Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983acaps...3..169w&link_type=abstract
(Acta Astrophysica Sinica, vol. 3, no. 3, 1983, p. 169-182) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 7, Dec. 19
Astronomy and Astrophysics
Astrophysics
7
Emission Spectra, Solar Prominences, Solar Spectra, Spectrum Analysis, Balmer Series, H Alpha Line, Least Squares Method, Optical Thickness
Scientific paper
A new method of analyzing the emission spectrum of solar prominences is presented, in which the source function is allowed to vary with optical depth. Least-squares fitting of the observed profile determines simultaneously the optical depth T(0), the Doppler width, and the factor characterizing the variation of the source function. This method is applied to the early Balmer lines in ten prominences of Ye (1961). The results show that as the source function of the self-reversed H-alpha line increases towards the center of the prominence, the value at the center is 1.2 - 2.5 times the value at the edge. Neglect of this variation will give too large values of T(0). The degree of attenuation by self-absorption also depends on this variation. Discussion of the variation gives support to the view that the main exciting mechanism in solar prominences is the scattering of the incident radiation.
Shi Zhing-Xian
Wang Jing-Xiu
No associations
LandOfFree
A method of analyzing the emission lines of solar prominences does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with A method of analyzing the emission lines of solar prominences, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A method of analyzing the emission lines of solar prominences will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1802115