Numerical simulation of excitation of solar oscillation modes for different turbulent models

TL;DR

This study uses numerical simulations with various turbulence models to understand their impact on solar oscillation modes, finding that the dynamic model aligns best with observations.

Contribution

It compares different LES turbulence models in simulating solar oscillation excitation, identifying the most accurate model for helioseismic properties.

Findings

Dynamic turbulence model best matches helioseismic data.

Different turbulence models significantly affect oscillation excitation.

Simulation results agree with observed solar oscillation spectra.

Abstract

The goal of this research is to investigate how well various turbulence models can describe physical properties of the upper convective boundary layer of the Sun. An accurate modeling of the turbulence motions is necessary for understanding the excitation mechanisms of solar oscillation modes. We have carried out realistic numerical simulations using several different physical Large Eddy Simulation (LES) models (Hyperviscosity approach, Smagorinsky, and dynamic models) to investigate how the differences in turbulence modeling affect the damping and excitation of the oscillations and their spectral properties and compare with observations. We have first calculated the oscillation power spectra of radial and non-radial modes supported by the computational box with the different turbulence models. Then we have calculated the work integral input to the modes to estimate the influence of the turbulence model on the depth and strength of the oscillation sources. We have compared these results with previous studies and with the observed properties of solar oscillations. We find that the dynamic turbulence model provides the best agreement with the helioseismic observations.