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

Jupiter's atmosphere has been observed to be depleted in helium (Yatm~0.24),suggesting active helium sedimentation in the interior. This is accounted forin standard Jupiter structure and evolution models through the assumption of anouter, He-depleted envelope that is separated from the He-enriched deepinterior by a sharp boundary. Here we aim to develop a model for Jupiter'sinhomogeneous thermal evolution that relies on a more self-consistentdescription of the internal profiles of He abundance, temperature, and heatflux. We make use of recent numerical simulations on H/He demixing, and onlayered (LDD) and oscillatory (ODD) double diffusive convection, and assume anidealized planet model composed of a H/He envelope and a massive core. Ageneral framework for the construction of interior models with He rain isdescribed. Despite, or perhaps because of, our simplifications made we findthat self-consistent models are rare. For instance, no model for ODD convectionis found. We modify the H/He phase diagram of Lorenzen et al. to reproduceJupiter's atmospheric helium abundance and examine evolution models as afunction of the LDD layer height, from those that prolong Jupiter's coolingtime to those that actually shorten it. Resulting models that meet theluminosity constraint have layer heights of about 0.1-1 km, corresponding to~10,-20,000 layers in the rain zone between ~1 and 3-4.5 Mbars. Presentlimitations and directions for future work are discussed, such as the formationand sinking of He droplets.

An Exploration of Double Diffusive Convection in Jupiter as a Result of Hydrogen-Helium Phase Separation