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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Tidal interactions between the embedded planets and their surroundingprotoplanetary disks are often postulated to produce the observed complex dustsubstructures, including rings, gaps, and asymmetries. In this Letter, weexplore the consequences of dust coagulation on the dust dynamics and ringmorphology. Coagulation of dust grains leads to dust size growth which, undertypical disk conditions, produces faster radial drifts, potentially threateningthe dust ring formation. Utilizing 2D hydrodynamical simulations ofprotoplanetary disks which include a full treatment of dust coagulation, wefind that if the planet does not open a gap quickly enough, the formation of aninner ring is impeded due to dust coagulation and subsequent radial drift.Furthermore, we find that a "buildup" of sub-mm sized grains often appears inthe dust emission at the outer edge of the dust disk.

Ring Morphology with Dust Coagulation in Protoplanetary Disks