Mixing is easy: New insights for cosmochemical evolution from pre-stellar core collapse

Abstract

Signposts of early planet formation are ubiquitous in substructured young discs. Dense, hot and high-pressure regions formed during gravitational collapse process, integral to star formation, facilitate dynamical mixing of dust within the protostellar disc. This provides an incentive to constrain the role of gas-dust interaction and resolve zones of dust concentration during star-disc formation. We explore if thermal and dynamical conditions developed during disc formation can generate gas flows that efficiently mix and transport well-coupled gas and dust components. We simulated the collapse of dusty molecular cloud cores with the hydrodynamics code PLUTO augmented with radiation transport and self-gravity. We used a 2D axisymmetric geometry and follow the azimuthal component of velocity. Dust was treated as Lagrangian particles that are subject to drag from the gas, whose motion is computed on a Eulerian grid. We considered 1, 10 and 100 micron-sized neutral spherical dust. Importantly, the equation of state accurately includes molecular hydrogen dissociation. We focus on molecular cloud core masses of 1 and 3 Msun and explore effects of initial rotation rates and cloud core sizes. Our study underlines mechanisms for early transport of dust from inner hot disc regions via the occurrence of meridional flows and outflow. The vortical flow fosters dynamical mixing and retention of dust while thermal pressure driven outflow replenishes dust in the outer disc. Young dynamical precursors to planet-forming discs exhibit regions with complex hydrodynamical gas features and high-temperature structures. These can play a crucial role in concentrating dust for subsequent growth into protoplanets. Dust transport, especially, from sub-au scales surrounding the protostar to outer relatively cooler parts, offers an efficient pathway for thermal reprocessing during pre-stellar core collapse. [Abridged]

Language edited version

References in corpus (133)

• SciPy 1.0--Fundamental Algorithms for Scientific Computing in Python
• Array Programming with NumPy
• Dust Grain Size Distributions and Extinction in the Milky Way, LMC, and SMC
• PLUTO: a Numerical Code for Computational Astrophysics
• First Results from High Angular Resolution ALMA Observations Toward the HL Tau Region
• The Disk Substructures at High Angular Resolution Project (DSHARP): I. Motivation, Sample, Calibration, and Overview
• A simple model for the evolution of the dust population in protoplanetary disks
• Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• The PLUTO Code for Adaptive Mesh Computations in Astrophysical Fluid Dynamics
• Two accreting protoplanets around the young star PDS 70
• Turbulence in Accretion Disks. Vorticity Generation and Angular Momentum Transport via the Global Baroclinic Instability
• An Ice Age JWST inventory of dense molecular cloud ices
• Spiral Density Waves in a Young Protoplanetary Disk
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. A Statistical Characterization of Class 0 and I Protostellar Disks
• Protostellar disk formation and transport of angular momentum during magnetized core collapse
• Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution
• The Effect of Jupiter's Formation on the Distribution of Refractory Elements and Inclusions in Meteorites
• Circumventing the radiation pressure barrier in the formation of massive stars via disk accretion
• Orbital and atmospheric characterization of the planet within the gap of the PDS 70 transition disk
• Millimeter-wave polarization of protoplanetary disks due to dust scattering
• The Shape of the Inner Rim in Proto-Planetary Disks
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Protostellar Core Formation
• Collapse of a Molecular Cloud Core to Stellar Densities: The First Three-Dimensional Calculations
• Three-dimensional simulation of massive star formation in the disk accretion scenario
• The Ubiquity of Micrometer-Sized Dust Grains in the Dense Interstellar Medium
• The thermodynamics of collapsing molecular cloud cores using smoothed particle hydrodynamics with radiative transfer
• Four annular structures in a protostellar disk less than 500,000 years old
• The subcritical baroclinic instability in local accretion disc models
• Formation Process of the Circumstellar Disk: Long-term Simulations in the Main Accretion Phase of Star Formation
• A protostellar system fed by a streamer of 10,500 au length
• Radiative transfer and the energy equation in SPH simulations of star formation
• Early Planet Formation in Embedded Disks (eDisk). I. Overview of the Program and First Results
• Protostellar collapse: radiative and magnetic feedbacks on small scale fragmentation
• Radiation hydrodynamics with Adaptive Mesh Refinement and application to prestellar core collapse. I Methods
• Protostellar Disk Formation Enabled by Removal of Small Dust Grains
• Collapse of a molecular cloud core to stellar densities: stellar core and outflow formation in radiation magnetohydrodynamics simulations
• Fragmentation of a Molecular Cloud Core versus Fragmentation of the Massive Protoplanetary Disk in the Main Accretion Phase
• Conditions for Circumstellar Disk Formation: Effects of Initial Conditions and Sink Treatment
• Dust Density Distribution and Imaging Analysis of Different Ice Lines in Protoplanetary Disks
• Grain growth in the envelopes and disks of Class I protostars
• The structure and stability of molecular cloud cores in external radiation fields
• The Origin and Formation of the Circumstellar Disk
• Direct evidence of dust growth in L183 from MIR light scattering
• Grain Growth and Density Distribution of the Youngest Protostellar Systems
• Baroclinic Vorticity Production in Protoplanetary Disks; Part I: Vortex Formation
• Planetesimal rings as the cause of the Solar System's planetary architecture
• First hydrodynamics simulations of radiation forces and photoionization feedback in massive star formation
• Multiple Gaps in the Disk of the Class I Protostar GY 91
• Fast and accurate frequency-dependent radiation transport for hydrodynamics simulations in massive star formation
• The VLA view of the HL Tau Disk - Disk Mass, Grain Evolution, and Early Planet Formation
• Protostellar birth with ambipolar and ohmic diffusion
• Radiation Magnetohydrodynamics Simulation of Proto-Stellar Collapse: Two-Component Molecular Outflow
• A Disk-Wind Model for the Near-Infrared Excess Emission in Protostars
• Collapse of a molecular cloud core to stellar densities: the formation and evolution of pre-stellar discs
• Relating jet structure to photometric variability: the Herbig Ae star HD 163296
• Three-Dimensional Radiation-Hydrodynamics Calculations of the Envelopes of Young Planets Embedded in Protoplanetary Disks
• A chemical solver to compute molecule and grain abundances and non-ideal MHD resistivities in prestellar core collapse calculations
• Low dust emissivities and radial variations in the envelopes of Class 0 protostars: a signature of early grain growth?
• The Fundamentally Different Dynamics of Dust and Gas in Molecular Clouds
• The early evolution of viscous and self-gravitating circumstellar disks with a dust component
• The Global Baroclinic Instability in Accretion Disks. II: Local Linear Analysis
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. III. Substructures in Protostellar Disks
• A Particle Module for the PLUTO Code: I - an implementation of the MHD-PIC equations
• Protostellar Outflows and Radiative Feedback from Massive Stars. II. Feedback, Star Formation Efficiency, and Outflow Broadening
• On the simultaneous evolution of massive protostars and their host cores
• Spiral Arms and a Massive Dust Disk with non-Keplerian Kinematics: Possible Evidence for Gravitational Instability in the Disk of Elias 2-27
• Evolution of Gas Giant Entropy During Formation by Runaway Accretion
• The ALMA early science view of FUor/EXor objects - V: continuum disc masses and sizes
• Formation and Evolution of Disks around Young Stellar Objects
• Protostellar Outflows and Radiative Feedback from Massive Stars
• Confirmation and Keplerian motion of the gap-carving protoplanet HD 169142 b
• Is the dust-to-gas ratio constant in molecular clouds?
• Gas and multi-species dust dynamics in viscous protoplanetary discs: the importance of the dust back-reaction
• The collapse of a molecular cloud core to stellar densities using radiation non-ideal magnetohydrodynamics
• ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT) II: Vertical stratification of CO, CS, CN, H${}_2$CO, and CH${}_3$OH in a Class I disk
• Collapse of a molecular cloud core to stellar densities: the radiative impact of stellar core formation on the circumstellar disc
• Probing the Protosolar Disk Using Dust Filtering at Gaps in the Early Solar System
• Effect of Grain Size on Differential Desorption of Volatile Species and on Non-ideal MHD Diffusivity
• Blobs, spiral arms, and a possible planet around HD 169142
• Mean gas opacity for circumstellar environments and equilibrium temperature degeneracy
• "Ash-fall" induced by molecular outflow in protostar evolution
• Protostellar collapse: the conditions to form dust rich protoplanetary disks
• Origin of isotopic diversity among carbonaceous chondrites
• Dust coagulation feedback on magnetohydrodynamic resistivities in protostellar collapse
• Indirect evidence of significant grain growth in young protostellar envelopes from polarized dust emission
• Global 3D radiation-hydrodynamic simulations of gas accretion: The opacity dependent growth of Saturn-mass planets
• Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region
• On the dynamics of dust during protostellar collapse
• Grain size limits derived from 3.6 μm and 4.5 μm coreshine
• Small dust grain dynamics on adaptive mesh-refinement grids. I. Methods
• A grid of 1D low-mass star formation collapse models
• Gravitoviscous protoplanetary disks with a dust component. I. The importance of the inner sub-au region
• Dust Transport and Processing in Centrifugally Driven Protoplanetary Disk Winds
• Millimeter-sized grains in the protostellar envelopes: where do they come from?
• First Core Properties: From Low- to High-mass Star Formation
• A detailed framework to incorporate dust in hydrodynamical simulations
• The properties of the inner disk around HL Tau: Multi-wavelength modeling of the dust emission
• Determining the mid-plane conditions of circumstellar discs using gas and dust modelling: a study of HD 163296
• A (sub)millimetre study of dense cores in Orion B9
• Hydrodynamic stability in accretion disks under the combined influence of shear and density stratification
• Growing dust grains in protoplanetary discs - II. The Radial drift barrier problem
• On the structure and mass delivery towards circumplanetary discs
• Early evolution of disk, outflow, and magnetic field of young stellar objects: Impact of dust model
• Birth of convective low-mass to high-mass second Larson cores
• Astrophysical fluid simulations of thermally ideal gases with non-constant adiabatic index: numerical implementation
• A Particle Module for the PLUTO Code: III -- Dust
• Makemake + Sedna: A Continuum Radiation Transport and Photoionization Framework for Astrophysical Newtonian Fluid Dynamics
• The magnetic diffusivities in 3D radiative chemo-hydrodynamic simulations of protostellar collapse
• Formation of Dust Rings and Gaps in Non-ideal MHD Disks Through Meridional Gas Flows
• Early planet formation in embedded protostellar disks: Setting the stage for the first generation of planetesimals
• Self-Induced Dust Traps Around Snow Lines in Protoplanetary Discs
• Dust entrainment in magnetically and thermally driven disk winds
• Co-evolution of dust grains and protoplanetary disks
• The birth and early evolution of a low mass protostar
• Coagulation Instability in Protoplanetary Disks: A Novel Mechanism Connecting Collisional Growth and Hydrodynamical Clumping of Dust Particles
• Dust coagulation and fragmentation in a collapsing cloud core and their influence on non-ideal magnetohydrodynamic effects
• Conditions for justifying single-fluid approximation for charged and neutral dust fluids and a smoothed particle magnetohydrodynamics method for dust-gas mixture
• Protostellar collapse: rotation and disk formation
• Fingerprints of the protosolar cloud collapse in the Solar System I: Distribution of presolar short-lived ${}^{26}$Al
• Grain Growth During Protostellar Disk Formation
• Kinematic and thermal signatures of the directly imaged protoplanet candidate around Elias 2-24
• Implementation of dust particles in three-dimensional magnetohydrodynamics simulation: Dust dynamics in a collapsing cloud core
• Dynamics of dust grains in turbulent molecular clouds. Conditions for decoupling and limits of different numerical implementations
• Dust Motion and Possibility of Dust Growth in a Growing Circumstellar Disk
• Impact of turbulence intensity and fragmentation velocity on dust particle size evolution and non-ideal magnetohydrodynamics effects
• Fast methods to track grain coagulation and ionization. II. Extension to thermal ionization
• Pebbles in an Embedded Protostellar Disk: The Case of CB26
• The effect of Jupiter on the CAI storage problem
• On the propagation of Alfvén waves in the dusty interstellar medium. Can we neglect dust inertia in molecular clouds?
• Kinematics signature of a giant planet in the disk of AS 209
• Optical Properties of Interstellar Dust around the Orion A Molecular Cloud
• Dust growth in molecular cloud envelopes: a numerical approach

Cited by in corpus (10)

• Formation and evolution of a protoplanetary disk: combining observations, simulations and cosmochemical constraints
• Sub-Neptunes Are Drier Than They Seem: Rethinking the Origins of Water-Rich Worlds
• FAUST. XVIII. Evidence for annular substructure in a very young Class 0 disk
• FAUST XXVI. The dust opacity spectral indices of protostellar envelopes bridge the gap between interstellar medium and disks
• Planetesimal formation via the streaming instability in simulations of infall dominated young disks
• Birth of magnetized low-mass protostars and circumstellar disks
• Dust evolution by chemisputtering during protostellar formation
• Turn up the light: Radiative efficiency of protostars at birth
• Non-equilibrium condensation of the first Solar System solids
• Numerical Insights into Disk Accretion, Eccentricity, and Kinematics in the Class 0 phase