Diagnostics of Ellerman Bombs

Background

The solar atmosphere is repleat with energetic phenomena that have characteristic observational signatures. Among them are Ellerman Bombs (Ellerman 1917) that are first and foremost recognized by strong emission in the wings of H-alpha, with little or no visible signal in the line core, indicating that the EB is formed at photospheric or upper photospheric heights, at most some few hundred km above the photosphere.

Goal

The primary goal of the project is to study how typical diagnostic lines available with the Swedish 1-m Solar Telescope (SST) and the Interface Region Imaging Spectrograph (IRIS) respond to Ellerman Bombs

Method

Synthesize observables from a 3D Bifrost simulation of flux emergence that show signs of reconnection events that can look like Ellerman Bombs.

1. Study the atmosphere

Copy the atmospheric file to your RH Atmos directory. Start with the file
/mn/stornext/d15/SAM/viggoh/3d/en024031_emer3.0/str/en024031_emer3.0str_400.ncdf
Use RH analysis tools to look for high temperature blobs in the photosphere/low chromosphere that could be Ellerman Bombs.

2. Run selected areas through RH 1.5D by Pereira and Uitenbroek (2015)

Lines to be synthesized are Mg h/k and Ca 8542

Compare the line profiles inside the Ellerman Bomb area and outside. Look at the line formation (contribution functions, optical depth scales,...

3. Look at the time evolution of the Ellerman Bomb

This entails running RH for more snapshots than the one above. They have snapshot number in the name (the atmosphere above being snapshot 400).