Size-selective Concentration of Chondrules and Other Small Particles in Protoplanetary Nebula Turbulence

By J. Cuzzi, R. Hogan, J. Paque, A. Dobrovolskis. 2000

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Size-selective concentration of particles in a weakly turbulent protoplanetary nebula may be responsible for the initial collection of chondrules and other constituents into primitive body precursors. This paper presents the main elements of this process of turbulent concentration. In the terrestrial planet region, both the characteristic size and size distribution of chondrules are explained. "Fluffier" particles would be concentrated in nebula regions that were at a lower gas density and/or more intensely turbulent. The spatial distribution of concentrated particle density obeys multifractal scaling, suggesting a close tie to the turbulent cascade process. This scaling behavior allows predictions of the probability distributions for concentration in the protoplanetary nebula to be made. Large concentration factors (>105) are readily obtained, implying that numerous zones of particle density significantly exceeding the gas density could exist. If most of the available solids were actually in chondrule-sized particles, the ensuing particle mass density would become so large that the feedback effects on gas turbulence due to mass loading could no longer be neglected. This paper describes the process, presenting its basic elements and some implications, without including the effects of mass loading.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e058c944bbc070964511cf094b446a1f1bcd704a

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Citations in the corpus

Planetary accretion in the inner Solar System (2004, background): “These solid-rich regions could evolve rapidly into planetesimals [ 53 ].”
Planetesimal Formation by Gravitational Instability (2002, background): “Extrapolation to the high Reynolds numbers of protoplanetary disks implies concentration of chondrules by factors of up to 105 (Cuzzi et al. 2001).”
Material Enhancement in Protoplanetary Nebulae by Particle Drift through Evaporation Fronts (2004, background): “However, turbulence can exist, providing 490 diffusivity, without necessarily providing the viscosity needed to evolve the disk (Prinn 1990; Cuzzi et al. 2001).”
Fossilized condensation lines in the Solar System protoplanetary disk (2015, background): “Also, small particles are not collected in vortices, but rather accumulate in the low-vorticity regions at the dissipation scale of the turbulent cascade (Cuzzi et al., 2001).”
Planetesimal formation by sweep-up: how the bouncing barrier can be beneficial to growth (2012, background): “…assume that the relative velocity is caused onlyby turbulence, and can therefore for small particles be estimated by (Weidenschilling & Cuzzi 1993; Cuzzi et al. 2001) ∆v = √ 9 2 αSt · cs (34) whereα = 10−3 is the turbulence parameter, St the Stokes number for the boulder given by Eq.25andcs the…”
Chondrule size and related physical properties: a compilation and evaluation of current data across all meteorite groups (2014, methodology): “Cuzzi et al. (1999) mentioned that the work was based on 235 chondrules. The measurements were made by disaggregation and masses (and densities) were also measured. Cuzzi et al. (2001) give a graphical distribution of the Stokes number for this set of chondrules. Teitler et al. (2010) expanded on th”
Measuring turbulence in TW Hydrae with ALMA: methods and limitations (2016, background): “A comparison with the α viscosity models is more complex, as the relation between vturb and α depends on the nature of the viscosity, with vturb ranging between a few αcs and √ αcs (Cuzzi et al. 2001).”
Astrophysics with Extraterrestrial Materials (2016, background): “…(b) gravitational instability models where solids become spatially concentrated in the nebula through dynamical interactions with the gas to levels where they become gravitationally bound and contract to form a coherent body (Goldreich & Ward 1973; Cuzzi et al. 2001, 2008; Johansen et al. 2007).”
Blowing in the wind: I. Velocities of chondrule-sized particles in a turbulent protoplanetary nebula (2003, methodology): “where we have substituted Vg = ca 1/2 (Cuzzi et al. 2001).”
FORMATION OF KUIPER BELT BINARIES BY GRAVITATIONAL COLLAPSE (2010, background): “However, particles can also clump in a turbulent flow (e.g., Cuzzi et al. 2001, 2008; Johansen et al. 2006).”
Planet formation and migration (2005, background): “But note that Cuzzi et al. (2001) make the point that dust density enhancement may only be significant for a narrow particle size range.”
A simple model for the evolution of the dust population in protoplanetary disks (2012, background): “…= tstop tL , (1) which under typical assumptions (Epstein drag law, compact spherical particles, isothermal gas density profile, and tL = Ω−1k , see Cuzzi et al. 2001) simplifies for particles near the disk midplane to St = a ρs Σg π 2 · (2) Here a is the radius and ρs the internal density of…”
Forming Planetesimals in Solar and Extrasolar Nebulae (2009, neutral): “By ignoring the difference between the turbulent diffusivity for mass, Dg ∼ δvoℓo ∼ δv2oto, with the turbulent diffusivity for angular momentum, αcghg ∼ αc2gΩ−1K , we extract the convenient prescriptions δvo ∼ √ αcg and ℓo ∼ √ αhg (Cuzzi et al. 2001, see also Youdin & Chiang 2004).”
Radial Flow of Dust Particles in Accretion Disks (2002, background): “Several studies showed that vortices or turbulent eddies can trap particles within some size range (Barge & Sommeria 1995; Cuzzi, Dobrovolskis, & Hogan 1996; Tanga et al. 1996; Klahr & Henning 1997; Cuzzi et al. 2001, see however Hodgson & Brandenburg 1998).”