Impact of Dust Size Distribution Including Large Dust Grains on Magnetic Resistivity: An Analytical Approach

Tsukamoto, Yusuke; Okuzumi, Satoshi

doi:10.3847/1538-4357/ac7b7b

Cited by 13 publications

(13 citation statements)

References 42 publications

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“…For the resistivity model, we adopt the analytical resistivity formula described in Tsukamoto & Okuzumi (2022) in which we analytically solve the equations for chemical equilibrium in the gas phase and detailed balance equations for dust charging. The dust size distribution considered in resistivity calculations is set to be…”

Section: Resistivity Calculationsmentioning

confidence: 99%

“…In protoplanetary disks, dust grains are not only the building blocks of the planets, but also play a key role in determining the ionization degree of the disk gas by adsorbing charged particles (ions and electrons) in the gas phase. Since the ionization degree determines the magnetic resistivity, i.e., the degree of coupling between the gas and magnetic field, the microscopic nature (µm to cm scale) of the dust grains is expected to influence the macroscopic disk evolution (100 AU, i.e., 10 15 cm scale) via magnetic resistivity (Zhao et al 2016;Marchand et al 2020;Guillet et al 2020;Tsukamoto & Okuzumi 2022).…”

Section: Introductionmentioning

confidence: 99%

“…Therefore, the adsorption of charged particles by the dust grains becomes ineffective, and the gas-phase ionization degree is expected to increase and magnetic resistivity to decrease accordingly. Recent studies on dust growth and associated changes in magnetic resistivity have shown a decrease in magnetic resistivity (Zhao et al 2016;Marchand et al 2020;Guillet et al 2020;Tsukamoto & Okuzumi 2022; Kawasaki et al 2022), and some studies have also shown changes in gas dynamics as a result (Lebreuilly et al 2023;Marchand et al 2023).…”

Section: Introductionmentioning

confidence: 99%

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Co-evolution of dust grains and protoplanetary disks

Tsukamoto¹,

Machida²,

Inutsuka³

2023

Preprint

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We propose a new evolutionary process of protoplanetary disks "co-evolution of dust grains and protoplanetary disks", revealed by dust-gas two-fluid non-ideal magnetohydrodynamics simulations considering the growth of dust and associated changes in magnetic resistivity. We found that the dust growth significantly affects disk evolution by changing the coupling between the gas and magnetic field. Moreover, once the dust grains sufficiently grow, the physical quantities (e.g., density and magnetic field) of the disk are well described by nontrivial power laws, regardless of the details of the dust model. In this disk structure, the radial profile of density is steeper and the disk mass is smaller than those of the model ignoring dust growth and they are more consistent with the disk observations. We analytically derive these power laws from the basic equations of non-ideal magnetohydrodynamics. The analytical power laws are determined only by observable physical quantities, e.g., central stellar mass and mass accretion rate, and do not include difficult-to-determine parameters e.g., viscous parameter α. Therefore, they are applicable to various stages of disk evolution. We believe that the disk structure provides a new basis for future studies on star and planet formation.

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Section: Resistivity Calculationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Co-evolution of dust grains and protoplanetary disks

Tsukamoto¹,

Machida²,

Inutsuka³

2023

Preprint

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“…Besides, dust grains are the main reservoirs of negative charges and thus also contribute to the conductivity. Therefore, the density, cosmic-ray ionization rate, and dust grain size distribution in a protostellar source can significantly affect the diffusion rates (Dapp et al 2012;Padovani et al 2014;Marchand et al 2016;Zhao et al 2016;Dzyurkevich et al 2017;Guillet et al 2020;Tsukamoto et al 2020;Kawasaki et al 2022;Tsukamoto & Okuzumi 2022). Observationally, it remains unclear at which scale the nonideal MHD effects become efficient.…”

Section: Introductionmentioning

confidence: 99%

Increasing Mass-to-flux Ratio from the Dense Core to the Protostellar Envelope around the Class 0 Protostar HH 211

Yen

Koch

Lee

et al. 2023

ApJ

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To study the transportation of magnetic flux from large to small scales in protostellar sources, we analyzed the Nobeyama 45 m N2H+ (1–0), JCMT 850 μm polarization, and Atacama Large Millimeter/submillimeter Array (ALMA) C18O (2–1) and 1.3 and 0.8 mm (polarized) continuum data of the Class 0 protostar HH 211. The magnetic field strength in the dense core on a 0.1 pc scale was estimated with the single-dish line and polarization data using the Davis–Chandrasekhar–Fermi method, and that in the protostellar envelope on a 600 au scale was estimated from the force balance between the gravity and magnetic field tension by analyzing the gas kinematics and magnetic field structures with the ALMA data. Our analysis suggests that from 0.1 pc–600 au scales, the magnetic field strength increases from 40–107 μG to 0.3–1.2 mG with a scaling relation between the magnetic field strength and density of B ∝ ρ 0.36±0.08, and the mass-to-flux ratio increases from 1.2–3.7 to 9.1–32.3. The increase in the mass-to-flux ratio could suggest that the magnetic field is partially decoupled from the neutral matter between 0.1 pc and 600 au scales, and hint at efficient ambipolar diffusion in the infalling protostellar envelope in HH 211, which is the dominant nonideal magnetohydrodynamic effect considering the density on these scales. Thus, our results could support the scenario of efficient ambipolar diffusion enabling the formation of the 20 au Keplerian disk in HH 211.

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“…They play a fundamental role in the cooling of star forming clouds through their absorption and thermal emission (McKee & Ostriker 2007), as well as their chemistry as privileged formation site of H 2 (Gould & Salpeter 1963). In addition, dust grains have a major impact on the coupling between the neutrals and the magnetic field through the magnetic resistivities (see for e.g., Marchand et al 2016;Zhao et al 2016;Marchand et al 2021;Tsukamoto & Okuzumi 2022). Last but not least, the grains are the building blocks of planets that are expected to be formed by the coagulation and local accumulation of dust in protoplanetary disks (see the review by Testi et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Protostellar collapse simulations in spherical geometry with dust coagulation and fragmentation

Lebreuilly¹,

Vallucci-Goy²,

Guillet³

et al. 2022

Preprint

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We model the coagulation and fragmentation of dust grains during the protostellar collapse with our newly developed shark code. It solves the gas-dust hydrodynamics in a spherical geometry and the coagulation/fragmentation equation. It also computes the ionization state of the cloud and the Ohmic, ambipolar and Hall resistivities. We find that the dust size distribution evolves significantly during the collapse, large grain formation being controlled by the turbulent differential velocity. When turbulence is included, only ambipolar diffusion remains efficient at removing the small grains from the distribution, brownian motion is only efficient as a standalone process. The macroscopic gas-dust drift is negligible for grain growth and only dynamically significant near the first Larson core. At high density, we find that the coagulated distribution is unaffected by the initial choice of dust distribution. Strong magnetic fields are found to enhance the small grains depletion, causing an important increase of the ambipolar diffusion. This hints that the magnetic field strength could be regulated by the small grain population during the protostellar collapse. Fragmentation could be effective for bare silicates, but its modeling relies on the choice of ill-constrained parameters. It is also found to be negligible for icy grains. When fragmentation occurs, it strongly affects the magnetic resistivities profiles. Dust coagulation is a critical process that needs to be fully taken into account during the protostellar collapse. The onset and feedback of fragmentation remains uncertain and its modeling should be further investigated.

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Impact of Dust Size Distribution Including Large Dust Grains on Magnetic Resistivity: An Analytical Approach

Cited by 13 publications

References 42 publications

Co-evolution of dust grains and protoplanetary disks

Co-evolution of dust grains and protoplanetary disks

Increasing Mass-to-flux Ratio from the Dense Core to the Protostellar Envelope around the Class 0 Protostar HH 211

Protostellar collapse simulations in spherical geometry with dust coagulation and fragmentation

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