Chromospheric Evaporation in an M1.8 Flare Observed by the Extreme-ultraviolet Imaging Spectrometer on Hinode
George A. Doschek, Harry P. Warren, Peter R. Young

TL;DR
This study reports detailed spectroscopic observations of chromospheric evaporation during an M1.8 solar flare, revealing multi-temperature plasma flows, isothermal sources, and possible reconnection-related downflows, enhancing understanding of flare dynamics.
Contribution
It provides the first comprehensive spectroscopic analysis of chromospheric evaporation in a complex flare using Hinode/EIS data, highlighting multi-temperature flow patterns and potential reconnection signatures.
Findings
150-200 km/s upflows in hot flare ions
Cooler ions show complex behavior with some upflows
Evidence of downward shock possibly related to reconnection
Abstract
We discuss observations of chromospheric evaporation for a complex flare that occurred on 9 March 2012 near 03:30 UT obtained from the Extreme-ultraviolet Imaging Spectrometer (EIS) on the Hinode spacecraft. This was a multiple event with a strong energy input that reached the M1.8 class when observed by EIS. EIS obtained a full-CCD spectrum of the flare. Chromospheric evaporation characterized by 150-200 km/s upflows was observed in multiple locations in multi-million degree spectral lines of flare ions such as Fe XXII, Fe XXIII, and Fe XXIV, with simultaneous 20-60 km/s upflows in million degree coronal lines from ions such as Fe XII - Fe XVI. The behavior of cooler, transition region ions such as O VI, Fe VIII, He II, and Fe X is more complex, but upflows were also observed in Fe VIII and Fe X lines. At a point close to strong energy input in space and time, the flare ions Fe XXII,…
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