Modelling convection in A star atmospheres. Bisectors and lineshapes of HD108642

TL;DR

This paper introduces VeDyn, a fast and practical code for modeling convection in A to F star atmospheres, accurately reproducing observed line bisectors by integrating advanced convection models with spectral synthesis.

Contribution

The paper develops and tests VeDyn, a new tool combining sophisticated convection modeling with spectral synthesis, enabling realistic simulations of stellar atmospheres efficiently.

Findings

Synthetic line bisectors match observed blue-bending in HD108642

VeDyn effectively models convective velocity structures in stellar atmospheres

The approach is computationally efficient for practical applications

Abstract

We present a code, VeDyn, for modelling envelopes and atmospheres of A to F stars focusing on accurate treatment of convective processes. VeDyn implements the highly sophisticated convection model of Canuto and Dubovikov (1998) but is fast and handy enough to be used in practical astrophysical applications. We developed the HME envelope solver for this convection model furtheron to consistently model the envelope together with the stellar atmosphere. The synthesis code SynthV was extended to account for the resulting velocity structure. Finally, we tested our approach on atomic line bisectors. It is shown that our synthetic line bisectors of HD108642 bend towards the blue and are of a magnitude comparable to the observed ones. Even though this approach of modelling convection requires the solution of a coupled system of nonlinear differential equations, it is fast enough to be applicable to many of the investigation techniques relying on model atmospheres.