1. Science Lessons Learned from TESIS and their Relevance to SWAP V. Slemzin, LPI PROBA 2 SWT, La Roche, 14 June 2010

2. TESIS scientific team (LPI): S. Kuzin, S. Bogachev, S. Shestov, V. Slemzin, A. Ulyanov, A. Reva CORONAS-Photon was launched on January 31, 2009 The projected time of the mission was 2 years The flight was terminated after 9 months in November 2009 because of problems with the satellite power system. TESIS

3. Array of TESIS instruments CHANNELS (7) MgXII 8.42 A Telescope 1 132 A FeXX-XXIII Telescope 2 171/304 A FeIX-X / He II CORONO- GRAPH 304ASPECTRO-HELIOGRAPH SphinX photometer SRC PAN Spectral Range, A 8.41- 8.42 131- 132 171-178 295-315 295- 315 285- 335 1-12 Field of View 45’Disk: 1 0 Corona: 2-5 R sun 2.5°~2°- Angular Resolution 3”1.7”20” X: 1.7” Y: 40” - Spectral Resolution 0.0002 A/pixel 7020 0.01 A/pixel~0.05 Exposition, sec 0.01-6000.01- 0.001

4. TESIS: parameters of EUV telescopes  Wavelength band 132 A (telescope I) 171 / 304 A (telescope II)  Focal length……………. 1600 mm  Mirror Aperture…...100 mm diameter  Field of view ……………………... 1°  Angular resolution……1.7 arc sec/pix  Max. cadence…………1 sec (partial frame) 10 sec (full frame) Typical cadence………..2 – 5 min  Detector……….… backside CCD 2048 × 2048 pixels

5. CORONAS-Photon orbit H orb =550-570 km, α = 82 0 Eclipse time for one 95 min orbit

6. TESIS resuls 1. Eruption of giant prominences in 304 A TESIS HeII 304 A 23/04-2009

7. 2. Dynamics of active regions in 171 A

8. 3. Short-time dynamics Nanoflares in 171 A Cadence 3 s, exposure 0.5 s Dynamics of spicules in 304 A

9. 4. Eruption of a giant prominence in 304 A and U-shaped magnetic feature 12 May 2009

10. 4. Quasi-static inner corona in 171 A Overexposure (10 s instead of 0.1s) Low straylight (one-mirror telescope)

11. Coronal dynamics during one solar rotation 1-27 September 2009 N W S E N

12. TESIS lessons  The scientific program was not fulfilled because the mission was terminated in November 2009 due to failure of the satellite power system. Total volume of information: 700 Gb, 150000 images.  In 2009 the solar activity was unexpectedly low. Two high temperature channels did not provide valuable data (Mg, 132 A)  At very low solar activity there are many specific phenomena as global and small scale: eruption of giant prominences, a lot of bright EUV points, rich magnetic structure of the inner corona, reconnection of closed structures with open interplanetary lines.  The 171 A band is very informative to study the inner corona (T ~ 1-2 MK) in global and local scales.  Perspectives: EUV imaging with resolution < 1” and cadence of 1 s (“Arka” project) Level 1 TESIS data are available at http://www.tesis.lebedev.ru/en/data_access.html

13. The inner corona in SWAP 1x10s 100x10s equatorial scan

14. 100x10s N W S E N 1x10s

15. SWAP – LASCO C2