Abstract
Investigations of solar activity require information about plasma in a wide range of temperatures. Generally, researchers require observations from telescopes producing monochromatic images of coronal plasma with cool, warm, and hot temperatures. Until now, monochromatic telescopic imaging has been made only in the Mg XII 8.42 Å line with the Mg XII spectroheliograph on board CORONAS-I, CORONAS-F, and CORONAS-PHOTON satellites. The Mg XII spectroheliograph used Bragg crystal optics. Its design is based on two main principles: (1) to select the working wavelength and the crystal in such a way that reflection occurs at small incident angles; (2) to use the aperture of the mirror as a spectral filter. We believe that these design principles can be applied to other spectral lines. In this article, we will review the design of the Mg XII spectroheliograph and present our thoughts on how to apply these principles to the Si XIV 6.18 Å and Si XIII 6.65 Å lines. A combination of the monochromatic Mg XII 8.42 Å, Si XIV 6.18 Å, and Si XIII 6.65 Å images will help us to study the dynamics of the hot plasma in the solar corona.
Highlights
Plasma in solar phenomena can be at a wide range of temperatures
We will review the design of the Mg XII spectroheliograph and present our thoughts on how these principles could be applied to other spectral lines
The Mg XII images mark the location of the heating in the solar corona, which makes the Mg XII spectroheliograph a useful instrument in studying the dynamics of hot plasma
Summary
Plasma in solar phenomena can be at a wide range of temperatures. Quiet Sun and active regions are at temperatures around 1 MK, while during flares, the coronal plasma can reach temperatures beyond 10 MK. Imaging spectrometers—such as the Extreme ultraviolet Imaging Spectrometer (Culhane et al, 2007) on board the Hinode satellite (Kosugi et al, 2007), the Coronal Diagnostic Spectrometer (Harrison et al, 1995) on board the Solar and Heliospheric Observatory (Domingo et al, 1995), the Interface Region Imaging Spectrograph (De Pontieu et al, 2014), or Marshall Grazing Incidence X-ray Spectrometer (MaGIXS; Kobayashi et al, 2011; Athiray et al, 2019)—can achieve this goal These instruments build raster images of the solar corona in multiple spectral lines. We will review the design of the Mg XII spectroheliograph and present our thoughts on how these principles could be applied to other spectral lines
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