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

A massive planet in a protoplanetary disc will open a gap in the discmaterial. A steep gap edge can be hydrodynamically unstable, which results inthe formation of vortices that can act as tracers for the presence of planetsin observational results. However, in a viscous disc, the potential formationof these vortices is dependent on the timescale over which the massive planetaccretes mass and with a sufficiently long timescale it is possible for novortices to form. Hence, there is a connection between the presence of vorticesand the growth timescale of the planet and it may therefore be possible toexclude a planetary interpretation of observed structure from the absence ofvortices. We have investigated the effect of the planet growth timescale onvortex formation for a range of planet masses and viscosities and have found anapproximate relation between the planet mass, viscosity and planet growthtimescale for which vortices are not formed within the disc. We then interpretthese results in the light of recent observations. We have also found thatplanets do not need to be close to a Jupiter mass to form vortices in the discif these discs have low viscosity, as these can be caused by planets as smallas a few Neptune masses.

Constraining the masses of planets in protoplanetary discs from the presence or absence of vortices -- Comparison with ALMA observations