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/

Zendy Plus

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

Zendy Tools

Zendy Open

We investigate formation mechanisms for icy super-Earth mass planets orbitingat 2-20 AU around 0.1-0.5 solar mass stars. A large ensemble of coagulationcalculations demonstrates a new formation channel: disks composed of largeplanetesimals with radii of 30-300 km form super-Earths on time scales ofroughly 1 Gyr. In other gas-poor disks, a collisional cascade grindsplanetesimals to dust before the largest planets reach super-Earth masses. Onceicy Earth-mass planets form, they migrate through the leftover swarm ofplanetesimals at rates of 0.01-1 AU per Myr. On time scales of 10 Myr to 1 Gyr,many of these planets migrate through the disk of leftover planetesimals fromsemimajor axes of 5-10 AU to 1-2 AU. A few per cent of super-Earths mightmigrate to semimajor axes of 0.1-0.2 AU. When the disk has an initial masscomparable with the minimum mass solar nebula scaled to the mass of the centralstar, the predicted frequency of super-Earths matches the observed frequency.

Coagulation Calculations of Icy Planet Formation Around 0.1--0.5~\msun\ Stars: Super-Earths From Large Planetestimals