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

Recent 3D-simulations have shown that the turbulent kinetic flux (TKF) issignificant. We discuss the effects of TKF on the size of convection zone andfind that the TKF may help to solve the solar abundance problem. The solarabundance problem is that, with new abundances, the solar convection zonedepth, sound speed in the radiative interior, the helium abundance and densityin the convective envelope are not in agreement with helioseismic inversions.We have done Monte Carlo simulations on solar convective envelope models withdifferent profile of TKF to test the effects. The solar abundance problem isrevealed in the standard solar convective envelope model with AGSS09composition, which shows significant differences ($\rm{\sim 10 %}$) on densityfrom the helioseicmic inversions, but the differences in the model with oldcomposition GN93 is small ($\rm{\sim 0.5 %}$). In the testing models withdifferent imposed TKF, it is found that the density profile is sensitive to thevalue of TKF at the base of convective envelope and insensitive to thestructure of TKF in the convection zone. Required value of turbulent kineticluminosity at the base is about $\rm{-13%\sim-19%L_{\odot}}$. Comparing withthe 3D-simulations, this value is plausible. This study is for the solarconvective envelope only. The evolutionary solar models with TKF are requiredfor investigating its effects on the solar interior structure below theconvection zone and the whole solar abundance problem, but the profile of TKFin the overshoot region is needed.

The solar abundance problem: the effect of the turbulent kinetic flux on the solar envelope model