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

In the general classical picture of pebble-based core growth, planetary coresgrow by accretion of single pebble species. The growing planet may reach theso-called pebble isolation mass, at which it induces a pressure bump thatblocks inward drifting pebbles exterior to its orbit, thereby stalling coregrowth by pebble accretion. In recent hydrodynamic simulations, pebblefiltration by the pressure bump depends on several parameters including coremass, disc structure, turbulent viscosity and pebble size. We investigated howaccretion of multiple, instead of single, pebble species affects core growthrates, and how the dependence of pebble isolation mass on turbulent viscosityand pebble size sets the final core masses. We performed numerical simulationsin viscous 1D disc, where maximal grain sizes were regulated by grain growth,fragmentation and drift limits. We confirm that core growth rates and finalcore masses are sensitive to three key parameters: threshold velocity at whichpebbles fragment on collision, turbulent viscosity and distribution of pebblespecies, which yield a diversity of planetary cores. With accretion of multiplepebble species, planetary cores can grow pretty fast, reaching over 30 -- 40$M_{\rm{E}}$ in mass. Potential cores of cold gas giants were able to form fromembryos initially implanted as far as 50 AU. Our results suggest that accretionof multi-species pebbles could explain: the estimated 25 -- 45 $M_{\rm{E}}$heavy elements abundance inside Jupiter's core; massive cores of extrasolarplanets; disc rings and gaps at wider orbits; early and rapid formation ofplanetary bodies.

Planetary core formation via multi-species pebble accretion