Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002acasn..43...41l&link_type=abstract
Acta Astronomica Sinica, vol.43, no.1, p. 41-47
Astronomy and Astrophysics
Astronomy
Scientific paper
The Doppler broadening, Stark broadening and various kinds of broadening parameters of He I 10830 A line in solar flare are calculated and discussed and consequently the following results are got: radiation damping can be neglected when compared with Doppler broadening, and in the case of generally accepted electron density in a solar flare (Ne=3.2×1013), all the damping terms will not lead to distinguishable broadening in the He I 10830 A profile. All the damping effects will not result in discernible increment of the half width of He I 10830 A until the electron density reaches to 1015cm-3 when the largest increment is about 10-3A. Therefore, the line center of He I 10830 A line can be taken as Doppler broadening. When electron density is greater than 1014cm-3, Stark broadening, especially that by electron collision, will play a major role in the broadening of He I 10830 A line. In order for the half width of the line resulted from Stark broadening to be 1-2 times greater than that from Doppler broadening, the half width from damping effect will be equivalent to that from Doppler effect. Consequently, the electron density will be of the order of 1017cm-3 if we interpret the observed He I 10830 A profiles in the 1989 limb flare by Stark broadening. Broadening effect caused by collision with helium atom (g3) has different impact on I12 and I3 component. The impact on I12 is about one order greater than that on I3. The observed He I 10830 A profiles of 1989 limb flare show that I12 and I3 have almost the same extended profile, therefore, they can not result from g3.
Li Handong
You Jian-Qi
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