1. INTRODUCTION

2. DATA AND REDUCTION  
2.2. UV Lightcurve Creation  
2.3. X-ray Lightcurve Creation  
2.4. Flare Identification with FLAIIL

3. M-DWARF FLARES IN THE FUV  
3.2. M-Dwarf Flares: Absolutely Different, Relatively the Same  
3.3. Energy Emitted at FUV Wavelengths Could be Dominated by Flares  
3.4. How Big Do Flares Get?  
3.5. How Small Do Flares Get? Microflares and Quiescent FUV Emission

4. FLARES IN ISOLATED EMISSION LINES  
4.1. Flare Frequency Distributions (FFDs) by Emission Line  
4.2. Ly α is a Gentle Giant  
4.3. Comparison to Solar Flares  
4.4. An Inconsistent Relationship Between Flare FUV and X-ray Emission  
4.5. Emission Line Profiles

5. STELLAR PROPERTIES AND STELLAR FLARES

6. FLARE LIGHTCURVES AND ENERGY BUDGETS  
6.1. Flare Lightcurves  
6.2. Spectral Energy Budget

7. A FIDUCIAL UV FLARE FOR MODELING PLANETARY ATMOSPHERES  
7.1. Observed and Unobserved FUV  
7.2. Blackbody  
7.3. EUV  
7.4. Lightcurve

8. M DWARF UV FLARES AND PLANETS  
8.2. A Discussion of Mass Loss  
8.3. A Glaring Unknown in the Planetary Impacts of Stellar Flares: Particle Events

9. SUMMARY