Ring formation by coagulation of dust aggregates in early phase of disk evolution around a protostar

Abstract

Ring structures are observed by (sub-)millimeter dust continuum emission in various circumstellar disks from early stages of Class 0 and I to late stage of Class II young stellar objects (YSOs). In this paper, we study one of the possible scenarios of such ring formation in early stage, which is coagulation of dust aggregates. The dust grains grow in an inside-out manner because the growth timescale is roughly proportional to the orbital period. The boundary of the dust evolution can be regarded as the growth front, where the growth time is comparable to the disk age. With radiative transfer calculations based on the dust coagulation model, we find that the growth front can be observed as a ring structure because dust surface density is sharply changed at this position. Furthermore, we confirm that the observed ring positions in the YSOs with an age of $\lesssim 1$ Myr are consistent with the growth front. The growth front could be important to create the ring structure in particular for early stage of the disk evolution such as Class 0 and I sources.

15 pages, 12 figures, 1 table, accepted for publication in ApJ

References in corpus (20)

• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Gas- and dust evolution in protoplanetary disks
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Closed-form expressions for particle relative velocities induced by turbulence
• Gaps, Rings, and Non-Axisymmetric Structures in Protoplanetary Disks - From Simulations to ALMA Observations
• Evidence of fast pebble growth near condensation fronts in the HL Tau protoplanetary disk
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. A Statistical Characterization of Class 0 and I Protostellar Disks
• Mass Estimates of a Giant Planet in a Protoplanetary Disk from the Gap Structures
• One Solution to the Mass Budget Problem for Planet Formation: Optically Thick Disks with Dust Scattering
• Formation of a Keplerian disk in the infalling envelope around L1527 IRS: transformation from infalling motions to Kepler motions
• Four annular structures in a protostellar disk less than 500,000 years old
• Protoplanetary disk rings and gaps across ages and luminosities
• The anomalously low (sub)millimeter spectral indices of some protoplanetary disks may be explained by dust self-scattering
• ALMA Observations of Infalling Flows toward the Keplerian Disk around the Class I Protostar L1489 IRS
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. III. Substructures in Protostellar Disks
• Growth and migration of solids in evolving protostellar disks I: Methods and Analytical tests
• ALMA Observations of the Protostar L1527 IRS: Probing Details of the Disk and the Envelope Structures
• Spontaneous ring formation in wind-emitting accretion discs
• Spiral Arms, Infall, and Misalignment of the Circumbinary Disk from the Circumstellar Disks in the Protostellar Binary System L1551 NE
• Substructure Formation in a Protostellar Disk of L1527 IRS

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• Different degrees of nitrogen and carbon depletion in the warm molecular layers of protoplanetary disks
• Grain Growth During Protostellar Disk Formation
• No evidence of the significant grain growth but tentative discovery of disk substructure in a disk around the Class I Protostar L1489 IRS
• Physical conditions for dust grain alignment in Class 0 protostellar cores II. The role of the radiation field in models aligning/disrupting dust grains
• On the origin of transition disk cavities: Pebble-accreting protoplanets vs Super-Jupiters
• On the crystallinity of silicate dust in evolving protoplanetary disks due to magnetically driven disk winds
• Multi-scale Dust Polarization and Spiral-like Stokes-I Residual in the Class I Protostellar System TMC-1A
• NIKA2 observations of dust grain evolution from star-forming filament to T-Tauri disk: Preliminary results from NIKA2 observations of the Taurus B211/B213 filament
• A VLA View of the Flared, Asymmetric Disk Around the Class 0 Protostar L1527 IRS