Chromospheric Evaporation In The Gradual Flare Phase

Details Chromospheric Evaporation In The Gradual Flare Phase Chromospheric Evaporation In The Gradual Flare Phase

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.446..257c&link_type=abstract

8th SOHO Workshop: Plasma Dynamics and Diagnostics in the Solar Transition Region and Corona. Proceedings of the Conference hel

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

SOHO/CDS observations are used to determine relative line-of-sight velocities and their temporal evolution in the late gradual flare phase. The observations started about 1 hour after the M6.8 two-ribbon flare in NOAA 8210 on April 29, 1998. Velocity maps in O V 629 A (Tmax = 0.25 MK), Fe XVI 360 A (Tmax = 2 MK), and Fe XIX 592 A (Tmax = 6.3 MK), covering temperatures from the transition region to the corona show strong gradients at the position of the Hα ribbons. Downflows are observed in the footpoint regions of the post-flare loops whereas the velocities observed further away from the magnetic neutral line are interpreted as upflows due to chromospheric evaporation. Loops are filled with hot plasma and their footpoints become visible later on at the former evaporation site. At the same time the Hα ribbon is slowly moving outward together with the location of the velocity gradient. Our observations strongly support models in which chromospheric evaporation driven by magnetic reconnection is responsible for the continuous formation of loops, which are visible for several hours after the flare's maximum in EUV and soft X-ray radiation.

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