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Solar flares sometimes lead to coronal mass ejections that directly affectthe Earth's environment. However, a large fraction of flares, including onsolar-type stars, are confined flares. What are the differences in physicalproperties between confined and eruptive flares? For the first time, wequantify thermodynamic and magnetic properties of hundreds of confined anderuptive flares of GOES class C5.0 and above, 480 flares total. We firstanalyze large flares of GOES class M1.0 and above observed by the SolarDynamics Observatory (SDO): 216 flares total, including 103 eruptive and 113confined flares, from 2010 until 2016 April, we then look at the entire datasetabove C5.0 of 480 flares. We compare GOES X-ray thermodynamic flare properties,including peak temperature and emission measure, and active-region andflare-ribbon magnetic field properties, including reconnected magnetic flux andpeak reconnection rate. We find that for fixed peak X-ray flux, confined anderuptive flares have similar reconnection fluxes; however, for fixed peak X-rayflux confined flares have on average larger peak magnetic reconnection rates,are more compact, and occur in larger active regions than eruptive flares.These findings suggest that confined flares are caused by reconnection betweenmore compact, stronger, lower lying magnetic-fields in larger active regionsthat reorganizes smaller fraction of these regions' fields. This reconnectionproceeds at faster rates and ends earlier, potentially leading to moreefficient flare particle acceleration in confined flares.

A Database of Magnetic and Thermodynamic Properties of Confined And Eruptive Solar Flares