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.

arXiv comment15 pages, 12 figures, 1 table, accepted for publication in ApJ

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• Resilience of Planetesimal Formation in Weakly-Reinforced Pressure Bumps
• Chemical footprints of giant planet formation. Role of planet accretion in shaping the C/O ratio of protoplanetary disks
• Formation of dust clumps with sub-Jupiter mass and cold shadowed region in gravitationally unstable disk around Class 0/I protostar in L1527 IRS
• Different degrees of nitrogen and carbon depletion in the warm molecular layers of protoplanetary disks
• Grain Growth During Protostellar Disk Formation
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