# Solar Ellerman Bombs in 1-D Radiative Hydrodynamics

## TL;DR

This study uses 1D radiative hydrodynamics simulations to investigate the atmospheric conditions of Ellerman Bombs, aiming to reproduce observed spectral line profiles and understand their physical origins.

## Contribution

The paper applies RADYN and line synthesis codes to simulate EB signatures, providing insights into their atmospheric temperature and dynamics, and challenges previous superheated photosphere models.

## Key findings

- Superheated regions (>10,000 K) are unlikely to produce EB signatures.
- Simulations can replicate some spectral line profiles but not all simultaneously.
- The physical conditions of EBs are complex and not fully captured by current models.

## Abstract

Recent observations from the Interface Region Imaging Spectrograph (IRIS) appear to show impulsive brightenings in high temperature lines, which when combined with simultaneous ground based observations in H$\alpha$, appear co-spatial to Ellerman Bombs (EBs). We use the RADYN 1-dimensional radiative transfer code in an attempt to try and reproduce the observed line profiles and simulate the atmospheric conditions of these events. Combined with the MULTI/RH line synthesis codes, we compute the H$\alpha$, Ca II 8542~\AA, and Mg II h \& k lines for these simulated events and compare them to previous observations. Our findings hint that the presence of superheated regions in the photosphere ($>$10,000 K) is not a plausible explanation for the production of EB signatures. While we are able to recreate EB-like line profiles in H$\alpha$, Ca II 8542~\AA, and Mg II h \& k, we cannot achieve agreement with all of these simultaneously.