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.

Accepted to A&A Letters

References in corpus (4)

• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• Imaging the water-snow line during a protostellar outburst
• Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line
• Collisions between sintered icy aggregates

Cited by in corpus (11)

• Dust continuum emission and the upper limit fluxes of sub-millimeter water lines of the protoplanetary disk around HD 163296 observed by ALMA
• Millimeter-sized Dust Grains Appear Surviving the Water-sublimating Temperature in the Inner 10 au of the FU Ori Disk
• Evolution of dust in protoplanetary disks of eruptive stars
• Collisional evolution of dust and water ice in protoplanetary discs during and after an accretion outburst
• The water-ice line as a birthplace of planets: Implications of a species-dependent dust fragmentation threshold
• 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
• Accretion bursts in young intermediate-mass stars make planet formation challenging
• Super-Earth formation in systems with cold giants