Dust Motion and Possibility of Dust Growth in a Growing Circumstellar Disk

Abstract

We calculate the evolution of a star-forming cloud core using a three-dimensional resistive magnetohydrodynamics simulation, treating dust grains as Lagrangian particles, to investigate the dust motion in the early star formation stage. We prepare six different-sized set of dust particles in the range $a_{\mathrm{d}}=0.01$--$1000\mu$m, where $a_{\mathrm{d}}$ is the dust grain size. In a gravitationally collapsing cloud, a circumstellar disk forms around a protostar and drives a protostellar outflow. Almost all the small dust grains ($a_{\mathrm{d}}\lesssim 10$--$100\mu$m) initially distributed in the region ${\theta }_0\lesssim 45^{\circ }$ are ejected from the center by the outflow, where ${\theta }_0$ is the initial zenith angle relative to the rotation axis, whereas only a small number of the large dust grains ($a_{\mathrm{d}}\gtrsim 100\mu$m) distributed in the region are ejected. All other grains fall onto either the protostar or disk without being ejected by the outflow. Regardless of the dust grain size, the behavior of the dust motion is divided into two trends after dust particles settle into the circumstellar disk. The dust grains reaching the inner disk region from the upper envelope preferentially fall onto the protostar, while those reaching the outer disk region or disk outer edge from the envelope can survive without an inward radial drift. These surviving grains can induce dust growth. Thus, we expect that the outer disk regions could be a favored place of planet formation.

arXiv commentAccepted for publication in MNRAS. 30 pages, 12 figures

References in corpus (48)

• 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
• Closed-form expressions for particle relative velocities induced by turbulence
• Rapid Coagulation of Porous Dust Aggregates Outside the Snow Line: A Pathway to Successful Icy Planetesimal Formation
• Observations of Protoplanetary Disk Structures
• Sintering-induced Dust Ring Formation in Protoplanetary Disks: Application to the HL Tau Disk
• Magnetic processes in a collapsing dense core. I Accretion and Ejection
• A Circumplanetary Disk Around PDS70c
• Outflows and Jets from Collapsing Magnetized Cloud Cores
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Protostellar Core Formation
• Mechanism of Magnetic Flux Loss in Molecular Clouds
• Dust masses of young disks: constraining the initial solid reservoir for planet formation
• On the water delivery to terrestrial embryos by ice pebble accretion
• Magnetic Fields and Rotations of Protostars
• Evolution of Protostellar Outflow around Low-mass Protostar
• Conditions for Circumstellar Disk Formation: Effects of Initial Conditions and Sink Treatment
• An Atmospheric Structure Equation for Grain Growth
• Bimodality of circumstellar disk evolution induced by Hall current
• The Origin and Formation of the Circumstellar Disk
• Grand Design Spiral Arms in A Young Forming Circumstellar Disk
• First MHD Simulation of Collapse and Fragmentation of Magnetized Molecular Cloud Cores
• Low dust emissivities and radial variations in the envelopes of Class 0 protostars: a signature of early grain growth?
• Evolution of Rotating Molecular Cloud Core with Oblique Magnetic Field
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. III. Substructures in Protostellar Disks
• There is no magnetic braking catastrophe: Low-mass star cluster and protostellar disc formation with 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
• Highly Ordered and Pinched Magnetic Fields in the Class 0 Proto-Binary System L1448 IRS 2
• "Ash-fall" induced by molecular outflow in protostar evolution
• Protostellar collapse: the conditions to form dust rich protoplanetary disks
• Indirect evidence of significant grain growth in young protostellar envelopes from polarized dust emission
• First Direct Simulation of Brown Dwarf Formation in a Compact Cloud Core
• Formation and evolution of protostellar accretion discs. II. From 3D simulation to a simple semi-analytic model of Class 0/I discs
• What is the role of stellar radiative feedback in setting the stellar mass spectrum?
• FRagmentation and Evolution of dense cores Judged by ALMA (FREJA). I (Overview). Inner $\sim$1000 au structures of prestellar/protostellar cores in Taurus
• Formation and evolution of protostellar accretion discs. I. Angular-momentum budget, gravitational self-regulation, and numerical convergence
• Structure Formation in a Young Protoplanetary Disk by a Magnetic Disk Wind
• Early evolution of disk, outflow, and magnetic field of young stellar objects: Impact of dust model
• Fast methods for tracking grain coagulation and ionization. I. Analytic derivation
• Dependence of Hall Coefficient on Grain Size and Cosmic Ray Rate and Implication for Circumstellar Disk Formation
• Conditions for justifying single-fluid approximation for charged and neutral dust fluids and a smoothed particle magnetohydrodynamics method for dust-gas mixture
• Dust coagulation and fragmentation in a collapsing cloud core and their influence on non-ideal magnetohydrodynamic effects
• Testing Disk Identification Methods Through Numerical Simulations of Protostellar Evolution
• Grain Growth During Protostellar Disk Formation
• Implementation of dust particles in three-dimensional magnetohydrodynamics simulation: Dust dynamics in a collapsing cloud core
• Growth of Magnetorotational Instability in Circumstellar Disks around Class 0 Protostars
• Fast methods to track grain coagulation and ionization. II. Extension to thermal ionization
• On the crystallinity of silicate dust in evolving protoplanetary disks due to magnetically driven disk winds
• Protoplanetary disk formation from the collapse of a prestellar core

Cited by in corpus (5)

• Formation and evolution of a protoplanetary disk: combining observations, simulations and cosmochemical constraints
• Mixing is easy: New insights for cosmochemical evolution from pre-stellar core collapse
• Impact of turbulence intensity and fragmentation velocity on dust particle size evolution and non-ideal magnetohydrodynamics effects
• Non-equilibrium condensation of the first Solar System solids
• Dust enrichment and growth in the earliest stages of protoplanetary disk formation