1. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 Identification of Lines in the Range 3.3 Å - 6.1 Å Observed in RESIK Spectra B. Sylwester, J. Sylwester, M. Siarkowski Space Research Centre, Polish Academy of Sciences, Wrocław, Poland K.J.H. Phillips NASA Goddard Space Flight Center, Greenbelt, USA L. Culhane Mullard Space Science Laboratory, Dorking, Surrey, UK J. Lang Rutherford Appleton Laboratory, Chilton, Didcot, UK C. Brown Naval Research Laboratory, Washington DC, USA V.D. Kuznietsov IZMIRAN, Moscow region, Troitsk, Russia

2. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 INTRODUCTION RESIK is a common project between NRL (USA), MSSL and RAL (UK), IZMIRAN (Russia) and SRC (Poland). It is Bragg bent crystal X-ray spectrometer placed aboard the CORONAS-F satellite. The wavelength coverage of RESIK is 3.3 Å ÷ 6.1 Å (four energy channels). Preliminary analysis of spectra collected indicates presence of many spectral features identified earlier in the flaring plasmas and corresponding to the transitions 1s-2p in H-like ions and 1s 2 -1s2p in He-like ions of S and Si. In addition many prominent lines not earlier observed can be identified in RESIK spectra. We have calibrated the spectra, establishing an absolute wavelength scale and determining the absolute photon fluxes. This made it possible to identify several spectral features, some of which are observed for the first time from astrophysical plasmas. In particular we have detected lines due to highly ionized potassium and chlorine. Potassium belongs to very low FIP elements (4,31 eV) while chlorine to high ones (12.97 eV).

3. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 http://www.cbk.pan.wroc.pl/resik_catalogue.htm http://www.cbk.pan.wroc.pl/resik_catalogue.htm http://www.cbk.pan.wroc.pl/legend/legend_2003.htm

4. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 Example spectra As an example of RESIK observations in the two successive slides, we present the spectra recorded for a moderate disk (N16W05 ) flare of C5.8 class. It was a short duration event observed over its entire duration. The spectrum filled in GREEN is the original one (counts vs bin numbers) while in BLUE corresponds to the absolute calibration (photons vs Å). The individual channels are presented in different blue semi- tones: 3.35 - 3.8 - 4.3 - 4.9 -6.0 Å.

5. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 RESIK background corrected spectrum (C5.8 flare on 22 Feb.2003) Spectrum integrated over the event duration (584 s). Red arrows indicate for Cl H- and He-like line positions. Red ? indicate for unidentified lines. K XVIII S XVI Ar XVII S XV-3p S XV-4p S XV Si XIII-3p Cl ? ? ? ? Ar XVI Ar XVII 3p

6. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 Reduced RESIK spectrum for (entire) flare on 22 Feb. 2003 The spectrum has been integrated over the flare duration – 584 sec. The individual channels are presented in different blue semi-tones. K XVIII Ar XVII S XV-4p S XV-3p S XVI-2p S XV-2p Si XIII-3p Cl XVII (Lyα) Cl XVI (R,I,F) Si XIII Si XIV Si XII Ar XVIII

7. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 Distribution of activity during 1 January – 14 March 2003 We have analysed here the RESIK spectra collected between 1 January and 14 March 2003. During this period 1163 time intervals have been chosen for which the spectra have been measured. The collected set of spectra covers as well very low activity level (~B4) as few M class flares. No single X class flare has been reported during analysed period.

8. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 Data analysis Using the ratio of total (lines+continuum) fluxes measured in the most energetically separated RESIK channels ( #1 and #4) in the regions (3.4 -3.8 Å) and (5.0 – 6.05 Å) respectively we have calculated the temperature and emission measure (in an isothermal approximation) for all analysed cases. This in turn allowed us to calculate the expected continuum level and subtract it from the observed spectrum in order to better see the lines.

9. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 RESIK average spectrum for 1 January – 14 March 2003 period SGI = 388.6 hours (1163 cases added)

10. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 The same in logarithmic scale

11. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 Average spectra grouped according to the temperature K XVIII 2p Ar XVIII 2p (Lyα) S XV 4p S XIV sat We averaged the observed spectra in individual groups characterised by different temperatures.

12. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 Average spectra grouped according to the temperature S XIV sat S XV 3p Si XIV 3p Lyβ Si XIII 3p Si XIII sat Poster P 0108

13. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 Channel 1 and 2 averaged RESIK spectra Ar XVII 3p Ar XVI sat K XVIII w,x,y,z S XVI 6p Ar XVIII 2p S XVI 4p Ar XVII w,x,y,z S XV 4p S XV 3p S XVI 5p S XIV sat S XIV sat ? ? ? Poster 0112

14. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 Channel 3 and 4 averaged RESIK spectra S XIV sat S XV 3p Cl XVI w,x,y,z S XVI 2p S XV w,x,y,z Si XIV 3p Si XIII 4p Si XIII 5p Si XII sat Si XIII 3p Si XII sat Si XIV 6p Si XIV 5p Si XIV 8p Al XIII 5p Al XIII 4p Al XIII 3p ? ?

15. 35th COSPAR: Scientific Commission E1.9; Paris, 18-25 July 2004 What can be done with RESIK unique observations Determination of chemical composition of X-ray flare and active region plasma with a high precision using emission line and continuum intensities (K, Ar, Cl, S, Si, Al). FIP dependence analysis of absolute coronal abundances: FIP (eV): 4.31 5.99 8.15 10.36 11.97 15.76 element: K Al Si S Cl Ar Differential emission measure analysis (DEM)-determination of the temperature structure of emitting regions. The RESIK range includes many strong emission lines due to transitions 1s-np and 1s 2 -1snp in H-like and He-like ions respectively. The lines corresponding to the transitions for n = 2 and 3 are routinely observed for Si, S and Ar ions. For some flares we observe the enhanced emission in spectral features coinciding with these transitions for n up to 9 or 10. ( The analysis of observed line series decrements.)