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 describe comprehensive calculations of the formation of icy planets anddebris disks at 30-150 AU around 1-3 solar mass stars. Disks composed of large,strong planetesimals produce more massive planets than disks composed of small,weak planetesimals. The maximum radius of icy planets ranges from roughly 1500km to 11,500 km. The formation rate of 1000 km objects - `Plutos' - is a usefulproxy for the efficiency of icy planet formation. Plutos form more efficientlyin massive disks, in disks with small planetesimals, and in disks with a rangeof planetesimal sizes. Although Plutos form throughout massive disks, Plutoproduction is usually concentrated in the inner disk. Despite the large numberof Plutos produced in many calculations, icy planet formation is inefficient.At the end of the main sequence lifetime of the central star, Plutos containless than 10% of the initial mass in solid material. This conclusion isindependent of the initial mass in the disk or the properties of planetesimals.Debris disk formation coincides with the formation of planetary systemscontaining Plutos. As Plutos form, they stir leftover planetesimals to largevelocities. A cascade of collisions then grinds the leftovers to dust, formingan observable debris disk. In disks with small (< 1-10 km) planetesimals,collisional cascades produce luminous debris disks with maximum luminosityroughly 0.01 times the stellar luminosity. Disks with larger planetesimalsproduce much less luminous debris disks. Observations of debris disks aroundA-type and G-type stars strongly favor models with small planetesimals. Inthese models, our predictions for the time evolution and detection frequency ofdebris disks agree with published observations. We suggest several criticalobservations that can test key features of our calculations.

Variations on Debris Disks II. Icy Planet Formation as a Function of the Bulk Properties and Initial Sizes of Planetesimals