Dust coagulation feedback on magnetohydrodynamic resistivities in protostellar collapse

Abstract

The degree of coupling between the gas and the magnetic field during the collapse of a core and the subsequent formation of a disk depends on the assumed dust size distribution. We study the impact of grain-grain coagulation on the evolution of magnetohydrodynamic (MHD) resistivities during the collapse of a prestellar core. We use a 1-D model to follow the evolution of the dust size distribution, out-of-equilibrium ionization state and gas chemistry during the collapse of a prestellar core. To compute the grain-grain collisional rate, we consider models for both random and systematic, size-dependent, velocities. We include grain growth through grain-grain coagulation and ice accretion, but ignore grain fragmentation. Starting with a MRN (Mathis et al. 1977) size distribution, we find that coagulation in grain-grain collisions generated by hydrodynamical turbulence is not efficient at removing the smallest grains, and as a consequence does not affect much the evolution of the Hall and ambipolar diffusion MHD resistivities which still severly drop during the collapse like in models without coagulation. The inclusion of systematic velocities, possibly induced by the presence of ambipolar diffusion, increases the coagulation rate between small and large grains, removing small grains earlier in the collapse and therefore limiting the drop in the Hall and ambipolar diffusion resistivities. At intermediate densities ($n_{\mathrm{H}}\sim 10^8$cm${}^{-3}$), the Hall and ambipolar diffusion resistivities are found to be higher by 1 to 2 orders of magnitude in models with coagulation than in models where coagulation is ignored, and also higher than in a toy model without coagulation where all grains smaller than $0.1\mu$m would have been removed in the parent cloud before the collapse. When grain drift velocities induced by ambipolar diffusion are included, dust coagulation ... (abridged)

References in corpus (42)

• Photodissociation and photoionisation of atoms and molecules of astrophysical interest
• Photoelectric Emission from Interstellar Dust: Grain Charging and Gas Heating
• Closed-form expressions for particle relative velocities induced by turbulence
• The evolution of amorphous hydrocarbons in the ISM: dust modelling from a new vantage point
• Magnetic processes in a collapsing dense core. I Accretion and Ejection
• Protostellar disk formation and transport of angular momentum during magnetized core collapse
• Collapse of Magnetized Singular Isothermal Toroids: II. Rotation and Magnetic Braking
• Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution
• Magnetic Braking and Protostellar Disk Formation: The Ideal MHD Limit
• Mechanism of Magnetic Flux Loss in Molecular Clouds
• The Ubiquity of Micrometer-Sized Dust Grains in the Dense Interstellar Medium
• Nonideal MHD Effects and Magnetic Braking Catastrophe in Protostellar Disk Formation
• Cosmic-ray ionisation in circumstellar discs
• Dust Dynamics in Compressible MHD Turbulence
• Can non-ideal magnetohydrodynamics solve the magnetic braking catastrophe?
• Protostellar Disk Formation Enabled by Removal of Small Dust Grains
• Does Magnetic Field-Rotation Misalignment Solve the Magnetic Braking Catastrophe in Protostellar Disk Formation?
• Bimodality of circumstellar disk evolution induced by Hall current
• Interstellar chemistry of nitrogen hydrides in dark clouds
• Magnetically self-regulated formation of early protoplanetary discs
• Cosmic-ray ionisation in collapsing clouds
• Dust growth in the interstellar medium: How do accretion and coagulation interplay?
• Disk Formation in Magnetized Clouds Enabled by the Hall Effect
• Variation in dust properties in a dense filament of the Taurus molecular complex (L1506)
• The Fundamentally Different Dynamics of Dust and Gas in Molecular Clouds
• A chemical solver to compute molecule and grain abundances and non-ideal MHD resistivities in prestellar core collapse calculations
• Freeze-out and coagulation in pre-protostellar collapse
• Cosmic ray induced ionisation of a molecular cloud shocked by the W28 supernova remnant
• Effect of Grain Size on Differential Desorption of Volatile Species and on Non-ideal MHD Diffusivity
• Mantle formation, coagulation and the origin of cloud/core-shine: II. Comparison with observations
• The Nonisothermal Stage of Magnetic Star Formation. I. Formulation of the Problem and Method of Solution
• Effect of Angular Momentum Alignment and Strong Magnetic Fields on the Formation of Protostellar Disks
• Grain size limits derived from 3.6 μm and 4.5 μm coreshine
• Small dust grain dynamics on adaptive mesh-refinement grids. I. Methods
• The Dynamics of Charged Dust in Magnetized Molecular Clouds
• Ionization and Dust Charging in Protoplanetary Disks
• The magnetic diffusivities in 3D radiative chemo-hydrodynamic simulations of protostellar collapse
• Dependence of Hall Coefficient on Grain Size and Cosmic Ray Rate and Implication for Circumstellar Disk Formation
• Constraint on ion-neutral drift velocity in the Class 0 protostar B335 from ALMA observations
• Depletion and fractionation of nitrogen in collapsing cores
• The challenges of modelling microphysics: ambipolar diffusion, chemistry, and cosmic rays in MHD shocks
• Dynamical scaling in Smoluchowski's coagulation equations: uniform convergence

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• Physical Modeling of Dust Polarization from Magnetically Enhanced Radiative Torque (MRAT) Alignment in Protostellar Cores with POLARIS
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• Implementation of dust particles in three-dimensional magnetohydrodynamics simulation: Dust dynamics in a collapsing cloud core
• TriPoD: Tri-Population size distributions for Dust evolution. Coagulation in vertically integrated hydrodynamic simulations of protoplanetary disks
• Dynamics of dust grains in turbulent molecular clouds. Conditions for decoupling and limits of different numerical implementations
• Impact of turbulence intensity and fragmentation velocity on dust particle size evolution and non-ideal magnetohydrodynamics effects
• Increasing mass-to-flux ratio from the dense core to the protostellar envelope around the Class 0 protostar HH 211
• FAUST XXVI. The dust opacity spectral indices of protostellar envelopes bridge the gap between interstellar medium and disks
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• On the propagation of Alfvén waves in the dusty interstellar medium. Can we neglect dust inertia in molecular clouds?
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• Effect of dust rotational disruption by radiative torques on radiation pressure feedback from massive protostars
• Discs and outflows in the early phases of massive star formation: influence of magnetic fields and ambipolar diffusion
• "Ashfall" Induced by Molecular Outflow in Protostar Evolution. II. Analytical Study on the Maximum Size of Dust Grains Lifted by Outflows
• Dust coagulation during the early stages of star formation: molecular cloud collapse and first hydrostatic core evolution