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Spectral Characteristics of Solar Flares in Different Chromospheric Lines and Their Implications View all abstracts by submitter

Hui Li   Submitted: 2007-02-25 22:46

Using the spectral data of representative solar ares observed with the infrared detector system of the solar spectrograph at Purple Mountain Observatory, we study the spectroscopic characteristics of solar ares in the Hα , the CaII 8542 and the HeI 10830 lines in different phases and various locations of ares, and discuss their possible implications in couple with space observations. Our results show that in the initial phase of a are the Hα line displays red-shift only and no wide-wing. Large broadenings of the Hα line are observed in a few minutes after the are onset within small regions of 3'' - 5'' in both disk and limb ares with/without non-thermal processes. Far wings similar to those of damping roadening appear not only in the Hα line but in the HeI 10830 line as well in ares with non-thermal processes. Sometimes we even detect weak far-wing emission in the CaII 8542 line in disk ares. Such large broadenings are observed in both the footpoints and the are loop-top regions, and possibly result from strong turbulence and/or macroscopic motions. Therefore, the so-called 'non-thermal wing' of the Hα line prossile is not a suffcient condition to distinguish whether non-thermal electrons are accelerated or not in a flare. The CaII 8542 line shows lower intensity in the loop-top regions and higher intensity in the parts close to the solar surface. Emissions larger than nearby continuum in the HeI 10830 line are detected only in small regions with strong X-ray emissions and avoid sunspot umbrae.

Authors: Hui Li, Jianqi You, Xingfeng Yu and Qiusheng Du
Projects: None

Publication Status: Solar Physics, accepted.
Last Modified: 2007-02-26 11:04
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