# Synergies between Asteroseismology and Three-dimensional Simulations of Stellar Turbulence

## TL;DR

This paper compares asteroseismically inferred stellar interior structures with predictions from 3D turbulence simulations to improve understanding of stellar convection and reduce reliance on adjustable parameters in traditional models.

## Contribution

It demonstrates promising agreement between 3D turbulence simulation predictions and asteroseismic observations of B stars, advancing the integration of simulations into stellar modeling.

## Key findings

- Good match between simulation and asteroseismic composition profiles
- Insights into boundary layer structure and wave generation
- Potential to improve stellar evolution models

## Abstract

Turbulent mixing of chemical elements by convection has fundamental effects on the evolution of stars. The standard algorithm at present, mixing-length theory (MLT), is intrinsically local, and must be supplemented by extensions with adjustable parameters. As a step toward reducing this arbitrariness, we compare asteroseismically inferred internal structures of two Kepler slowly pulsating B stars (SPB's; $M\sim 3.25 M_\odot$) to predictions of 321D turbulence theory, based upon well-resolved, truly turbulent three-dimensional simulations (Arnett , et al. 2015, Christini, et al. 2016) which include boundary physics absent from MLT. We find promising agreement between the steepness and shapes of the theoretically-predicted composition profile outside the convective region in 3D simulations and in asteroseismically constrained composition profiles in the best 1D models of the two SPBs. The structure and motion of the boundary layer, and the generation of waves, are discussed.