Massive discs around low-mass stars

Abstract

We use a suite of SPH simulations to investigate the susceptibility of protoplanetary discs to the effects of self-gravity as a function of star-disc properties. We also include passive irradiation from the host star using different models for the stellar luminosities. The critical disc-to-star mass ratio for axisymmetry (for which we produce criteria) increases significantly for low-mass stars. This could have important consequences for increasing the potential mass reservoir in a proto Trappist-1 system, since even the efficient Ormel et al. (2017) formation model will be influenced by processes like external photoevaporation, which can rapidly and dramatically deplete the dust reservoir. The aforementioned scaling of the critical $M_d/M_{\ast }$ for axisymmetry occurs in part because the Toomre $Q$ parameter has a linear dependence on surface density (which promotes instability) and only an $M_{\ast }^{1/2}$ dependence on shear (which reduces instability), but also occurs because, for a given $M_d/M_{\ast }$, the thermal evolution depends on the host star mass. The early phase stellar irradiation of the disc (for which the luminosity is much higher than at the zero age main sequence, particularly at low stellar masses) can also play a key role in significantly reducing the role of self-gravity, meaning that even Solar mass stars could support axisymmetric discs a factor two higher in mass than usually considered possible. We apply our criteria to the DSHARP discs with spirals, finding that self-gravity can explain the observed spirals so long as the discs are optically thick to the host star irradiation.

arXiv comment21 pages, Accepted for publication MNRAS

References in corpus (79)

• 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
• MESA Isochrones and Stellar Tracks (MIST). I: Solar-Scaled Models
• MESA Isochrones and Stellar Tracks (MIST) 0: Methods for the construction of stellar isochrones
• Disk Frequencies and Lifetimes in Young Clusters
• Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1
• The Disk Substructures at High Angular Resolution Project (DSHARP): I. Motivation, Sample, Calibration, and Overview
• Nonlinear Outcome of Gravitational Instability in Cooling, Gaseous Disks
• Modelling Accretion in Protobinary Systems
• A simple model for the evolution of the dust population in protoplanetary disks
• SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations
• Protoplanetary Disk Structures in Ophiuchus
• Evolutionary models for low-mass stars and brown dwarfs: uncertainties and limits at very young ages
• Gravitational Instabilities in Circumstellar Disks
• A seven-planet resonant chain in TRAPPIST-1
• The locality of transport in self-gravitating accretion discs
• Investigating fragmentation conditions in self-gravitating accretion discs
• Spiral Density Waves in a Young Protoplanetary Disk
• The nature of the TRAPPIST-1 exoplanets
• On the diversity and statistical properties of protostellar discs
• On the Role of Disks in the Formation of Stellar Systems: A Numerical Parameter Study of Rapid Accretion
• Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations
• The effect of cooling on the global stability of self-gravitating protoplanetary discs
• A Parametric Modeling Approach to Measuring the Gas Masses of Circumstellar Disks
• A Triple Protostar System Formed via Fragmentation of a Gravitationally Unstable Disk
• Dust grain growth in rho-Ophiuchi protoplanetary disks
• Testing the locality of transport in self-gravitating accretion discs - II. The massive disc case
• Pseudo-viscous modeling of self-gravitating discs and the formation of low mass ratio binaries
• Accelerated planetesimal growth in self-gravitating protoplanetary discs
• The Coupled Physical Structure of Gas and Dust in the IM Lup Protoplanetary Disk
• Formation of planets by tidal downsizing of giant planet embryos
• The Disk Substructures at High Angular Resolution Project (DSHARP): III. Spiral Structures in the Millimeter Continuum of the Elias 27, IM Lup, and WaOph 6 Disks
• Formation of TRAPPIST-1 and other compact systems
• Radiative transfer and the energy equation in SPH simulations of star formation
• The Thermal Regulation of Gravitational Instabilities in Protoplanetary Disks II. Extended Simulations with Varied Cooling Rates
• On the convergence of the critical cooling timescale for the fragmentation of self-gravitating discs
• Formation of Giant Planets by Disk Instability on Wide Orbits Around Protostars with Varied Masses
• Non-convergence of the critical cooling timescale for fragmentation of self-gravitating discs
• Towards a Population Synthesis Model of Objects formed by Self-Gravitating Disc Fragmentation and Tidal Downsizing
• 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
• Time-dependent models of the structure and evolution of self-gravitating protoplanetary discs
• Grand Design Spiral Arms in A Young Forming Circumstellar Disk
• G11.92-0.61 MM 1: A fragmented Keplerian disk surrounding a proto-O star
• Towards a population synthesis model of self-gravitating disc fragmentation and tidal downsizing II: The effect of fragment-fragment interactions
• Smoothed particle hydrodynamics with radiative transfer in the flux-limited diffusion approximation
• On the origin of the spiral morphology in the Elias 2-27 circumstellar disc
• Introducing a Hybrid Method of Radiative Transfer for Smoothed Particle Hydrodynamics
• Stability of self-gravitating discs under irradiation
• Exploring the conditions required to form giant planets via gravitational instability in massive protoplanetary discs
• The effects of opacity on gravitational stability in protoplanetary discs
• Pebble-driven planet formation for TRAPPIST-1 and other compact systems
• The Jeans Mass as a Fundamental Measure of Self-Gravitating Disc Fragmentation and Initial Fragment Mass
• The role of disc self-gravity in the formation of protostars and protostellar discs
• The Nature of Angular Momentum Transport in Radiative Self-Gravitating Protostellar Discs
• Pebbles versus Planetesimals: The case of Trappist-1
• Fragment Production and Survival in Irradiated Disks: A Comprehensive Cooling Criterion
• The Thermal Regulation of Gravitational Instabilities in Protoplanetary Disks. IV. Simulations with Envelope Irradiation
• Interior characterization in multiplanetary systems: TRAPPIST-1
• Identifying and Analysing Protostellar Disc Fragments in Smoothed Particle Hydrodynamics Simulations
• Where can a Trappist-1 planetary system be produced?
• Toroidal vortices and the conglomeration of dust into rings in protoplanetary discs
• The fragmentation of protostellar discs: the Hill criterion for spiral arms
• Viscosity prescription for gravitationally unstable accretion disks
• Is the spiral morphology of the Elias 2-27 circumstellar disc due to gravitational instability?
• Disc formation and fragmentation using radiative non-ideal magnetohydrodynamics
• Are Elias 2-27's spiral arms driven by self-gravity, or by a companion? A comparative spiral morphology study
• Directly observing continuum emission from self-gravitating spiral waves
• The temporal requirements of directly observing self-gravitating spiral waves in protoplanetary discs with ALMA
• The Maximum Mass Solar Nebula and the early formation of planets
• The Properties of Prestellar Discs in Isolated and Multiple Prestellar Systems
• Observing substructure in circumstellar discs around massive young stellar objects
• Shaken and stirred: the effects of turbulence and rotation on disc and outflow formation during the collapse of magnetised molecular cloud cores
• Fragmentation favoured in discs around higher mass stars
• An Efficient Radiative Cooling Approximation for Use in Hydrodynamic Simulations
• Fragmentation of protoplanetary disks around M-dwarfs
• Efficient radiative transfer techniques in hydrodynamic simulations
• Pebble accretion in self-gravitating protostellar discs

Cited by in corpus (24)

• Solution to the debris disc mass problem: planetesimals are born small?
• Predicting the kinematic evidence of gravitational instability
• Proplyds in the Flame Nebula NGC 2024
• Radiation shielding of protoplanetary discs in young star-forming regions
• Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation
• Resolved near-UV hydrogen emission lines at 40-Myr super-Jovian protoplanet Delorme 1 (AB)b: Indications of magnetospheric accretion
• Peter Pan Discs: finding Neverland's parameters
• Binary companions triggering fragmentation in self-gravitating discs
• Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A close low mass companion to ET Cha
• Exploring the possibility of Peter Pan discs across stellar mass
• TW Hya: an old protoplanetary disc revived by its planet
• Has the dust clump in the debris disk of Beta Pictoris moved?
• The observational impact of dust trapping in self-gravitating discs
• AB Aurigae: Possible evidence of planet formation through the gravitational instability
• A giant planet shaping the disk around the very low-mass star CIDA 1
• Filling in the Gaps: Can Gravitationally Unstable Discs Form the Seeds of Gas Giant Planets?
• An imaged 15Mjup companion within a hierarchical quadruple system
• Planet formation and disk mass dependence in a pebble-driven scenario for low mass stars
• Searching for wide-orbit gravitational instability protoplanets with ALMA in the dust continuum
• Using simultaneous mass accretion and external photoevaporation rates for d203-504 to constrain disc evolution processes
• Formation of super-Earths in icy dead zones around low-mass stars
• Line ratio identification of external photoevaporation
• Constraining protoplanetary disc mass using the GI wiggle
• Gravitational instability in planet-forming discs