Conduction-driven chromospheric evaporation in a solar flare

Details Conduction-driven chromospheric evaporation in a solar flare Conduction-driven chromospheric evaporation in a solar flare

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...329..456z&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 329, June 1, 1988, p. 456-463. Research supported by the Lockheed Independe

Astronomy and Astrophysics

Astrophysics

35

Chromosphere, Conductive Heat Transfer, Evaporation, Solar Corona, Solar Flares, Solar X-Rays, Calcium, Doppler Effect, Line Spectra, Magnesium, Solar Maximum Mission, X Ray Spectra

Scientific paper

Observations of gentle chromospheric evaporation during the cooling phase of a solar flare are presented. Line profiles of the low-temperature (T of about 6 x 10 to the 6th K) coronal Mg XI line, observed with the X-Ray Polychromator on the Solar Maximum Mission, show a blueshift that persisted for several minutes after the impulsive heating phase. This result represents the first detection of an evaporation signature in a soft X-ray line formed at this low temperature. By combining the Mg XI blueshift velocity data with simultaneous measurements of the flare temperature derived from Ca XIX observations, it is demonstrated that the upward flux of enthalpy transported by this gently evaporating plasma varies linearly with the downward flux of thermal energy conducted from the corona. This relationship is consistent with models of solar flares in which thermal conduction drives chromospheric evaporation during the early part of the cooling phase.

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