Observational Analysis of Lyα Emission in Equivalent-magnitude Solar Flares

Abstract

The chromospheric Ly α line of neutral hydrogen (1216 Å) is the most intense emission line in the solar spectrum, yet until recently observations of flare-related Ly α emission have been scarce. Here, we examine the relationship between nonthermal electrons accelerated during the impulsive phase of three M3 flares that were co-observed by RHESSI, GOES, and the Solar Dynamics Observatory, and the corresponding response of the chromosphere in Ly α . Despite having identical X-ray magnitudes, these flares showed significantly different Ly α responses. The peak Ly α enhancements above the quiescent background for these flares were 1.5%, 3.3%, and 6.4%. However, the predicted Ly α enhancements from FISM2 were consistently <2.5%. By comparing the properties of the nonthermal electrons derived from spectral analysis of hard X-ray observations, flares with a “harder” spectral index were found to produce a greater Ly α enhancement. The percentage of nonthermal energy radiated by the Ly α line during the impulsive phase was found to range from 2.0% to 7.9%. Comparatively, the radiative losses in He ii (304 Å) were found to range from 0.6% to 1.4% of the nonthermal energy while displaying enhancements above the background of 7.3% to 10.8%. FISM2 was also found to underestimate the level of He ii emission in two of the three flares. These results may have implications for space weather studies and for modeling the response of the terrestrial atmosphere to changes in the solar irradiance, and will guide the interpretation of flare-related Ly α observations that will become available during Solar Cycle 25.

Keywords

• Solar flares
• Solar physics
• Solar x-ray flares
• Solar extreme ultraviolet emission
• Solar chromosphere
• Active sun