Correlated Dynamics of Hot and Cool Plasmas in the Main Phase of a Solar Flare

Details Correlated Dynamics of Hot and Cool Plasmas in the Main Phase of a Solar Flare Correlated Dynamics of Hot and Cool Plasmas in the Main Phase of a Solar Flare

Mar 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...568l..61k&link_type=abstract

The Astrophysical Journal, Volume 568, Issue 1, pp. L61-L65.

Astronomy and Astrophysics

Astronomy

64

Magnetohydrodynamics: Mhd, Plasmas, Sun: Corona, Sun: Flares, Sun: Uv Radiation

Scientific paper

We report far-ultraviolet observations of a solar limb flare obtained by the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer. At a fixed pointing of the slit above the limb, spectra were simultaneously obtained in several emission lines that covered a wide temperature range from ~104 to ~107 K. The temporal evolution of the spectra revealed, for the first time, a high degree of correlation between the dynamical behavior of hot (T~107 K) and cool (T~104 K) coronal material during the main phase of a flare. We note that the data did not show any indication of the presence of a prominence. Hot and cool plasmas brightened at nearly the same location. Their Doppler shifts, which were opposite to each other, reached peak values simultaneously. Thereafter, the two components showed anticorrelated, rapidly damped, and oscillatory Doppler shifts and a very similar decay of the line widths, but with the cool plasma reaching maximum brightness before the hot plasma. This behavior points to an active role for cool plasma in the dynamics of this flare, different from the usual picture of passive cooling after the impulsive phase. We suggest a model in which the localized cooling of coronal plasma by the thermal instability triggers magnetic reconnection through the resulting enhanced resistivity, the combined processes leading to the correlated dynamics of hot and cool plasmas in a loop-loop interaction geometry.

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