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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. - PowerPoint PPT Presentation
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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)
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