Revisiting turbulent properties of solar convection with 3D radiative hydrodynamic modeling

TL;DR

This study uses 3D radiative hydrodynamic simulations to explore the complex turbulent structures and dynamics of the solar convection zone, revealing depth-dependent variations in turbulent scales and flow patterns.

Contribution

It introduces a detailed 3D simulation approach that uncovers new insights into the turbulent properties and scale variations in the solar convection zone.

Findings

Characteristic convective scale increases with depth up to 7 Mm.

Turbulent flows become weaker and more homogeneous near the bottom of the hydrogen ionization zone.

Turbulent spectra indicate a change in convective patterns below 7 Mm.

Abstract

We discuss the turbulent structure and dynamics of the upper solar convection zone using a 3D radiative hydrodynamic simulation model at 45 degrees latitude. The model reveals the self-formation of meridional flows, the leptocline, and the radial differential rotation. Unlike previous studies, the model shows a complex variation of the characteristic scales of turbulent flows with depth. In particular, an increase in the characteristic convective scale is trackable within an individual snapshot up to a depth of 7 Mm, near the bottom of the hydrogen ionization zone, where turbulent flows become weaker and more homogeneous. However, the turbulent spectra show an increase in scale with depth and a qualitative change in convective patterns below 7 Mm (near the bottom of the leptocline), suggesting changes in the diffusivity properties and energy exchange among different scales.