Ice Condensation as a Planet Formation Mechanism

By K. Ros. Proceedings of the International Astronomical Union, 2013

200 citations recorded by the source corpus.

Abstract Particles in protoplanetary discs grow rapidly to millimetre-sizes via coagulation, but further growth to centimetre-sized pebbles is not yet completely understood. We investigate particle growth by ice condensation in a model where we take the dynamical behaviour of vapour and ice particles into account, as well as the size evolution due to condensation and sublimation. Our results show that efficient growth from dust to pebbles is possible close to the water ice line at ~3 AU, with particles growing from millimetres to decimetres on a time scale of 10000 yr.

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Citations in the corpus

Direct mapping of the temperature and velocity gradients in discs Imaging the vertical CO snow line around IM Lupi (2017, background): “In particular, molecular snow lines – the two-dimensional surface where abundant volatiles condensate onto dust grains – result in increased solid particle stickiness and dust-to-gas ratio, promoting particle growth (e.g. Ciesla & Cuzzi 2006; Ros & Johansen 2013).”
Concentrating small particles in protoplanetary disks through the streaming instability (2016, background): “Some interesting possibilities include photo-evaporation of the gaseous disk (Carrera et al. 2017), radial pile-up of solids (Dra̧żkowska et al. 2016; Gonzalez et al. 2017), and ice condensation and sublimation (Ros & Johansen 2013; Ida & Guillot 2016; Schoonenberg & Ormel 2017).”
The structure of protoplanetary discs around evolving young stars (2014, background): “Both of these requirements are satisfied at the ice line, where an increased amount of heavy elements is likely to be present owing to the condensation of ice grains and pebbles (Ros & Johansen 2013).”
EVIDENCE OF FAST PEBBLE GROWTH NEAR CONDENSATION FRONTS IN THE HL TAU PROTOPLANETARY DISK (2015, methodology): “Nevertheless, the model used by Ros & Johansen (2013) can in principle to be applied to other condensation fronts.”
Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, background): “In these regions we can expect particle growth to large pebble sizes and large pebble surface densities (Ros & Johansen 2013), possibly aided by the emergence of a pressure bump (Kretke & Lin 2007).”
Molecules with ALMA at Planet-forming Scales (MAPS). I. Program Overview and Highlights (2021, background): “…2017), while rapid disintegration of pebbles crossing the snowline result in traffic jams (Birnstiel et al. 2010), and diffusive flows across snowlines result in large reservoirs of solids directly outside of the snowline location (Stevenson & Lunine 1988; Ciesla & Cuzzi 2006; Ros & Johansen 2013).”
An ALMA Survey of Protoplanetary Disks in the σ Orionis Cluster (2017, background): “Finally, volatile carbon may be locked 8 up in large icy bodies in the disk midplane (Bergin et al. 2010; Ros & Johansen 2013; Guidi et al. 2016).”
The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores (2015, background): “An enhancement of the solid mass by more than a factor of 2 might have been produced by the so-called ‘‘cold-finger effect’’ (Morfill and Voelk, 1984; Ros and Johansen, 2013), but this would have happened only locally at the snowline and therefore could explain at most the formation of one giant-pla”
Dust Evolution and the Formation of Planetesimals (2016, background): “Other proposed explanations include pressure bumps formed due to magnetised turbulence (Johansen et al. 2009; Dittrich et al. 2013; Flock et al. 2015) or condensation fronts (Cuzzi & Zahnle 2004; Ros & Johansen 2013; Zhang et al. 2015; Okuzumi et al. 2015).”
Formation of planetary systems by pebble accretion and migration (2018, background): “Therefore, our work would benefit from an improved physical description of the disc edge (Flock et al. 2017), while also treating the particle size evolution through coagulation and sublimation (Ros & Johansen 2013; Schoonenberg & Ormel 2017).”
Planetesimal formation near the snowline: in or out? (2017, methodology): “However, Ros & Johansen (2013) have shown that particle growth due to diffusion and subsequent condensation of water across the vertical snowline is negligible compared to the same process across the radial snowline.”
Fluffy dust forms icy planetesimals by static compression (2013, background): “Several possibilities have been proposed to overcome these barriers (Johansen et al. 2007; Pinilla et al. 2012; Windmark et al. 2012; Lambrechts & Johansen 2012; Ros & Johansen 2013; Garaud et al. 2013).”
Pebble-isolation mass: Scaling law and implications for the formation of super-Earths and gas giants (2018, methodology): “The final pebble sizes in our model were determined by radial drift alone, where we did not take the effects of fragmentation (Brauer et al. 2008; Birnstiel et al. 2011), bouncing (Zsom et al. 2010), or condensation (Ros & Johansen 2013; Schoonenberg & Ormel 2017) into account.”
Astrochemistry and compositions of planetary systems (2020, background): “This effect can be greatly enhanced by the presence of radial drift of particles across the snowline (Ciesla and Cuzzi 2006; Ros and Johansen 2013): in the presence of a radial pressure gradient the gas orbits at sub-Keplerian velocities for a given radius (Whipple 1972; Weidenschilling 1977), resul”
A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+ (2017, background): “Enhanced settling associated with low turbulence may also lead to less grain growth across condensation fronts (Ros & Johansen 2013).”
Separating gas-giant and ice-giant planets by halting pebble accretion (2014, background): “In these regions particle sizes and the local surface density are set by a condensation-sublimation cycle across the ice line, resembling hail formation (Ros & Johansen 2013).”