Evolution of Dust In Protoplanetary Disks With Magnetized Winds

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   The impact of dust evolution on the dead zone outer edge in magnetized protoplanetary disks

   Timmy N. Delage, Matías Gárate, Satoshi Okuzumi et al. · 2023 · A&A 674, A190 (2023) · cited 7 times · AI summary available

   Abstract

   [Abridged] Aims. We provide an important step toward a better understanding of the magnetorotational instability (MRI)-dust coevolution in protoplanetary disks by presenting a proof of concept that dust evolution ultimately plays a crucial role in the MRI activity. Methods. First, we study how a fixed power-law dust size distribution with varying parameters impacts the MRI activity, especially the steady-state MRI-driven accretion, by employing and improving our previous 1+1D MRI-driven turbulence model. Second, we relax the steady-state accretion assumption in this disk accretion model, and partially couple it to a dust evolution model in order to investigate how the evolution of dust (dyna…

2. Very close Not relevant

   Toward a Population Synthesis of Disks and Planets I. Evolution of Dust with Entrainment in Winds and Radiation Pressure

   Remo Burn, Alexandre Emsenhuber, Jesse Weder et al. · 2022 · A&A 666, A73 (2022) · cited 2 times · AI summary available

   Abstract

   Millimeter astronomy provides valuable information on the birthplaces of planetary systems. In order to compare theoretical models with observations, the dust component has to be carefully calculated. Here, we aim to study the effects of dust entrainment in photoevaporative winds and the ejection and drag of dust due to effects caused by radiation from the central star. We improved and extended the existing implementation of a two-population dust and pebble description in the global Bern/Heidelberg planet formation and evolution model. Modern prescriptions for photoevaporative winds were used and we account for settling and advection of dust when calculating entrainment rates. In order to pr…

3. Very close Not relevant

   Planet-disk-wind interaction: the magnetized fate of protoplanets

   Gaylor Wafflard-Fernandez, Geoffroy Lesur · 2023 · Solar and Stellar Astrophysics · cited 11 times · AI summary available

   Abstract

   Models of planet-disk interaction are mainly based on 2D and 3D viscous hydrodynamical simulations. Accretion is classically prescribed by an alpha parameter which characterizes the turbulent radial transport of angular momentum (AM) in the disk. This accretion scenario has been questioned for a few years and an alternative paradigm has been proposed that involves the vertical transport of AM by MHD winds. We revisit planet-disk interaction in such context, with a focus on the planet's ability to open a gap and produce meridional flows. Accretion, magnetic field and wind torque in the gap are also explored, as well as the gravitational torque exerted by the disk onto the planet. We carry out…

4. Very close Not relevant

   Coevolution of Dust Growth and Gravitational Instability in Massive Protostellar Disks

   Ryota Yamamuro, Ryoki Matsukoba, Kei E. I. Tanaka et al. · 2026 · Solar and Stellar Astrophysics · AI summary available

   Abstract

   Massive protostellar disks are expected to sustain high accretion rates through gravitational instability, while dust growth may modify their opacity, cooling efficiency, and stability. Conversely, the time-dependent and nonaxisymmetric structures produced by gravitational instability may regulate the local conditions for dust growth. However, the coupled evolution of dust growth and gravitational instability in massive protostellar disks has not yet been explored self-consistently. We present two-dimensional hydrodynamic simulations that follow gas dynamics, dust growth, and opacity-dependent radiative cooling in a massive protostellar disk. We find that dust grains rapidly grow to millimet…

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   A question of personalities: evolution of viscous and wind-driven protoplanetary discs in the presence of dead zones

   Simin Tong, Richard Alexander, Giovanni Rosotti · 2024 · Earth and Planetary Astrophysics · cited 4 times · AI summary available

   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…

6. Very close Not relevant

   Revised description of dust diffusion and a new instability creating multiple rings in protoplanetary disks

   Ryosuke T. Tominaga, Sanemichi Z. Takahashi, Shu-ichiro Inutsuka · 2019 · Earth and Planetary Astrophysics · cited 41 times · AI summary available

   Abstract

   Various instabilities have been proposed as a promising mechanism to accumulate dust. Moreover, some of them are expected to lead to the multiple-ring structure formation and the planetesimal formation in protoplanetary disks. In a turbulent gaseous disk, the growth of the instabilities and the dust accumulation are quenched by turbulent diffusion of dust grains. The diffusion process has been often modeled by a diffusion term in the continuity equation for the dust density. The dust diffusion model, however, does not guarantee the angular momentum conservation in a disk. In this study, we first formulate equations that describe the dust diffusion and also conserve the total angular momentum…

7. Very close Not relevant

   Coagulation-Fragmentation Equilibrium for Charged Dust: Abundance of Submicron Grains Increases Dramatically in Protoplanetary Disks

   Vitaly Akimkin, Alexei V. Ivlev, Paola Caselli et al. · 2023 · Solar and Stellar Astrophysics · cited 4 times · AI summary available

   Abstract

   Dust coagulation in protoplanetary disks is not straightforward and is subject to several slow-down mechanisms, such as bouncing, fragmentation and radial drift to the star. Furthermore, dust grains in UV-shielded disk regions are negatively charged due to collisions with the surrounding electrons and ions, which leads to their electrostatic repulsion. For typical disk conditions, the relative velocities between micron-size grains are small and their collisions are strongly affected by the repulsion. On the other hand, collisions between pebble-size grains can be too energetic, leading to grain fragmentation. The aim of the present paper is to study a combined effect of the electrostatic and…

8. Very close Not relevant

   Electric heating and angular momentum transport in laminar models of protoplanetary disks

   William 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…