Formation of the Mg II h&k lines in various solar features
Background
The h and k lines from Mg II are prime diagnostics of the Solar upper chromosphere and prime observables from the IRIS satellite. Their formation has been studied through the use of a Bifrost model of enhanced network in two papers in the series "Formation of IRIS Diagnostics":The Formation of IRIS Diagnostics. I. A Quintessential Model Atom of Mg II and General Formation Properties of the Mg II h&k Lines
The Formation of IRIS Diagnostics. II. The Formation of the Mg II h&k Lines in the Solar Atmosphere
Goal
To study the formation of the Mg II h & k lines in a Bifrost model of a coronal hole region.Method
RH is used to solve the equations of statistical equilibrium for a given model atom and model atmosphere. The 1.5D version is to be used.Procedure
Choose a snapshot from a Bifrost model of a coronal hole region. Make an input atmosphere in RH format from the original Bifrost format. Choose some characteristic features (network, internetwork, etc) and calculate the Mg II h & k lines using RH for these columns. The Bifrost files are in the directory /mn/stornext/d9/matsc/3d/run/ch012012_hion Don't copy over the files (they are very large) but make symbolic links into a directory where you work.Last modified: Sun Feb 14 18:58:50 CET 2021