1. XUV monochromatic imaging spectroscopy in the SPIRIT experiment on the CORONAS-F mission I. Diagnostics of solar corona plasma by means of EUV Spectroheliograph RES-C on CORONAS-F spacecraft. II. XUV-diagnostics and modeling of active plasma structures observed in the SPIRIT experiment on the orbital station CORONAS-F. A.Urnov, I.Zhitnik, S.Kuzin, S. Bogachev, S.Bozhenkov, F.Goryaev, S.Shestov P.N.Lebedev Physics Institute of Russian Academy of Sciences (FIAN) urnov@sci.lebedev.ru

2. http://coronas.izmiran.ru/

3. CORONAS-F satellite

4. CORONAS-F CORONAS-F was launched July 31, 2001 at 0800 GMT and passed away December 07, 2005 The satellite was launched by a Cyclone rocket SL-14 at the launch pad Plesetsk (Russia). The inclination of the orbit is 83 degrees and the altitude about 500km. This orbit permits observational periods until 20 days without interruption by entering the Earth's shadow.Cyclone rocket

5. CORONAS-F (russian version) Launch Date: July 31, 2001 More on CORONAS project More on CORONAS project Science Objectives Energy transfer from the solar interior to the surface and subsequent release in non-stationary solar events Origin and propagation of solar cosmic rays Solar global oscillations and internal structure of the Sun Dynamic phenomena of the active Sun and geophysical effects of solar flares

6. Space experiments on XUV spectroscopy at the Lebedev Institute (FIAN)

8. EUV images by SRT device

9. “Spider” observed in the Mg XII channel (8.42A)

10. X-ray sources spatially resolved in the Mg XII line images

11. Remarkable flares for the period 23.10.2003 – 04.11.2003

12. Temporal evolution of the flux in the Mg XII channel

13. The flux in the Mg XII channel recorded during the flare with high temporal resolution

14. Optical layout of the RES-C spectroheliometer

15. RES-S spectroheliogram in 177-207A

16. RES-S spectroheliogram in 285-335A

17. Solar corona resolved in the Si (303.32 A) and the He II (303.78 A) ion lines by the spectroheliograph RES

18. Fe XII lines at 195 A resolved by the RES device

19. Flare spectra in Fe XII and Fe XIII lines recorded by the RES

20. The Catalog of solar lines in the region 280-330 A Zhitnik et al., Astronomy Letters, 31, #1,37-56, 2005 1. Resolution of experimental spectra is about 0.1 A. 2. The accuracy of wavelength determination is about 0.04 A. 3. The accuracy of relative intensity calibration is below 20 %. 4. Region 279-331: 100 lines registered; 54 lines identified; 15 lines (of them 12 are unidentified) were observed only in flares. Temperature range 10 5 – 10 7 K. 5. Region 177-207: 65 lines registered; 48 lines identified; 1 prominent flare line. Temperature range 10 6 – 10 7 K. 6. 50 Lines of Fe in different ionization stages (mainly Fe X – Fe XV) were observed.

21. Density diagnostics Density sensitive ratios: Fe XI 1.3 MK 181.14/180.41, 181.14/179.76, 181.14/184.41 Fe XII 1.6 MK 190.07/200.36, 190.07/186.85+186.88 Fe XIII T = 1.6 MK 203.80+203.82/202.04; 321.40/320.81; 312.87/321.40; 318.13/321.40 Fe XV T = 2 MK 307.75/324.98; 284.16/307.75; 327.03/307.75 S XI T = 2 MK 291.58/285.82; 291.58/281.40 S XII T = 2 MK 288.42/299.54 Ni XV 2.5 MK 176.11/176.74, 176.11/179.27 Diagnostics is based on CHIANTI (http://www.solar.nrl.navy.mil/chianti.html).

22. Self-consistency check RatioTeTe AR 1 29.12.2001AR 2 29.12.2001AR 30.12.2001 FeXIII 321.40/320.81 1.6 MK 1.9e92.5e92.4e9 FeXIII 312.87/321.40 1.6 MK 1.9e93.4e92.5e9 FeXIII 318.13/321.40 1.6 MK 4.3e95.2e95.4e9 FeXV 307.75/324.98 2 MK 3.9e94.4e9No data FeXV 327.03/321.77 2 MK 1.7e101.1e101.13e10 FeXV 284.16/307.75 2 MK Out of range SXI 291.58/285.82 2 MK 1.4e92.3e91.6e9 SXI 291.58/281.40 2 MK 1.7e91.8e9 SXII 288.42/299.54 2 MK 1.8e92e92.2e9 Problem lines: FeXIII 318.13; FeXV 327.03, 284.16. Adopted lines: FeXIII 321.40, 320.81, 312.87; Fe XV 307.75, 324.98; S XI 291.58, 285.82, 281.40; S XII 288.42, 299.54.

23. Preliminary results Quiet Sun N80-90 E0 16.09.2001 03.59.36 AR NOAA 9765 29.12.2001 14:48:53 Flare M5.6 AR 9608 16.09.2001 03:59:36 Flare M7.6 AR 9628 25.09.2001 04:50:42 Log N e 8.79.3>9.710

24. Diagnostics in region 176-207 A Density sensitive ratios: Ni XV 2.5 MK 176.11/176.74, 176.11/179.27 Fe XIII 1.6 MK 203.80+203.82/202.04 Fe XII 1.6 MK 190.07/200.36, 190.07/186.85+186.88 Fe XI 1.3 MK 181.14/180.41, 181.14/179.76, 181.14/184.41 Lines for DEM reconstruction: Fe X 1.3 MK 177.24, 184.54; Fe XI 1.3 MK 181.14, 182.17; Fe XII 1.6 MK 190.07; S XI 2MK 188.68, 191.27; Ni XV 2.5 MK 176.11; Ca XIV 4 MK 193.87; Ca XVII 6.3 MK 192.82; Fe XVII 7.9 MK 204.65; Fe XXIV 16 MK 192.03

25. Two kinds of diagnostics 1) N e diagnostics at selected T e based on density sensitive intensity ratios. More than 10 ratios were found in experimental spectra. 2) DEM analysis. More than 30 density insensitive lines were selected for DEM determination.

26. DEM for the active region and the flare 28.12.2001

27. Properties of RES spectral lines used for the DEM analysis and observed-to-predicted intensity ratios: left column corresponds to the BI and the right one in brackets to the CHIANTI. ActiveRegionNOAA 9765Flare X3.4 class28.12.2001 (Å) IonIntensity ErrorObserv./Predic.Intensity ErrorObserv./Predic. 279.74CrXXII - - - 365 17 1.00 (1.05) 291.98NiXVIII 816 80 0.99 (0.93) 4605 433 1.05 (0.74) 292.49FeXXII - - - 651 18 1.01 (0.87) 292.82Si IX 288 30 1.01 (0.91) 311 14 0.92 (0.96) 296.14Si IX 483 50 1.00 (0.92) 586 13 1.02 (0.85) 302.19CaXVIII 154 20 1.00 (1.32) 3212 301 1.00 (1.17) 303.33Si XI 2800 300 1.00 (1.04) 1614 303 1.00 (1.51) 315.02MgVIII 612 60 1.00 (1.02) 636 18 1.00 (1.17) 320.57NiXVIII 392 40 1.01 (0.96) 1828 261 0.89 (0.87)

28. DEM for different active regions and the flare

29. SPIDER: 12.11.2001(Mg)

30. 2001, November 12 SXTSPIRIT MgXII

31. 1 1 1 1 2001, November 12 SXT & SPIRIT SXTMgXIIALL

32. SXT+Mg, 12.11.2001 (Height)

33. 2001, October 22 SXTSPIRIT MgXII

34. 1 2 111 2 2 2 2001, October 22 SXT & SPIRIT SXTMgXIIALL

35. SPIDER: 29.12.2001(Mg)

36. SPIDER: 29.12.2002 (304,284,175, Mg)

37. The same SPIDER (IAT,195)

38. The same SPIDER (IAT+Mg)

39. Height distribution of line intensities (29.12.2001)

40. Height distribution of the DEM (29.12.2001)

41. GOES data

43. Spider activity

45. Comparison of GOES & Mg XII time profiles

47. Correlation of GOES & MgXII fluxes

48. GOES 1-8 response ratios

49. Empirical law

50. Temporal profiles of emission measure and luminosity

56. Conclusions XUV spectroheliograph RES provides: The distribution of electron density over the temperature The distribution of the DEM over the temperature and the height Diagnostics of thermal/supra-thermal regions Diagnostics of elemental abundances Temporal profiles and localization of 8 MK plasma