The RHESSI Spectrometer

By David M. Smith, R. Lin, P. Turin, D. Curtis, J. Primbsch, R. Campbell, R. Abiad, P. Schroeder, C. Cork, E. Hull and 10 more. 2002

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RHESSI Observations of Particle Acceleration and Energy Release in an Intense Solar Gamma-Ray Line Flare (2003, background): “The narrow prompt de-excitation lines of Fe, Mg, Si, Ne, C, and O are resolved for the first time (Smith et al. 2003).”
Deducing Electron Properties from Hard X-ray Observations (2011, background): “The angular distribution of accelerated ions can be studied by measuring the energies and widths of broad γ -ray lines (for details, see Smith et al. 2003).”
Electron Bremsstrahlung Hard X-Ray Spectra, Electron Distributions, and Energetics in the 2002 July 23 Solar Flare (2003, background): “(The spectra above 300 keV are discussed in Share et al. 2003 and Smith et al. 2003.)”
RHESSI Microflare Statistics. II. X-Ray Imaging, Spectroscopy, and Energy Distributions (2007, methodology): “These background-subtracted observed count spectra are forward-fitted with a model in photon space converted back to count space using the full RHESSI detector response matrix (Smith et al. 2002) in the OSPEX software package, an updated version of the SPEX code (Schwartz 1996).”