The Outcome of Collisions between Gaseous Clumps formed by Disk Instability

Abstract

The disk instability model is a promising pathway for giant planet formation in various conditions. At the moment, population synthesis models are used to investigate the outcomes of this theory, where a key ingredient of the disk population evolution are collisions of self-gravitating clumps formed by the disk instabilities. In this study, we explore the wide range of dynamics between the colliding clumps by performing state-of-the-art Smoothed Particle Hydrodynamics simulations with a hydrogen-helium mixture equation of state and investigate the parameter space of collisions between clumps of different ages, masses (1--10 Jupiter mass), various impact conditions (head-on to oblique collisions) and a range of relative velocities. We find that the perfect merger assumption used in population synthesis models is rarely satisfied and that the outcomes of most of the collisions lead to erosion, disruption or a hit-and-run. We also show that in some cases collisions can initiate the dynamical collapse of the clump. We conclude that population synthesis models should abandon the simplifying assumption of perfect merging. Relaxing this assumption will significantly affect the inferred population of planets resulting from the disk instability model.

arXiv comment14 pages, 12 figures, accepted by A&A

References in corpus (33)

• The chemical composition of the Sun
• Galaxy Harassment and the Evolution of Clusters of Galaxies
• Formation of giant planets by fragmentation of protoplanetary disks
• Clumps in the Outer Disk by Disk Instability: Why They are Initially Gas Giants and the Legacy of Disruption
• Fragmentation of gravitationally unstable gaseous protoplanetary disks with radiative transfer
• Images of Embedded Jovian Planet Formation At A Wide Separation Around AB Aurigae
• Formation of Terrestrial Planets from Protoplanets under a Realistic Accretion Condition
• A giant exoplanet orbiting a very low-mass star challenges planet formation models
• Giant Planet Formation, Evolution, and Internal Structure
• The Effect of Composition on the Evolution of Giant and Intermediate-Mass Planets
• Core Formation in Giant Gaseous Protoplanets
• Towards a population synthesis model of self-gravitating disc fragmentation and tidal downsizing II: The effect of fragment-fragment interactions
• The Challenge of Forming a Fuzzy Core in Jupiter
• Forming Mercury by Giant Impacts
• The Jeans Mass as a Fundamental Measure of Self-Gravitating Disc Fragmentation and Initial Fragment Mass
• Consequences of Giant Impacts on Early Uranus for Rotation, Internal Structure, Debris, and Atmospheric Erosion
• Metallicity of the Massive Protoplanets Around HR 8799 If Formed by Gravitational Instability
• Bifurcation in the history of Uranus and Neptune: the role of giant impacts
• On the Evolution and Survival of Protoplanets Embedded in a Protoplanetary Disk
• Identifying and Analysing Protostellar Disc Fragments in Smoothed Particle Hydrodynamics Simulations
• Numerical aspects of Giant Impact simulations
• The fragmentation of protostellar discs: the Hill criterion for spiral arms
• The Dynamical Fate of Self-Gravitating Disc Fragments After Tidal Downsizing
• Formation of intermediate-mass planets via magnetically-controlled disk fragmentation
• Atmospheric Erosion by Giant Impacts onto Terrestrial Planets: A Scaling Law for any Speed, Angle, Mass, and Density
• Constraining surface properties of asteroid (162173) Ryugu from numerical simulations of Hayabusa2 mission impact experiment
• Heavy Element Enrichment of a Jupiter-mass Protoplanet as a Function of Orbital Location
• Constraining the initial planetary population in the gravitational instability model
• The EOS/Resolution Conspiracy: Convergence in Proto-Planetary Collision Simulations
• A dynamical mass for GJ 463 b: A massive super-Jupiter companion beyond the snow line of a nearby M dwarf
• Could Uranus and Neptune form by collisions of planetary embryos?
• Characterizing fragmentation and sub-Jovian clump properties in magnetized young protoplanetary disks
• The link between infall location, early disc size, and the fraction of self-gravitationally fragmenting discs

Cited by in corpus (3)

• DIPSY: A new Disc Instability Population SYnthesis, II. The Populations of Companions Formed Through Disc Instability
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