1. Introduction
2. Observations and data preparation
3. Methodology
3.1. eROSITA variability tests
3.2. Variability test comparison
3.3. Optical contamination by bright stars
3.4. Visualisations
4. Results
4.1. Variability test results
4.2. The most variable eFEDS sources
4.3. Stellar flare events
4.4. Remarks on the AGN sub-sample
5. Comparison with 2RXS
6. Comparison with the XMM-ATLAS field
7. Summary