XUV monochromatic imaging spectroscopy in the SPIRIT experiment

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

http: //coronas. izmiran. ru/

CORONAS-F satellite

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 500 km. This orbit permits observational periods until 20 days without interruption by entering the Earth's shadow.

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

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

EUV images by SRT device

“Spider” observed in the Mg XII channel (8. 42 A)

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

Remarkable flares for the period 23. 10. 2003 – 04. 11. 2003

Temporal evolution of the flux in the Mg XII channel

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

Optical layout of the RES-C spectroheliometer

RES-S spectroheliogram in 177 -207 A

RES-S spectroheliogram in 285 -335 A

Solar corona resolved in the Si (303. 32 A) and the He II (303. 78 A) ion lines by the spectroheliograph RES

Fe XII lines at 195 A resolved by the RES device

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

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

Density diagnostics Diagnostics is based on CHIANTI (http: //www. solar. nrl. navy. mil/chianti. html). 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

Self-consistency check Ratio Te AR 1 29. 12. 2001 AR 2 29. 12. 2001 AR 30. 12. 2001 Fe. XIII 321. 40/320. 81 1. 6 MK 1. 9 e 9 2. 5 e 9 2. 4 e 9 Fe. XIII 312. 87/321. 40 1. 6 MK 1. 9 e 9 3. 4 e 9 2. 5 e 9 Fe. XIII 318. 13/321. 40 1. 6 MK 4. 3 e 9 5. 2 e 9 5. 4 e 9 Fe. XV 307. 75/324. 98 2 MK 3. 9 e 9 4. 4 e 9 No data Fe. XV 327. 03/321. 77 2 MK 1. 7 e 10 1. 13 e 10 Fe. XV 284. 16/307. 75 2 MK Out of range SXI 291. 58/285. 82 2 MK 1. 4 e 9 2. 3 e 9 1. 6 e 9 SXI 291. 58/281. 40 2 MK 1. 7 e 9 1. 8 e 9 SXII 288. 42/299. 54 2 MK 1. 8 e 9 2 e 9 2. 2 e 9 Problem lines: Fe. XIII 318. 13; Fe. XV 327. 03, 284. 16. Adopted lines: Fe. XIII 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.

Preliminary results Log Ne Quiet Sun N 80 -90 E 0 16. 09. 2001 03. 59. 36 AR NOAA 9765 29. 12. 2001 14: 48: 53 Flare M 5. 6 AR 9608 16. 09. 2001 03: 59: 36 8. 7 9. 3 >9. 7 Flare M 7. 6 AR 9628 25. 09. 2001 04: 50: 42 10

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 2 MK 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

Two kinds of diagnostics 1) Ne diagnostics at selected Te 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.

DEM for the active region and the flare 28. 12. 2001

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. Active Region NOAA 9765 Flare X 3. 4 class 28. 12. 2001 (Å) Ion Intensity Error Observ. /Predic. Intensity Error Observ. /Predic. 279. 74 Cr. XXII - - - 365 17 1. 00 (1. 05) 291. 98 Ni. XVIII 816 80 0. 99 (0. 93) 4605 433 1. 05 (0. 74) 292. 49 Fe. XXII - - - 651 18 1. 01 (0. 87) 292. 82 Si IX 288 30 1. 01 (0. 91) 311 14 0. 92 (0. 96) 296. 14 Si IX 483 50 1. 00 (0. 92) 586 13 1. 02 (0. 85) 302. 19 Ca. XVIII 154 20 1. 00 (1. 32) 3212 301 1. 00 (1. 17) 303. 33 Si XI 2800 300 1. 00 (1. 04) 1614 303 1. 00 (1. 51) 315. 02 Mg. VIII 612 60 1. 00 (1. 02) 636 18 1. 00 (1. 17) 320. 57 Ni. XVIII 392 40 1. 01 (0. 96) 1828 261 0. 89 (0. 87)

DEM for different active regions and the flare

SPIDER: 12. 11. 2001(Mg)

2001, November 12 SXT SPIRIT Mg. XII

2001, November 12 1 1 SXT Mg. XII 1 ALL 1 SXT & SPIRIT

SXT+Mg, 12. 11. 2001 (Height)

2001, October 22 SXT SPIRIT Mg. XII

2001, October 22 1 1 2 2 SXT & SPIRIT SXT Mg. XII ALL

SPIDER: 29. 12. 2001(Mg)

SPIDER: 29. 12. 2002 (304, 284, 175, Mg)

The same SPIDER (IAT, 195)

The same SPIDER (IAT+Mg)

Height distribution of line intensities (29. 12. 2001)

Height distribution of the DEM (29. 12. 2001)

GOES data

Spider activity

Comparison of GOES & Mg XII time profiles

Correlation of GOES & Mg. XII fluxes

GOES 1 -8 response ratios

Empirical law

Temporal profiles of emission measure and luminosity

Temporal profiles of emission measure and luminosity

Temporal profiles of emission measure and luminosity

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