Structure Formation in a Young Protoplanetary Disk by a Magnetic Disk Wind

Abstract

Structure formation in young protoplanetary disks is investigated using a one-dimensional model including the formation and the evolution of disks. Recent observations with ALMA found that a ring-hole structure may be formed in young protoplanetary disks, even when the disk is embedded in the envelope. We present a one-dimensional model for the formation of a protoplanetary disk from a molecular cloud core and its subsequent long-term evolution within a single framework. Such long-term evolution has not been explored by numerical simulations due to the limitation of computational power. In our model, we calculate the time evolution of the surface density of the gas and the dust with the wind mass loss and the radial drift of the dust in the disk. We find that the MHD disk wind is a viable mechanism for the formation of ring-hole structure in young disks. We perform a parameter study of our model and derive condition of the formation of ring-hole structures within $6\times 10^5$ years after the start of the collapse of the molecular cloud core. The final outcome of the disk shows five types of morphology and this can be understood by comparing the timescale of the viscous diffusion, the mass loss by MHD disk wind and the radial drift of the dust. We discuss the implication of the model for the WL 17 system, which is suspected to be an embedded, yet transitional, disk.

18pages, 16 figures, accepted for publication in the Astrophysical Journal

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Cited by in corpus (25)

• Observations of Protoplanetary Disk Structures
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. III. Substructures in Protostellar Disks
• The formation of rings and gaps in wind-launching non-ideal MHD disks: three-dimensional simulations
• Early Planet Formation in Embedded Disks (eDisk). IV. The Ringed and Warped Structure of the Disk around the Class I Protostar L1489 IRS
• Ring formation by coagulation of dust aggregates in early phase of disk evolution around a protostar
• Pebble accretion in class 0/I YSOs as a possible pathway for early planet formation
• FAUST IX. Multi-band, multi-scale dust study of L1527 IRS. Evidence for dust properties variations within the envelope of a Class 0/I YSO
• Planetesimal formation at the gas pressure bump following a migrating planet I. Basic characteristics of the new formation model
• Formation of dust clumps with sub-Jupiter mass and cold shadowed region in gravitationally unstable disk around Class 0/I protostar in L1527 IRS
• New growth mechanism of dust grains in protoplanetary disks with magnetically driven disk winds
• Primordial Dusty Rings and Episodic Outbursts in Protoplanetary Discs
• DBNets: A publicly available deep learning tool to measure the masses of young planets in dusty protoplanetary discs
• IRAS4A1: Multi-wavelength continuum analysis of a very flared Class 0 disk
• Self-consistent ring model in protoplanetary disks: temperature dips and substructure formation
• No evidence of the significant grain growth but tentative discovery of disk substructure in a disk around the Class I Protostar L1489 IRS
• Dust Motion and Possibility of Dust Growth in a Growing Circumstellar Disk
• Magnetohydrodynamics in a Cylindrical Shearing Box
• Dust rings as a footprint of planet formation in a protoplanetary disk
• Formation of multiple-planet systems in resonant chains around M dwarfs
• Detection of Substructures in Young Transition Disk WL 17
• On the origin of transition disk cavities: Pebble-accreting protoplanets vs Super-Jupiters
• Planetesimal formation by the gravitational instability of dust ring structures
• Modelling the secular evolution of proto-planetary disc dust sizes -- A comparison between the viscous and magnetic wind case
• On the crystallinity of silicate dust in evolving protoplanetary disks due to magnetically driven disk winds
• A VLA View of the Flared, Asymmetric Disk Around the Class 0 Protostar L1527 IRS