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Mg II Lines Observed during the X-class Flare on 29 March 2014 by the Interface Region Imaging Spectrograph | | W. Liu
; P. Heinzel
; L. Kleint
; J. Kasparova
; | | Date: |
2 Nov 2015 | | Abstract: | Mg II lines represent one of the strongest emissions from the chromospheric
plasma during solar flares. In this article, we studied the Mg II lines
observed during the X1 flare on March 29 2014 (SOL2014-03-29T17:48) by IRIS.
IRIS detected large intensity enhancements of the Mg II h and k lines,
subordinate triplet lines, and several other metallic lines at the flare
footpoints during this flare. We have used the advantage of the slit-scanning
mode (rastering) of IRIS and performed, for the first time, a detailed analysis
of spatial and temporal variations of the spectra. Moreover, we were also able
to identify positions of strongest HXR emissions using RHESSI observations and
to correlate them with the spatial and temporal evolution of Mg II spectra. The
light curves of the Mg II lines increase and peak contemporarily with the HXR
emissions but decay more gradually. There are large red asymmetries in the Mg
II h and k lines after the flare peak. We see two spatially well separated
groups of Mg II line profiles, non-reversed and reversed. In some cases, the Mg
II footpoints with reversed profiles are correlated with HXR sources. We show
the spatial and temporal behavior of several other line parameters (line
metrics) and briefly discuss them. Finally, we have synthesized the Mg II k
line using our non-LTE code with the MALI technique. Two kinds of models are
considered, the flare model F2 of Machado et al. (1980) and the models of
Ricchiazzi and Canfield (1983). Model F2 reproduces the peak intensity of the
unreversed Mg II k profile at flare maximum but does not account for high wing
intensities. On the other hand, the RC models show the sensitivity of Mg II
line intensities to various electron-beam parameters. Our simulations also show
that the microturbulence produces a broader line core, while the intense line
wings are caused by an enhanced line source function. | | Source: | arXiv, 1511.0480 | | Services: | Forum | Review | PDF | Favorites | |
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