Evolution of Dust In Protoplanetary Disks With Magnetized Winds
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 (αturb = 10−5) where magnetized winds drive most of the accretion (Ṁacc,tot ≃ Ṁwind,acc), and wind-driven mass loss comparable to the accretion rate (Ṁwind,outflow ≃ Ṁacc,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.
Related
- The ALMA Survey of Gas Evolution of PROtoplanetary disks (AGE-PRO): Evolution of dust properties from multi-wavelength observations
- The ALMA Survey of Gas Evolution of PROtoplanetary disks (AGE-PRO): Evolution of dust properties from multi-wavelength observations
- Simulating the thermodynamics of gas, radiation, and multispecies dust. Method and applications to protoplanetary disks
- The colors of protoplanetary disks. Impact of nonspherical dust particles on the polarized and total intensity colors
- Simulating the thermodynamics of gas, radiation, and multispecies dust: Method and applications to protoplanetary disks
BibTeX
@misc{goksu2026evolution,
title = {{Evolution of Dust In Protoplanetary Disks With Magnetized Winds}},
author = {Olcay Goksu and Ralph Pudritz and Timmy Delage},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.08484},
eprint = {2611.08484},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.08484},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Evolution of Dust In Protoplanetary Disks With Magnetized Winds
AU - Olcay Goksu
AU - Ralph Pudritz
AU - Timmy Delage
PY - 2026
DA - 2026/11/05
PB - arXiv
DO - 10.48550/arxiv.2611.08484
UR - https://arxiv.org/abs/2611.08484
AB - 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_turb = 10^−5) where magnetized winds drive most of the accretion (Ṁ_acc,tot ≃ Ṁ_wind,acc), and wind-driven mass loss comparable to the accretion rate (Ṁ_wind,outflow ≃ Ṁ_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.
ER -