ALEXIS: Recreating the X-Ray Emission from the Full Solar Disk as a Linear Combination of Discrete Regions in the Extreme Ultraviolet and Soft X-Rays

Abstract Despite a wealth of multiwavelength, spatially resolved, time-domain solar activity data, an accurate and complete temporospatial solar flare census is unavailable, which impedes our understanding of the physics of flare production. We present an Automatically Labeled EUV and X-Ray Incident SolarFlares (ALEXIS) pipeline, designed to decompose the X-ray flux of the full solar disk into a minimum set of discrete regions on the solar surface. ALEXIS returns an average rms error between the X-Ray Sensor time series and the discrete EUV signals of 0.066 ± 0.036 for a randomly selected test bed sample of 1000 hr-long data segments from 2010 May to 2020 March. Flare emission that requires multiple regions was found to be synchronous (flares occurring at the same time), sympathetic (flares separated by minutes), or needed to capture the background emission before and/or after the main flare. ALEXIS uses the original full resolution and cadence of both the Atmospheric Imaging Assembly instrument and the GOES13–15 Solar X-Ray Imager. Comparison of ALEXIS’s catalog with those produced by the SWPC and SolarSoft show that these canonical databases need revisiting for 62% and 15% of the subsample, respectively. Additionally, we increased the number of flares reported by the SWPC and SolarSoft by 15%. Our pipeline misses 6.7% of the 1057 flare subsample and returns 5% of false positives from 1211 flares reported by ALEXIS. The ALEXIS catalog returns flare peak times, coordinates, the corrected scaled X-ray magnitude, and the associated NOAA active region with a HARP identifier number independently from any external data products.