The influence of infall on the properties of protoplanetary discs

Abstract

We perform a population synthesis of protoplanetary discs including infall with a total of $50000$ simulations using a 1D vertically integrated viscous evolution code, studying a large parameter space in final stellar mass. Initial conditions and infall locations are chosen based on the results from a radiation-hydrodynamic population synthesis of circumstellar discs. We also consider a different infall prescription based on a magnetohydrodynamic (MHD) collapse simulation in order to assess the influence of magnetic fields on disc formation. The duration of the infall phase is chosen to produce a stellar mass distribution in agreement with the observationally determined stellar initial mass function. We find that protoplanetary discs are very massive early in their lives. When averaged over the entire stellar population, the discs have masses of $\sim 0.3$ and $0.1{\mathrm{M}}_{\odot }$ for systems based on hydrodynamic or MHD initial conditions, respectively. In systems with final stellar mass $\sim 1{\mathrm{M}}_{\odot }$, we find disc masses of $\sim 0.7{\mathrm{M}}_{\odot }$ for the `hydro' case and $\sim 0.2{\mathrm{M}}_{\odot }$ for the `MHD' case at the end of the infall phase. Furthermore, the inferred total disc lifetimes are long, $\approx 5-7\mathrm{Myr}$ on average, despite our choice of a high value of $10^{-2}$ for the background viscosity $\alpha$-parameter. In addition, fragmentation is common in systems that are simulated using hydrodynamic cloud collapse, with more fragments of larger mass formed in more massive systems. In contrast, if disc formation is limited by magnetic fields, fragmentation is suppressed entirely.

26 pages, 14 figures. Accepted to A&A

References in corpus (22)

• Direct Imaging of Multiple Planets Orbiting the Star HR 8799
• Gas- and dust evolution in protoplanetary disks
• On the diversity and statistical properties of protostellar discs
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. A Statistical Characterization of Class 0 and I Protostellar Disks
• Global simulations of protoplanetary disks with ohmic resistivity and ambipolar diffusion
• The Two Modes of Gas Giant Planet Formation
• Imaging the water-snow line during a protostellar outburst
• Global Models for the Evolution of Embedded, Accreting Protostellar Disks
• Numerical requirements for simulations of self gravitating and non-self gravitating disks
• A giant exoplanet orbiting a very low-mass star challenges planet formation models
• Magnetically self-regulated formation of early protoplanetary discs
• Age Gradients in the Stellar Populations of Massive Star Forming Regions Based on a New Stellar Chronometer
• On the gap-opening criterion of migrating planets in protoplanetary disks
• Convergence of the critical cooling rate for protoplanetary disk fragmentation achieved; the key role of numerical dissipation of angular momentum
• Modeling disk fragmentation and multiplicity in massive star formation
• Circumplanetary disks around young giant planets: a comparison between core-accretion and disk instability
• The Planetary Accretion Shock: I. Framework for Radiation-hydrodynamical Simulations and First Results
• Mean gas opacity for circumstellar environments and equilibrium temperature degeneracy
• Identifying and Analysing Protostellar Disc Fragments in Smoothed Particle Hydrodynamics Simulations
• The fragmentation criteria in local vertically stratified self-gravitating disk simulations
• In situ accretion of gaseous envelopes on to planetary cores embedded in evolving protoplanetary discs
• The Role of Disc Self-Gravity in Circumbinary Planet Systems: I. Disc Structure and Evolution

Cited by in corpus (22)

• RV-detected planets around M dwarfs: Challenges for core accretion models
• In-situ extreme mass ratio inspirals via sub-parsec formation and migration of stars in thin, gravitationally unstable AGN discs
• Understanding planet formation using microgravity experiments
• A framework for the architecture of exoplanetary systems. I. Four classes of planetary system architecture
• Population study on MHD wind-driven disc evolution -- Confronting theory and observation
• Kepler-167e as a Probe of the Formation Histories of Cold Giants with Inner Super-Earths
• A framework for the architecture of exoplanetary systems. II. Nature versus nurture: Emergent formation pathways of architecture classes
• New binaries from the SHINE survey
• Atmospheric characterization of the super-Jupiter HIP 99770 b with KPIC
• Presolar grain dynamics: creating nucleosynthetic variations through a combination of drag and viscous evolution
• Magnetic disk winds in protoplanetary disks: Description of the model and impact on global disk evolution
• The imprint of X-ray photoevaporation of planet-forming discs on the orbital distribution of giant planets -- II. Theoretical predictions
• The link between infall location, early disc size, and the fraction of self-gravitationally fragmenting discs
• The influence of metallicity on a combined stellar and disk evolution
• Populating The Milky Way: Characterising Planet Demographics by Combining Galaxy Formation Simulations and Planet Population Synthesis Models
• DIPSY: A new Disc Instability Population SYnthesis, II. The Populations of Companions Formed Through Disc Instability
• Giant planets population around B stars from the first part of the BEAST survey
• Calibrated Gas Accretion and Orbital Migration of Protoplanets in 1D Disc Models
• DIPSY: A new Disc Instability Population SYnthesis, I. Modeling, evolution of individual systems, and tests
• Interpreting the atmospheric composition of exoplanets: sensitivity to planet formation assumptions
• Origin of compact exoplanetary systems during disk infall
• On the Efficacy of Ocean Formation with a Primordial Hydrogen Atmosphere