The evolution of the water distribution in a viscous protoplanetary disk

By F. Ciesla, J. Cuzzi. 2005

304 citations recorded by the source corpus.

Astronomical observations have shown that protoplanetary disks are dynamic objects through which mass is transported and accreted by the central star. This transport causes the disks to decrease in mass and cool over time, and such evolution is expected to have occurred in our own solar nebula. Age dating of meteorite constituents shows that their creation, evolution, and accumulation occupied several Myr, and over this time disk properties would evolve significantly. Moreover, on this timescale, solid particles decouple from the gas in the disk and their evolution follows a different path. It is in this context that we must understand how our own solar nebula evolved and what effects this evolution had on the primitive materials contained within it. Here we present a model which tracks how the distribution of water changes in an evolving disk as the water-bearing species experience condensation, accretion, transport, collisional destruction, and vaporization. Because solids are transported in a disk at different rates depending on their sizes, the motions will lead to water being concentrated in some regions of a disk and depleted in others. These enhancements and depletions are consistent with the conditions needed to explain some aspects of the chemistry of chondritic meteorites and formation of giant planets. The levels of concentration and depletion, as well as their locations, depend strongly on the combined effects of the gaseous disk evolution, the formation of rapidly migrating rubble, and the growth of immobile planetesimals. Understanding how these processes operate simultaneously is critical to developing our models for meteorite parent body formation in the Solar System and giant planet formation throughout the galaxy. We present examples of evolution under a range of plausible assumptions and demonstrate how the chemical evolution of the inner region of a protoplanetary disk is intimately connected to the physical processes which occur in the outer regions.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0772d95dfde4bf66c7f85d4479e5481ef1af9bed

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Citations in the corpus

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”
Planetesimal formation starts at the snow line (2017, methodology): “We take water ice evaporation and recondensation of water vapor into account following the treatment proposed by Ciesla & Cuzzi (2006).”
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).”
Towards initial mass functions for asteroids and Kuiper Belt Objects (2010, unknown): “Here we provide some notational clarifications to better connect the distribution functions P (Φ, S) and Fp(Φ, S) of this paper to similar functions in CHPD01 and Hogan and Cuzzi(2007). We first note that we have defined P (Φ, S) in this paper as a probability per unit log10(Φ) and log10(S) (as in C”
Planetesimal formation near the snowline: in or out? (2017, methodology): “…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. (2016a), which focuses on the…”
Populating the asteroid belt from two parent source regions due to the migration of giant planets—“The Grand Tack” (2012, background): “As the actual formation location of Jupiter is unknown, it is tested at a range of values, but nominally set at 3.5 AU due to estimates of the snow line location (Ciesla and Cuzzi 2006; Lecar et al. 2006; Garaud and Lin 2007).”
Building Terrestrial Planets (2012, background): “…2 and 4 AU, the low temperatures allow water ice to condense, enhancing the surface density of solid material and drastically increasing the typical embryo mass to perhaps an Earth mass or more (e.g., Ciesla & Cuzzi 2006, Dodson-Robinson et al. 2009, Kokubo & Ida 2002, Stevenson & Lunine 1988).”
The Effect of Internal Dissipation and Surface Irradiation on the Structure of Disks and the Location of the Snow Line around Sun-like Stars (2006, background): “…(“pebbles” to “boulders”) have a different intrinsic motion which is sensitively dependent on the structure (temperature, pressure gradient) and dynamical nature (tubulent versus laminar) of the nebular gas (Morfill & Voelk 1984, Supulver & Lin 2000, Youdin & Chiang, 2004, Ciesla & Cuzzi 2006).”
Chemical enrichment of giant planets and discs due to pebble drift (2017, background): “This idea has been explored in relation to the water snow line or generic volatiles (Stepinski & Valageas 1997; Hueso & Guillot 2003; Ciesla & Cuzzi 2006; Garaud 2007); however, increasing the abundance of water inside the water snow line is clearly of little help in enhancing the C/O ratio.”
Spectroastrometric Imaging of Molecular Gas within Protoplanetary Disk Gaps (2008, background): “Further, gaps in the radial gas distribution will block the inwards migration of particles rich in volatiles, strongly affecting the chemistry of the inner disk (Ciesla & Cuzzi 2006).”
Protoplanetary Disks and Their Evolution (2011, background): “The complex origin of the gas-phase water and its implications for understanding disk structure and evolution have been recently discussed by Meijerink et al. (2009) and Ciesla & Cuzzi (2006).”
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).”
Toward Planetesimals: Dense Chondrule Clumps in the Protoplanetary Nebula (2008, background): “Models suggest that the density, temperature, and composition of the nebula evolved significantly over several million years (Bell et al 1995, D’Alessio et al. 2005, Ciesla and Cuzzi 2006).”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “The existence of ice at the snow line depends on inward drift of small particles (Ciesla and Cuzzi, 2006), which may be blocked by an outer, ice giant-mass object (Lambrechts et al.”
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).”
Water and astrobiology (2007, background): “Likewise, freezeout of icy grains in the disk can influence the transport of energy, mass, and angular momentum in the disk (Pollack et al., 1994; Ciesla and Cuzzi, 2006).”
H2O and OH Gas in the Terrestrial Planet-forming Zones of Protoplanetary Disks (2008, background): “With both solid migration and diffusion controlling water transport, water vapor concentrations become sensitive to an array of parameters, including disk viscosity and planetesimal growth rates, and water concentrations may trace disk evolution (Ciesla & Cuzzi 2006).”