B. R. Dennis

TL;DR: The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) as mentioned in this paper uses nine rotating modulation collimators that time-modulate the incident flux as the spacecraft rotates.

TL;DR: Using coordinated observations from instruments on the Advanced Composition Explorer (ACE), the Solar and Heliospheric Observatory (SOHO), and the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), this article evaluated the energetics of two well-observed flare/CME events on 21 April 2002 and 23 July 2002.

TL;DR: In this article, the authors compared the physical characteristics of the two flares and found that the main difference between them was in the pre-flare state of the coronal plasma at the flare site: before the first flare it was relatively cool (3 × 106 K) and tenuous (4 × 109 cm-3), but owing to the residual effects of the first X-ray flare, it was hotter and denser at the onset of the second flare, and they are led to believe from these data that the plasma filling the flaring loops absorbed most of the energy

TL;DR: In this article, the authors compare four different methods of calculating uncertainty estimates in fitting parameterized models to Ramaty High Energy Solar Spectroscopic Imager X-ray spectra, considering only statistical sources of error.