A. Gordon Emslie

TL;DR: In this paper, the history of solar flare phenomena are examined in an introduction for advanced undergraduate and graduate physics students, with diagrams, graphs, and photographs of coronal mass ejections.

TL;DR: In this paper, the authors present and analyze the first high-resolution hard X-ray spectra from a solar flare observed in both Xray/gamma-ray continuum and gamma-ray lines, and derive the evolution of the nonthermal mean electron flux distribution by directly fitting the RHESSI Xray Spectra with the thin-target bremsstrahlung from a double power-law electron distribution with a low-energy cutoff.

TL;DR: In this article, the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) was used to construct spatially resolved hard X-ray spectra for each of four prominent features: a bright, soft source high in the corona, two localized, hard footpoints in opposite polarity magnetic regions that show highly correlated flux and spectral variations in time.

TL;DR: In this paper, the model-independent deconvolution of the hard X-ray spectrum is used to obtain the effective mean electron spectrum (E) in the source and the model dependent interpretation of this mean spectrum in terms of physical processes operating in that source.

TL;DR: In this paper, the authors examined empirical atmospheric structures that are consistent with enhanced white-light continuum emission in solar flares, and found that the radiative coupling of the upper chromosphere and temperature minimum regions (through Balmer continuum photons) and the transition region and upper-chromosphere (through XUV photons) can account for white light emission in the solar flares.