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 500km. 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)

SPIRIT (SPectroheliographIc X-Ray Imaging Telescope) is the current experiment on board the CORONAS-F satellite launched 31 July 2001 (Orayevskii & Sobelman, 2002). The main goal of the experiment SPIRIT is to study a structure and dynamics of solar atmosphere in a wide scale of heights – from the chromosphere to a far corona by the XUV imaging spectroscopy. Since the launch of the

CORONAS-F satellite more than three hundred thousands of images and spectroheliograms were recorded.

Spectral bands of the SPIRIT instrument and excitation temperatures of ions in solar plasma

Spectral band The main emitting ions T, 106 K

8.418 - 8.423 Å MgXII 10 177-207 Å S VIII-XI, Fe VIII-XVII,Ca XIV,XVII, FeXXIV

XXIV 1.3-16

285 - 335 Å HeII, CIV, MgVIII, SiIX-XI, FeXIII-XVII, NiXVIII, Co XVII, CaXVIII, CrXXII, FeXXII

0.05-15

171 ± 3 Å Fe IX –X 1.3

175 ± 5 Å FeX – XI 1.3

195 ± 6 Å FeXII 1.6

284 ± 8 Å FeXV 2

EUV images by SRT device

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

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 177-207A

RES-S spectroheliogram in 285-335A

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 – 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.

Density diagnosticsDensity 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).

Self-consistency checkRatio Te AR 1 29.12.2001 AR 2 29.12.2001 AR 30.12.2001

FeXIII 321.40/320.81 1.6 MK 1.9e9 2.5e9 2.4e9

FeXIII 312.87/321.40 1.6 MK 1.9e9 3.4e9 2.5e9

FeXIII 318.13/321.40 1.6 MK 4.3e9 5.2e9 5.4e9

FeXV 307.75/324.98 2 MK 3.9e9 4.4e9 No data

FeXV 327.03/321.77 2 MK 1.7e10 1.1e10 1.13e10

FeXV 284.16/307.75 2 MK Out of range Out of range Out of range

SXI 291.58/285.82 2 MK 1.4e9 2.3e9 1.6e9

SXI 291.58/281.40 2 MK 1.7e9 1.8e9 1.8e9

SXII 288.42/299.54 2 MK 1.8e9 2e9 2.2e9

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.

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 Ne 8.7 9.3 >9.7 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 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

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 X3.4 class 28.12.2001

(Å) Ion Intensity Error Observ./Predic. Intensity Error Observ./Predic.

279.74 CrXXII - - - 365 17 1.00 (1.05)

291.98 NiXVIII 816 80 0.99 (0.93) 4605 433 1.05 (0.74)

292.49 FeXXII - - - 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 CaXVIII 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 MgVIII 612 60 1.00 (1.02) 636 18 1.00 (1.17)

320.57 NiXVIII 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 MgXII

11 1

1

2001, November 12

SXT & SPIRIT

SXT MgXII ALL

SXT+Mg, 12.11.2001 (Height)

2001, October 22

SXT SPIRIT MgXII

1

2

1 1 1

222

2001, October 22

SXT & SPIRIT

SXT MgXII 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 & MgXII fluxes

GOES 1-8 response ratios

Empirical law

tAtMgXIIIBtGOESI ,,

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