On the 3D time evolution of the dust size distribution in protostellar envelopes

Abstract

Dust plays a fundamental role during protostellar collapse, disk and planet formation. Recent observations suggest that efficient dust growth may begin early, in the protostellar envelopes, potentially even before the formation of the disk. Three-dimensional models of protostellar evolution, addressing multi-size dust growth, gas and dust dynamics and magnetohydrodynamics, are required to characterize the dust evolution in the embedded stages of star formation. We aim to establish a new framework for dust evolution models, following in 3D the dust size distribution both in time and space, in MHD models describing the formation and evolution of star-disk systems, at low numerical cost. We present our work coupling the COALA dust evolution module into the code RAMSES, performing the first 3D MHD simulation of protostellar collapse including simultaneously polydisperse dust growth modeled by the Smoluchowski equation as well as dust dynamics in the terminal velocity approximation. Ice-coated micron-sized grains can rapidly grow in the envelope and survive by not entering the fragmentation regime. The evolution of the dust size distribution is highly anisotropic due to the turbulent nature of the collapse and the development of favorable locations such as outflow cavity walls, which enhance locally the dust-to-gas ratio. We analyzed the first 3D non-ideal MHD simulations that self-consistently account for the dust dynamics and growth during the protostellar stage. Very early in the lifetime of a young embedded protostar, micron-sized grains can grow, and locally the dust size distribution deviates significantly from the MRN initial shape. This new numerical method opens the perspective to treat simultaneously gas/dust dynamics and dust growth in 3D simulations at a low numerical cost for several astrophysical environments.

Accepted for publication in A&A, 14 pages, 9 figures

References in corpus (42)

• Interstellar Dust Grains
• Cosmological Hydrodynamics with Adaptive Mesh Refinement: a new high resolution code called RAMSES
• Gas- and dust evolution in protoplanetary disks
• Closed-form expressions for particle relative velocities induced by turbulence
• Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution
• Aggregate dust particles at comet 67P/Churyumov-Gerasimenko
• Characterizing young protostellar disks with the CALYPSO IRAM-PdBI survey: large Class 0 disks are rare
• Protostellar Disk Formation Enabled by Removal of Small Dust Grains
• Grain growth in the envelopes and disks of Class I protostars
• Dust growth and evolution in protoplanetary disks
• Grain Growth and Density Distribution of the Youngest Protostellar Systems
• Variation in dust properties in a dense filament of the Taurus molecular complex (L1506)
• Including Dust Coagulation in Hydrodynamic Models of Protoplanetary Disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet
• Low dust emissivities and radial variations in the envelopes of Class 0 protostars: a signature of early grain growth?
• DustPy: A Python Package for Dust Evolution in Protoplanetary Disks
• A dynamical constraint on interstellar dust models from radiative torque disruption
• Incorporating Ambipolar and Ohmic Diffusion in the AMR MHD code RAMSES
• Probing changes of dust properties along a chain of solar-type prestellar and protostellar cores in Taurus with NIKA
• "Ash-fall" induced by molecular outflow in protostar evolution
• Protostellar collapse: the conditions to form dust rich protoplanetary disks
• Dust coagulation feedback on magnetohydrodynamic resistivities in protostellar collapse
• Protostellar collapse simulations in spherical geometry with dust coagulation and fragmentation
• Small dust grain dynamics on adaptive mesh-refinement grids. I. Methods
• Rapid Elimination of Small Dust Grains in Molecular Clouds
• Gravitoviscous protoplanetary disks with a dust component. II. Spatial distribution and growth of dust in a clumpy disk
• Planet-induced Vortices with Dust Coagulation in Protoplanetary Disks
• Gravitoviscous protoplanetary disks with a dust component. III. Evolution of gas, dust, and pebbles
• Grain growth for astrophysics with Discontinuous Galerkin schemes
• The young protostellar disk in IRAS16293-2422 B is hot and shows signatures of gravitational instability
• Fast methods for tracking grain coagulation and ionization. I. Analytic derivation
• FAUST IX. Multi-band, multi-scale dust study of L1527 IRS. Evidence for dust properties variations within the envelope of a Class 0/I YSO
• Dust coagulation and fragmentation in a collapsing cloud core and their influence on non-ideal magnetohydrodynamic effects
• Impact of magneto-rotational instability on grain growth in protoplanetary disks: I. Relevant turbulence properties
• Impact of magneto-rotational instability on grain growth in protoplanetary disks: II. Increased grain collisional velocities
• TriPoD: Tri-Population size distributions for Dust evolution. Coagulation in vertically integrated hydrodynamic simulations of protoplanetary disks
• Is the mm/submm dust polarization a robust tracer of the magnetic field topology in protostellar envelopes? A model exploration
• Dust dynamics in current sheets within protoplanetary disks. I. Isothermal models including ambipolar diffusion and Ohmic resistivity
• Dust evolution during the protostellar collapse: influence on the coupling between the neutral gas and the magnetic field
• Physical conditions for dust grain alignment in Class 0 protostellar cores II. The role of the radiation field in models aligning/disrupting dust grains
• Cometary dust collected by MIDAS on board Rosetta. I. Dust particle catalog and statistics
• The rotational disruption of porous dust aggregates from ab-initio kinematic calculations
• Dust enrichment and growth in the earliest stages of protoplanetary disk formation