Amplitudes of solar p modes: modelling of the eddy time-correlation function

TL;DR

This paper explores the modeling of solar p mode amplitudes by analyzing the eddy time-correlation function, combining theoretical developments with observational data to better understand stellar convection zones.

Contribution

It introduces a new approach using the Ornstein-Uhlenbeck process to model eddy time correlations in stellar convection, linking theory with observations.

Findings

Eddy time-correlation functions can be effectively modeled with the Ornstein-Uhlenbeck process.

Recent observational data support the theoretical models of eddy correlations.

The approach enhances understanding of turbulent convection in stars.

Abstract

Modelling amplitudes of stochastically excited oscillations in stars is a powerful tool for understanding the properties of the convective zones. For instance, it gives us information on the way turbulent eddies are temporally correlated in a very large Reynolds number regime. We discuss the way the time correlation between eddies is modelled and we present recent theoretical developments as well as observational results. Eventually, we discuss the physical underlying meaning of the results by introducing the Ornstein-Uhlenbeck process, which is a sub-class of a Gaussian Markov process.