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

After 25 years of laboratory research on protoplanetary dust agglomeration, aconsistent picture of the various processes that involve colliding dustaggregates has emerged. Besides sticking, bouncing and fragmentation, othereffects, like, e.g., erosion or mass transfer, have now been extensivelystudied. Coagulation simulations consistently show that $\rm \mu$m-sized dustgrains can grow to mm- to cm-sized aggregates before they encounter thebouncing barrier, whereas sub-$\rm \mu$m-sized water-ice particles can directlygrow to planetesimal sizes. For siliceous materials, other processes have to beresponsible for turning the dust aggregates into planetesimals. In thisarticle, these processes are discussed, the physical properties of the emergingdusty or icy planetesimals are presented and compared to empirical evidencefrom within and without the Solar System. In conclusion, the formation ofplanetesimals by a gravitational collapse of dust "pebbles" seems the mostlikely.

Dust evolution in protoplanetary discs and the formation of planetesimals. What have we learned from laboratory experiments?