An alternative look at the snowline in protoplanetary disks

Abstract

We have calculated an evolution of protoplanetary disk from an extensive set of initial conditions using a time-dependent model capable of simultaneously keeping track of the global evolution of gas and water-ice. A number of simplifications and idealizations allows for an embodiment of gas-particle coupling, coagulation, sedimentation, and evaporation/condensation processes. We have shown that, when the evolution of ice is explicitly included, the location of the snowline has to be calculated directly as the inner edge of the region where ice is present and not as the radius where disk's temperature equals the evaporation temperature of water-ice. The final location of the snowline is set by an interplay between all involved processes and is farther from the star than implied by the location of the evaporation temperature radius. The evolution process naturally leads to an order of magnitude enhancement in surface density of icy material.

arXiv commentAccepted for publication in A&A. 8 pages, 4 figures

References in corpus (4)

• Models of the in situ formation of detected extrasolar giant planets
• On the Snow Line in Dusty Protoplanetary Disks
• Extra-Solar Planets
• Models of the formation of the planets in the 47 UMa system

Cited by in corpus (18)

• A simple model for the evolution of the dust population in protoplanetary disks
• Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution
• High-resolution simulations of the final assembly of Earth-like planets 1: terrestrial accretion and dynamics
• Extrasolar planet population synthesis IV. Correlations with disk metallicity, mass and lifetime
• Can Planets survive Stellar Evolution?
• Grain opacity and the bulk composition of extrasolar planets. I. Results from scaling the ISM opacity
• Equilibrium Condensation from Chondritic Porous IDP Enriched Vapor: Implications for Mercury and Enstatite Chondrite Origins
• Global Modeling of Nebulae with Particle Growth, Drift and Evaporation Fronts. I: Methodology and Typical Results
• Formation of giant planets in disks with different metallicities
• Planets in triple star systems--the case of HD188753
• Consequences of the simultaneous formation of giant planets by the core accretion mechanism
• Formation of giant planets around stars with various masses
• K2-99: a subgiant hosting a transiting warm Jupiter in an eccentric orbit and a long-period companion
• Evolution of dust in protoplanetary disks of eruptive stars
• Gravitoviscous protoplanetary disks with a dust component. III. Evolution of gas, dust, and pebbles
• A Link Between the Semi-Major Axis of Extrasolar Gas Giant Planets and Stellar Metallicity
• The Invisible Majority? Evolution and Detection of Outer Planetary Systems without Gas Giants
• Formation of pebbles in (gravito-)viscous protoplanetary disks with various turbulent strengths