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

Solar activity in 2007/2008 1998/02/01 1998/12/01 Solar events in 1998: Flares: M - 94 X - 14 CMEs - 700 EIT waves: 173 (Mar97-Jun98 Proba 2 launch EIT 171 EIT 195 EIT 171 EIT 195 1998/02/01 1998/12/01

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 0.00668 SWAP 175 175 0.142

For the plasma of active regions (averaged): FeIX FeX FeXI  ion Iion/total LgT 171.073 Fe IX 0.348 5.9 174.534 Fe X 0.147 6.0 175.266 Fe X 0.045 6.0 177.243 Fe X 0.087 6.0 179.764 Fe XI 0.017 6.1 180.407 Fe X 0.132 6.0 181.137 Fe XI 0.014 6.1 182.169 Fe XI 0.034 6.1 184.543 Fe X 0.038 6.0 184.803 Fe XI 0.010 6.1 185.213 Fe VIII 0.023 5.6 Contributions of hot and cold lines 173.405 Fe XX LgT=7.0 - Flares 173.080 O VI LgT=5.5 – CH, QS CHIANTI ver. 3 For the plasma of active regions (averaged): Total (LgT<5.8) = 0.086 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 1.8.106 46 SWAP 175 440 4500 1.2.105 96 Contrast in SWAP images will be less than for EIT 195 Å (better for registration)

K. J. H. Phillips. The high-temperature response of the TRACE 171 Ả and 195 Ả channels. ApJ, 626:1110–1115, 2005. He used the last CHIANTI Ver.5 At T=10 MK (rel. int) 171 Continuum – 0.512 FeXX (173.4 A) - 0.413, Max at 10 MK 195 Continuum – 0.237 FeXXIV(192.02 A) - 0.461, Max at 20 MK CaXVII (192.82 A) 0.278, Max at 6 MK 171 Å 195 Å

Solar corona at 1MK SPIRIT 175 Å EIT 195 Å Typical heights in 175 <h> ~ 20-70 Mm (0,03-0,1Rsun ) Contrast is lower, but structures are more distinct (lesser temperature interval)

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

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

Coronal Mass Ejections (17-18 November 2003) Two-color movies (SPIRIT 175/304 Å) 175 – blue, 304 - 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?

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

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!

Events of September 07 and 13, 2005 (no EIT data) GOES X17.0 17:40UT (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

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.

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

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

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

SPIRIT off-limb measurements Eruption of Feb 2, 2003 02:55 04:07 04:28 05:41 06:02

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)

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)

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)

Solar eclipses Very useful for in-flight calibration (scattered light)! 11 June 2002 8 April 2005

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.

TESIS telescope-spectroheliometer (CORONAS-Photon mission)   Parameter Channel 134 А 304 А Mg1, 2 Spectral band, A 132 - 136 295 - 315 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 0.01 - 600 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=150-190 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