Science Lessons Learned from TESIS and their Relevance to SWAP

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

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 Eclipse time for one 95 min orbit Horb =550-570 km, α = 820

6. TESIS resuls1. 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 rotation1-27 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. 1x10s N W S E N 100x10s

15. SWAP – LASCO C2