Patterns of X-ray line emission variability as observed by the RESIK Bragg spectrometer

Details Patterns of X-ray line emission variability as observed by the RESIK Bragg spectrometer Patterns of X-ray line emission variability as observed by the RESIK Bragg spectrometer

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003esasp.535..733s&link_type=abstract

In: Solar variability as an input to the Earth's environment. International Solar Cycle Studies (ISCS) Symposium, 23 - 28 June 2

Physics

6

Solar Physics, X-Rays, Spectra, Instruments: Resik

Scientific paper

RESIK is a unique Bragg bent crystal spectrometer operating continuously since August 2001. By now, it has collected ~10 GB of solar flare and active region spectra in a very much unexplored spectral region between 3.2 Å and 6.1 Å. In this paper we present a number of representative observations covering periods of various solar activity: from the most active level (M+ flares) to exceptionally quiet corona. We present also a tentative list of the spectral features observed. In the wavelength range observed by RESIK there are a number of strong emission lines corresponding to H- and He-like resonance transitions of Si, S, Ar and K ions. These lines are formed by thermal plasma of temperature between 5 and 50 MK, and therefore their analysis reveal the distribution of hot plasma over this interval. RESIK sees lines from a number of different elements, so it is possible to do abundance analyses. The elements concerned have a wide range of first ionisation potentials (FIPs) so it has been possible to examine the dependence of coronal or flare abundances on FIP. We have observed substantial variations of the K/Ar line ratio, and respective line/continuum ratios, which can be best explained by allowing for changes in the chemical composition of the coronal plasma

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