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

Context: Planets in accretion disks can excite spiral shocks, and---ifmassive enough---open gaps in their vicinity. Both of these effects caninfluence the overall disk thermal structure.  Aims: We model planets of different masses and semimajor axes in disks ofvarious viscosities and accretion rates to examine their impact on diskthermodynamics and highlight the mutable, non-axisymmetric nature of icelinesin systems with massive planets.  Methods: We conduct a parameter study using numerical hydrodynamicssimulations where we treat viscous heating, thermal cooling and stellarirradiation as additional source terms in the energy equation, with some runsincluding radiative diffusion. Our parameter space consists of a gridcontaining different combinations of planet and disk parameters.  Results: Both gap opening and shock heating can displace the iceline, withthe effects being amplified for massive planets in optically thick disks. Thegap region can split an initially hot (T>170 K) disk into a hot inner disk anda hot ring just outside of the planet's location, while shock heating canreshape the originally axisymmetric iceline into water-poor islands alongspirals. We also find that radiative diffusion does not alter the picturesignificantly in this context.  Conclusions: Shock heating and gap opening by a planet can effectively heatup optically thick disks and in general move and/or reshape the water iceline.This can affect the gap structure and migration torques. It can also produceazimuthal features that follow the trajectory of spiral arms, creating hotzones, "islands" of vapor and ice around spirals which could affect theaccretion or growth of icy aggregates.

The impact of planet wakes on the location and shape of the water iceline in a protoplanetary disk