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

Spatial distribution and growth of dust in a clumpy protoplanetary disksubject to vigorous gravitational instability and fragmentation is studiednumerically with sub-au resolution using the FEOSAD code. Hydrodynamicsequations describing the evolution of self-gravitating and viscousprotoplanetary disks in the thin-disk limit were modified to include a dustcomponent consisting of two parts: sub-micron-sized dust and grown dust with avariable maximum radius. The conversion of small to grown dust, dust growth,friction of dust with gas, and dust self-gravity were also considered. We foundthat the disk appearance is notably time-variable with spiral arms, dustyrings, and clumps, constantly forming, evolving, and decaying. As aconsequence, the total dust-to-gas mass ratio is highly non-homogeneousthroughout the disk extent, showing order-of-magnitude local deviations fromthe canonical 1:100 value. Gravitationally bound clumps formed throughgravitational fragmentation have a velocity pattern that deviates notably fromthe Keplerian rotation. Small dust is efficiently converted into grown dust inthe clump interiors, reaching a maximum radius of several decimeters.Concurrently, grown dust drifts towards the clump center forming a massivecompact central condensation (70-100 $M_\oplus$). We argue that protoplanetsmay form in the interiors of inward migrating clumps before they dispersethrough the action of tidal torques. We foresee the formation of protoplanetsat orbital distances of several tens of au with initial masses of gas and dustin the protoplanetary seed in the (0.25-1.6) $M_{\rm Jup}$ and (1.0-5.5)$M_\oplus$ limits, respectively. The final masses of gas and dust in theprotoplanets may however be much higher due to accretion from surroundingmassive metal-rich disks/envelopes.

Gravitoviscous protoplanetary disks with a dust component. II. Spatial distribution and growth of dust in a clumpy disk