1. SPIRIT observations of the Sun in 175 Å and scientific tasks for SWAP&LYRA V. Slemzin P.N. Lebedev Physical Institute, Moscow

2. Solar activity in 2007/2008 1998/02/01 1998/12/01
Solar events in 1998:
Flares: M X
CMEs
EIT waves: (Mar97-Jun98
Proba 2 launch
EIT 171
EIT 195
EIT 171
EIT 195
1998/02/ /12/01

3. Comparison of CORONAS-F/SPIRIT, EIT and SWAP
Effective area Seff=A*R2*T*Q
(preliminary)
Temperature response
Telescope
λmax
Max Seff, cm2
EIT 171
174
0.0303
EIT 195
190
0.0192
SPIRIT 175
178
SWAP 175
175
0.142

4. For the plasma of active regions (averaged):
FeIX
FeX
FeXI
 ion Iion/total LgT
Fe IX
Fe X
Fe X
Fe X
Fe XI
Fe X
Fe XI
Fe XI
Fe X
Fe XI
Fe VIII
Contributions of hot and cold lines
Fe XX LgT= Flares
O VI LgT=5.5 – CH, QS
CHIANTI ver. 3
For the plasma of active regions (averaged):
Total (LgT<5.8) = Total (LgT > 6.2) = 0.110
ph/pix.s for different solar structures (model estimations)
device λ QS AR FL CH
EIT
195
580
9700 46
SWAP
175
440
4500 96
Contrast in SWAP images will be less than for EIT 195 Å (better for registration)

5. K. J. H. Phillips. The high-temperature response of the TRACE 171 Ả and 195 Ả channels. ApJ, 626:1110–1115, He used the last CHIANTI Ver.5
At T=10 MK (rel. int)
171
Continuum – 0.512
FeXX (173.4 A) , Max at 10 MK
195
Continuum – 0.237
FeXXIV( A) , Max at 20 MK
CaXVII ( A) , Max at 6 MK
171 Å
195 Å

6. Solar corona at 1MK SPIRIT 175 Å EIT 195 Å
Typical heights in 175 <h> ~ Mm (0,03-0,1Rsun )
Contrast is lower, but structures are more distinct (lesser temperature interval)

7. Solar flares X17 flare SPIRIT 175 Å 14 Jun 2003 T=52 s B 13 flare
The 175 Å band has less dynamic range and scattering light from bright flares.
The magnetosphere of the Earth protects from solar energetic particles
SPIRIT 175 Å
12 Jun 2003
T=42 s
C 61 flare
TRACE 171 Å
20 Sep 1998
T~35-47 s
M 18 flare

8. Coronal waves in 175 and 195 Å 28 October 2003 26 October 2003
V~190 km/s
EIT+SPIRIT

9. Coronal Mass Ejections (17-18 November 2003)
Two-color movies (SPIRIT 175/304 Å)
175 – blue, red
Disappearing coronal structures are colored in blue, so they have T ~ 1MK. Are they erupted or expanded into the higher corona? EUV dimmings – primary or secondary phenomena?

10. Large-scale dimmings in 175 Å
Halo CME of October 28, 2003
EIT 284 A
Pearson>0.5
Pearson<0.5
Total dimming Temporal derivative Light curves of dimming regions
projected CME onset

11. Propagation inside extended dimming region
EIT 195 Å
Temporal derivatives of the profiles (- dp/dt)
CME onset
09:02 UT 36
543
1-4 24
376
1-3 12
148
1-2
t, min
L, Mm
box
The speed of dimming propagation is similar to the average speed of EIT wave, but no wave was observed!

12. Events of September 07 and 13, 2005 (no EIT data)
GOES X :40UT
(No CME data)
07/09
13/09
AR 10808
GOES X1.7 23:22 UT
GOES X1.5 19:27 UT
CME onset 19:35:50

13. EUV dimmings: footprints of disappearing trans-equatorial and interconnecting loops (?)
Arguments which confirm association of dimmings with TIL footprints:
Footprints of large magnetic loops are situated inside dimming areas. Wang et al.ApJ 2001, Liu et al. ApJ 2006.
Type II bursts associated with TIL disappearance are located in the vicinity of EUV dimming regions.
Pohjolainen et al. Apj2001, A&A 2005.
3. Starting of dimmings is ahead of EIT and Moreton waves on 0.5-1h, so remote dimmings cannot be created through propagation of surface disturbance.
Problems:
Large loops are not always visible (too hot or too low density?)
Area of dimmings are much larger than TIL cross-section.
The cause of initial brightening in the dimming area is unclear.
The mechanism of dimming propagation may be different.

14. Prominence activation and eruption (2 Dec 2003)
EIT 195 Å/LASCO
SPIRIT 175/304 Å
Hα HACO

15. Heating of the prominence material
10:24:10
T~1MK
175 A
(SPIRIT)
10:23:45

16. EUV solar irradiance from SPIRIT and EIT
Sp175/EIT 195
Sp304/EIT 304
EIT bakeout

17. SPIRIT off-limb measurements
Eruption of Feb 2, 2003
02: : : : :02

18. Attenuation of the total flux (h =10-20 km)
Absorption of solar EUV emission in the Earth’s atmosphere during satellite occultations H
Sun
Earth
telescope
R+h R
Attenuation of the total flux (h =10-20 km)
Height profile from image ratio (h <1 km)

19. Measurements before and during the geomagnetic storm of 23 May 2002
К(h) – extinction coefficient,
T0 – normalizing coefficient
Vertical profile К(h) is retrieved solving the inversion problem
Measurements before and during the geomagnetic storm of 23 May 2002
Profiles Retrieved extinction
(least-squares method)

20. Retrieval of Absorption Profiles in High Atmosphere from Solar Occultation Data
Difference in optical thickness  for two rays with radial distances r0 and rm
The kernel (r) may be found using the Tikhonov method
(r)

21. Solar eclipses Very useful for in-flight calibration (scattered light)!
11 June April 2005

22. Preliminary tasks for SWAP&LYRA from SPIRIT observations
Precursors of X-ray flares and CME in the lower corona. Are the observed features primary or secondary to the main process?
Development of large-scale EUV dimmings and their relationship with coronal (EIT) waves.
Correlations of brightness in 1MK coronal structures. Relationship with global magnetic interconnections.
Variations of total UV/EUV flux with solar activity. Cross-correlations of fluxes in various spectral bands.
Kinematics and heating of eruptive prominences. Relationship between prominence eruption and dimming origination.
Study of response of high atmosphere of the Earth to variations of solar activity. Temporal and spatial dynamics of disturbance dissipation.

23. TESIS telescope-spectroheliometer (CORONAS-Photon mission)
Parameter
Channel
134 А
304 А
Mg1, 2
Spectral band, A
8.418 – 8.423
Field of view
Disk – 35'; Corona – from 2 till 5 Rsun (with mirrors shifting)
45'
Spatial resolution, arc sec 1 2
Spectral resolution, λ/Δλ 10
2×10-4 A/cell
Exposure time, s
Mirrors effective area, cm2
100 60
Detectors: back-side CCD (2048x2048) E2V Co, GB
Soft X-ray Spectrophotometer SphinX
(J. Sylwester, Poland)
E= 0.5 keV– 15 keV, ΔE= eV (256 ch), Δt=0.01 s
Detector: Si (Amtek), dynamic range - 105
CORONAS-PHOTON
Orbit: H=500 km, incl=82.50
Telemetry: X-band radio transmitter set 8.2 GHz
Launch - end of 2007