Evolution of Dust In Protoplanetary Disks With Magnetized Winds
Authors: Olcay Goksu, Ralph Pudritz, Timmy Delage
Abstract
Observations and theory increasingly indicate that protoplanetary disks are weakly turbulent, implying that magnetized disk winds may dominate their angular momentum transport and long-term evolution. Yet dust evolution in wind-dominated disks remains poorly understood, despite its importance for planet formation. In particular, whether wind-dominated disk evolution can create regions with enhanced dust-to-gas mass ratios that enable planetesimal formation via the streaming instability is unclear. We build a parametric hybrid disk evolution model that includes turbulent accretion, wind-driven accretion, and wind-driven mass loss to investigate dust evolution in magnetized protoplanetary disks. We employ this model to carry out a parameter study in which the initial total accretion rate, the wind-driven mass loss rate, and the turbulence strength are varied. We find that although wind-dominated disks are more favorable to dust growth and concentration than turbulence-dominated disks, conditions suitable for the streaming instability arise only within the inner few au and only under the most extreme conditions: very weak turbulence ($α_\text{turb} = 10^{-5}$) where magnetized winds drive most of the accretion ($\dot{M}_\text{acc,tot} \simeq \dot{M}_\text{wind,acc}$), and wind-driven mass loss comparable to the accretion rate ($\dot{M}_\text{wind,outflow} \simeq \dot{M}_\text{acc,wind}$). Our results therefore imply that, beyond the inner few au, the parametric wind-driven evolution models considered in the literature do not by themselves produce conditions suitable for planetesimal formation via the streaming instability, motivating more physically complete models in which spontaneous, long-lived dust traps can arise.
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Abstract
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Abstract
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Abstract
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Abstract
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Abstract
Whether the angular momentum of protoplanetary discs is redistributed by viscosity or extracted by magnetised winds is a long-standing question. Demographic indicators, such as gas disc sizes and stellar accretion rates, have been proposed as ways of distinguishing between these two mechanisms. In this paper, we implement one-dimensional gas simulations to study the evolution of "hybrid" protoplanetary discs simultaneously driven by viscosity and magnetised winds, with dead zones present. We explore how the variations of disc properties, including initial disc sizes, dead zone sizes and angular momentum transport efficiency, affect stellar accretion rates, disc surface density profiles, disc…
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Abstract
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Abstract
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Electric heating and angular momentum transport in laminar models of protoplanetary disksWilliam Béthune, Henrik Latter · 2020 · Earth and Planetary Astrophysics · cited 13 times · AI summary available
Abstract
The vertical temperature structure of a protoplanetary disk bears on several processes relevant to planet formation, such as gas and dust grain chemistry, ice lines and convection. The temperature profile is controlled by irradiation from the central star and by any internal source of heat as caused by gas accretion. We investigate the heat and angular momentum transport generated by the resistive dissipation of magnetic fields in laminar disks. We use local one-dimensional simulations to obtain vertical temperature profiles for typical conditions in the inner disk (0.5 to 4 au). Using simple assumptions for the gas ionization and opacity, the heating and cooling rates are computed self-cons…
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