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XUV monochromatic imaging spectroscopy in the SPIRIT experiment on the CORONAS-F mission

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.

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XUV monochromatic imaging spectroscopy in the SPIRIT experiment on the CORONAS-F mission

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  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.

  5. CORONAS-F (russian version) Launch Date: July 31, 2001 More on CORONAS project

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

  7. EUV images by SRT device

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

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

  10. Remarkable flares for the period 23.10.2003 – 04.11.2003

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

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

  13. Optical layout of the RES-C spectroheliometer

  14. RES-S spectroheliogram in 177-207A

  15. RES-S spectroheliogram in 285-335A

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

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

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

  19. 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 105 – 107K. 5. Region 177-207: 65 lines registered; 48 lines identified; 1 prominent flare line. Temperature range 106 – 107K. 6. 50 Lines of Fe in different ionization stages (mainly Fe X – Fe XV) were observed.

  20. 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).

  21. Self-consistency check 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.

  22. Preliminary results

  23. 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

  24. Two kinds of diagnostics • Ne diagnostics at selected Te based on density sensitive intensity ratios. More than 10 ratios were found in experimental spectra. • DEM analysis. More than 30 density insensitive lines were selected for DEM determination.

  25. DEM for the active region and the flare 28.12.2001

  26. 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.

  27. DEM for different active regions and the flare

  28. SPIDER: 12.11.2001(Mg)

  29. 2001, November 12 SXT SPIRIT MgXII

  30. 2001, November 12 1 1 1 SXT MgXII ALL 1 SXT & SPIRIT

  31. SXT+Mg, 12.11.2001 (Height)

  32. 2001, October 22 SXT SPIRIT MgXII

  33. 2001, October 22 1 1 1 1 2 2 2 2 SXT & SPIRIT SXT MgXII ALL

  34. SPIDER: 29.12.2001(Mg)

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

  36. The same SPIDER (IAT,195)

  37. The same SPIDER (IAT+Mg)

  38. Height distribution of line intensities (29.12.2001)

  39. Height distribution of the DEM (29.12.2001)

  40. GOES data

  41. Spider activity

  42. Comparison of GOES & Mg XII time profiles

  43. Correlation of GOES & MgXII fluxes

  44. GOES 1-8 response ratios

  45. Empirical law

  46. Temporal profiles of emission measure and luminosity

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