English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We model particle growth in a turbulent, viscously evolving protoplanetarynebula, incorporating sticking, bouncing, fragmentation, and mass transfer athigh speeds. We treat small particles using a moments method and largeparticles using a traditional histogram binning, including a probabilitydistribution function of collisional velocities. The fragmentation strength ofthe particles depends on their composition (icy aggregates are stronger thansilicate aggregates). The particle opacity, which controls the nebula thermalstructure, evolves as particles grow and mass redistributes. While growing,particles drift radially due to nebula headwind drag. Particles of differentcompositions evaporate at "evaporation fronts" (EFs) where the midplanetemperature exceeds their respective evaporation temperatures. We track thevapor and solid phases of each component, accounting for advection and radialand vertical diffusion. We present characteristic results in evolutions lasting$2 \times 10^5$ years. In general, (a) mass is transferred from the outer toinner nebula in significant amounts, creating radial concentrations of solidsat EFs, (b) particle sizes are limited by a combination of fragmentation,bouncing, and drift, (c) "lucky" large particles never represent a significantamount of mass, and (d) restricted radial zones just outside each EF becomecompositionally enriched in the associated volatiles. We point out implicationsfor mm-submm SEDs and inference of nebula mass, radial banding, the role ofopacity on new mechanisms for generating turbulence, enrichment of meteoritesin heavy oxygen isotopes, variable and nonsolar redox conditions, primaryaccretion of silicate and icy planetesimals, and the makeup of Jupiter's core.

Global Modeling of Nebulae with Particle Growth, Drift and Evaporation Fronts. I: Methodology and Typical Results