What pebbles are made of: Interpretation of the V883 Ori disk

Abstract

Recently, an Atacama Large Millimeter/submillimeter Array (ALMA) observation of the water snow line in the protoplanetary disk around the FU Orionis star V883 Ori was reported. The radial variation of the spectral index at mm-wavelengths around the snow line was interpreted as being due to a pileup of particles interior to the snow line. However, radial transport of solids in the outer disk operates on timescales much longer than the typical timescale of an FU Ori outburst ($10^1$--$10^2$ yr). Consequently, a steady-state pileup is unlikely. We argue that it is only necessary to consider water evaporation and re-coagulation of silicates to explain the recent ALMA observation of V883 Ori because these processes are short enough to have had their impact since the outburst. Our model requires the inner disk to have already been optically thick before the outburst, and our results suggest that the carbon content of pebbles is low.

arXiv commentAccepted to A&A Letters

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Cited by in corpus (17)

• A Near-IR Spectroscopic Survey of FU Orionis Objects
• The ice composition in the disk around V883 Ori revealed by its stellar outburst
• How cores grow by pebble accretion I. Direct core growth
• Methanol and its relation to the water snowline in the disk around the young outbursting star V883 Ori
• A Lagrangian Model for Dust Evolution in Protoplanetary Disks: Formation of Wet and Dry Planetesimals at Different Stellar Masses
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• Millimeter-sized Dust Grains Appear Surviving the Water-sublimating Temperature in the Inner 10 au of the FU Ori Disk
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• Thermal processing of primordial pebbles in evolving protoplanetary disks
• Solving for the 2D Water Snowline with Hydrodynamic Simulations. Emergence of gas outflow, water cycle and temperature plateau
• A Chemical Map of the Outbursting V883 Ori system: Vertical and Radial Structures
• Fast formation of large ice pebbles after FU Orionis outbursts
• Super-Earth formation in systems with cold giants
• Accretion bursts in young intermediate-mass stars make planet formation challenging