Material Enhancement in Protoplanetary Nebulae by Particle Drift through Evaporation Fronts

By J. Cuzzi, K. Zahnle. 2004

175 citations recorded by the source corpus.

Solid material in a protoplanetary nebula is subject to vigorous redistribution processes relative to the nebula gas. Meter-sized particles drift rapidly inward near the nebula midplane, and material evaporates when the particles cross a condensation/evaporation boundary. The material cannot be removed as fast in its vapor form as it is being supplied in solid form, so its concentration increases locally by a large factor (more than an order of magnitude under nominal conditions). As time goes on, the vapor-phase enhancement propagates for long distances inside the evaporation boundary (potentially all the way into the star). Meanwhile, material is enhanced in its solid form over a characteristic length scale outside the evaporation boundary. This effect is applicable to any condensible (water, silicates, etc.). Three distinct radial enhancement/depletion regimes can be discerned by use of a simple model. Meteoritic applications include oxygen fugacity and isotopic variations, as well as isotopic homogenization in silicates. Planetary system applications include more robust enhancement of solids in Jupiter's core formation region than previously suggested. Astrophysical applications include differential, time-dependent enhancement of vapor phase CO and H2O in the terrestrial planet regions of actively accreting protoplanetary disks.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c766fdbf04c52088cc760cd6f7c542b1d8fdc64f

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Citations in the corpus

Ice Condensation as a Planet Formation Mechanism (2013, background): “In contrast, Cuzzi & Zahnle (2004) considered inwards materi l drift across the ice line, which would enhance the vapour density in the inner disc, followed by a phase of accumulation of solids by condensation onto immobile planetesimals formed outside of the ice line.”
Towards initial mass functions for asteroids and Kuiper Belt Objects (2010, background): “This will cause large amounts of mass to migrate from the outer Solar System to the inner Solar System much faster than the gas evolves, elevating the relative abundance of solids significantly (Stepinski and Valageas, 1996, 1997; Cuzzi and Zahnle, 2004; Ciesla and Cuzzi, 2006; Kornet et al., 2001).”
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).”
Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water (2014, background): “Inside the snow line, water ice sublimes, thus adding H2O to the vapor phase (Cuzzi and Zahnle, 2004).”
RINGED SUBSTRUCTURE AND A GAP AT 1 au IN THE NEAREST PROTOPLANETARY DISK (2016, background): “This and any subsequent re-condensation can modify the solid opacities, and thereby the associated continuum emission (e.g., Cuzzi & Zahnle 2004).”
Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, background): “…ice when crossing the condensation fronts, causing a higher dust-to-gas ratio just outside the ice line, and the evaporated gas may diffuse outward and recondense onto dust outside the ice line, both leading to enhanced grain growth beyond the ice line (Cuzzi & Zahnle 2004; Stammler et al. 2017).”
Redox Conditions in the Solar Nebula: Observational, Experimental, and Theoretical Constraints (2008, background): “While Cuzzi and Zahnle (2004) suggested that enhancements of 100 to 1000 are possible, that work considered only a steady-state case.”
Planet Formation around Stars of Various Masses: The Snow Line and the Frequency of Giant Planets (2007, background): “Models that relax the assumption of a smooth radial profile find an enhanced surface density near the snow line (e.g. Cuzzi & Zahnle 2004; Ciesla & Cuzzi 2006).”
The evolution of the water distribution in a viscous protoplanetary disk (2005, background): “Cuzzi and Zahnle (2004) argued that until planetesimals grow outside the snow line, bodies from the outer nebula will continuously migrate into the inner nebula and vaporize, enriching the gas with water and suggest that this could explain the presence of oxidized species in primitive meteorites.”
Planetesimal formation near the snowline: in or out? (2017, background): “Works that have investigated the role of water diffusion and condensation on the growth and distribution of solids include Stevenson & Lunine (1988), Cuzzi & Zahnle (2004), Ciesla & Cuzzi (2006), Ros & Johansen (2013), Estrada et al. (2016), Armitage et al. (2016) and, recently, Krijt et al.…”
Grain Retention and Formation of Planetesimals near the Snow Line in MRI-driven Turbulent Protoplanetary Disks (2007, background): “Efficient inward transport of solid materials combined with the slow diffusion of the heavy elemental vapor can further enhance the contrast in grains’ surface density (Cuzzi & Zahnle 2004).”
Planetesimal formation starts at the snow line (2017, background): “It was also proposed that the icy dust aggregates can pileup (Cuzzi & Zahnle 2004) or even significantly grow thanks to water vapor recondensation at the snow line (Ros & Johansen Article number, page 1 of 11 ar X iv :1 71 0.”