Gravity II: explaining the equatorially antisymmetric gravity moments of Jupiter
• Tidal Response and Shape of Hot Jupiters

Cited by in corpus (4)

• First principles simulations of dense hydrogen
• Study of Jupiter's Interior: Comparison of 2, 3, 4, 5, and 6 Layer Models
• Ab Initio Entropy Calculations of Water Predict the Interiors of Uranus and Neptune to be 15-30% Colder than Previous Models
• NeuralCMS: A deep learning approach to study Jupiter's interior