On line contribution functions and examining spectral line formation in 3D model stellar atmospheres
Anish Mayur Amarsi
TL;DR
This paper derives a new expression for line contribution functions in 3D stellar atmospheres and compares LTE and non-LTE spectral line formation, enhancing understanding of spectral diagnostics.
Contribution
It introduces an expression for the contribution function to flux depression in 3D stellar models, advancing spectral line formation analysis.
Findings
Derived an expression for the contribution function in 3D models
Compared LTE and non-LTE formation of OI777nm lines
Highlighted differences in spectral line formation mechanisms
Abstract
Line contribution functions are useful diagnostics for studying spectral line formation in stellar atmospheres. I derive an expression for the contribution function to the abso- lute flux depression that emerges from three-dimensional box-in-a-star model stellar atmospheres. I illustrate the result by comparing the local thermodynamic equilibrium (LTE) spectral line formation of the high-excitation permitted OI777nm lines with the non-LTE case.
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