The Stagger-grid: A Grid of 3D Stellar Atmosphere Models - II. Horizontal and Temporal Averaging and Spectral Line Formation

TL;DR

This paper investigates how different averaging methods of 3D stellar atmosphere models affect spectral line formation, revealing that certain averaging techniques better represent LTE spectral lines, especially in the upper atmosphere.

Contribution

It systematically compares various averaging methods of 3D stellar atmospheres and assesses their impact on LTE spectral line formation, providing guidance for model simplification.

Findings

Averages over constant column-mass density best represent LTE line formation.

Averages over geometrical height are less appropriate for spectral line modeling.

Optical depth-based averages are affected by reversed granulation at higher temperatures.

Abstract

We study the implications of averaging methods with different reference depth scales for 3D hydrodynamical model atmospheres computed with the Stagger-code. The temporally and spatially averaged (hereafter denoted as <3D>) models are explored in the light of local thermodynamic equilibrium (LTE) spectral line formation by comparing spectrum calculations using full 3D atmosphere structures with those from <3D> averages. We explore methods for computing mean <3D> stratifications from the Stagger-grid time-dependent 3D radiative hydro- dynamical atmosphere models by considering four different reference depth scales (geometrical depth, column-mass density, and two optical depth scales). Furthermore, we investigate the influence of alternative averages (logarithmic or enforced hydrostatic equilibrium, flux-weighted temperatures). For the line formation we compute curves of growth for Fe i and Fe ii lines in LTE . The resulting <3D> stratifications for the four reference depth scales can be considerably different. We find typically that in the upper atmosphere and in the superadiabatic region just below the optical surface, where the temperature and density fluctuations are highest, the differences become considerable and increase for higher Teff, lower logg, and lower [Fe/H]. The differential comparison of spectral line formation shows distinctive differences depending on which <3D> model is applied. The averages over layers of constant column-mass density yield the best mean <3D> representation for LTE line formation, while the averages on layers at constant geometrical height are the least appropriate. Unexpectedly, the usually preferred averages over layers of constant optical depth are prone to the increasing interference of the reversed granulation towards higher effective temperature, in particular at low metallicity.