ECCCO: The EUV CME and Coronal Connectivity Observatory
Understanding the dynamics of eruptive events leaving the Sun and the conditions that produce the outward streaming solar wind requires knowledge of the middle corona, the region between 1.5–3 Rs. All matter, magnetic fields, and energy leaving the Sun pass through this poorly-understood sector of the Sun’s atmosphere, but observations in this region are limited. To fill this gap, we introduce The EUV CME and Coronal Connectivity Observatory (ECCCO), which has been proposed for the current NASA Heliophysics SMEX call. ECCCO consists of two instruments: an imager that views the Sun out to 3 Rs and a spectrograph that produces spectrally pure, overlapped images of the Sun (overlappograms). Both instruments will have two channels, a long channel ranging from 171 — 208 Å to capture plasma in the 1-2.5 MK range, and a short channel ranging from 126 — 138 Å to capture hot plasma in the 8-12 MK range. The science goals of ECCCO are two-fold: 1. To understand the sources, release and acceleration of the solar wind, and 2. To understand the symbiotic relationship between eruptive solar events and the large scale coronal structure.
Dr. Reeves is a Senior Astrophysicist at the Harvard-Smithsonian Center for Astrophysics. Her research focuses on two main, interconnected topics: thermal energy transport during solar eruptions, and the magnetic reconnection process that drives solar eruptions. She is currently the US Project Scientist for the X-Ray Telescope on the Hinode mission, and the is the PI of the proposal submitted to the NASA Heliophysics SMEX call to build ECCCO, the EUV CME and Coronal Connectivity Observatory.