The diversity of spectral shapes of hydrogen Lyman lines and Mg II lines in a quiescent prominence
Authors:
P. Schwartz, S. Gunar, J. Koza, P. Heinzel
Image & caption:
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Image caption::
Statistical distribution of profiles of the spectral lines Lyα-Lyδ a Mg II h a k according to numbers of peaks: all detected peaks on abscissa versus peaks above noise on ordinate. Different colors/symbols corresponds to mark affiliation of profiles to one of the following groups: 1p -profiles with only one peak, 2p_a&mp_b - profiles with two peaks above the noise and one or more lost in noise, 2p_{ab} - 2-peak profiles with peaks detected regardless the noise, 2p_a - profiles with only two peaks both above noise, 2p_a&mp_b - profiles with peaks above noise and one or more lost in the noise, xp - peculiar profiles and profiles not belonging to any of the previous groups.
Description:
In this work we are analyzing characteristics of profiles of the spectral lines of hydrogen Lyman series Lyα-Lyδ and UV lines h a k of singly ionized magnesium (Mg II) observed on October 22, 2013 with two space-born spectrographs SoHO/SUMER and IRIS in a quiescent solar prominence. Except for the following profile characteristics - integrated intensity, depth of the dip - so-called reversal - in the profile cores due to the self-absorption, and asymmetry of intensities at peaks around the reversals, which were used in our previous works, in this work numbers of peaks and reversals in spectral profiles of more complex shapes (multi-peak profiles) were also analyzed. Moreover, noise was also taken into account in this analysis. Results of this work show that for diagnostics of velocities of prominence fine structures the best approach is analyzing asymmetries of peaks in the multi-peak Mg II line profiles. On the other hand, for diagnostics of temperature and gas pressure of the prominence plasma, analysis of reversal depth and integrated intensities of profiles only with deep reversals surrounded with two peaks above noise for a combination of the spectral lines Lyα-Lyδ a Mg II h a k.
Reference:
Astronomy and Astrophysics 684, article no. A197, p. 1-25 (2024)
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