Physics
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..107..311w&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 107, no. 2, 1987, p. 311-321. Research supported by the Chinese Academy of Sciences.
Physics
4
Chromosphere, H Alpha Line, H Beta Line, Solar Flares, Solar Spectra, Spectrographs, Abundance, Line Spectra, Penumbras, Solar Corona, Telescopes
Scientific paper
Spectra of a 2B flare were observed simultaneously at H-alpha, H-beta, and Ca II H, K lines on February 3, 1983 with the Nanjing University multichannel spectrograph, and five semiempirical models corresponding to different times of the chromospheric flare have been computed. During the impulsive phase, rapid outward expansion of the flare chromospheric region is followed by a quick downward contraction, and the transition region undergoes a pulse process. The time of maximum chromospheric evaporation is about the same as that of the spectral line intensities, and the chromosphere is most compact just after the maximum of the spectral line intensities. The distribution of microturbulence velocity in the chromospheric flare shows some deviation from that in the case of the quiet sun.
Cheng Fang
Wei-Qun Gan
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