Formation of activity indicators in 3D model atmosphere
Background
Several spectral lines have been used as activity indicators for stars. How these are formed and what influences the variation over the surface is less known.
Goal
The goal of the project is to study the formation of spectral lines in several 3D models.
Method
The RH 1.5D code is used to solve the equations of statistical equilibrium for a given model atom and model atmosphere.
Procedure
- Find appropriate spectral lines to study through searching through the litterature, e.g. Frasca et al 2010
- Make model atoms for these spectral lines
- Calculate the spectral profile as function of (x,y) position of the model atmosphere, using RH
- Study the mean spectrum and the variation. Look at how the line is formed.
3D models are in the process of being generated so links will be provided.