1. Science and Space Weather Opportunities for PROBA2 M. Dominique STCE meeting, May 31 2012

2. Generalities Date: May 04, 2012 – consecutively to A. BenMoussa’s degradation meeting One of the bi-annual PROBA2 science working team meetings Meeting partners from the new eHeroes FP7 project (informal kick-off of WP5) About 40 international participants from: Belgium, France, Ireland, Switzerland, Poland, Italy, Russia, India, USA …

3. Generalities Goals: Discuss the status of the on-going science with SWAP and LYRA on-board PROBA2 + present the achievements Give an overview of the possibilities with PROBA2 to our colleagues from the other institutes … and benefit from their expertise Identify new topics to investigate Establish collaborations with other instrument teams, institutes … Set up joint campaigns for observing unusual events

4. http://proba2.sidc.be/Presentations/20120503_04-ROB-PROBA2days/

5. First part: effect of particles on space-born instruments Increase the noise Induce long term degradation Affect the electronics

6. First part: effect of particles on space-born instruments Effects on six instruments: CORONAS-F/Resik CORONAS- PHOTON/SphinX SDO/EVE SOHO/SEM PROBA2/SWAP PROBA2/LYRA Which particles involved ? Potential long term impact ? How to exploit the information from various instruments ? Topic addressed by WP5 in the new PF7 project eHeroes

7. Second part: science with PROBA2 Long term solar irradiance Flares Coronal seismology with SWAP and LYRA EUV waves Bright points

8. Long term solar irradiance Two EUV channels of LYRA Cross-comparison with SDO/EVE, TIMED/SEE, and SOHO/SEM Impact of channel 3 degradation

9. Solar flares with LYRA: Ly- α flare Ly-  has twice the emission in GOES 0.1-0.8nm It shows a radiative loss between 7 10 24 erg/s and 1.4 10 25 erg/s (same order as SEM 30.4 nm, factor 10 with SEM 0.1-50nm and with GOES). LYRA probably underestimates the Ly-  flare flux due to its large pass- bands (a factor10 at most). The Ly-  emission alone is small wrt to the total energy release.

10. Solar flares with LYRA: QPP QPP = quasi-periodic pulsations of solar irradiance observed during the onset of solar flares Periods of about 10 sec and 2 min detected in LYRA Comparison with other instruments: time delays between EUV and soft X- ray in the 2-30 s range.

11. Helio-seismology with SWAP and LYRA SWAP (unused so far in this context): can be used for seismology of transverse oscillations of long loops. SWAP: seismology of slow waves? LYRA (first results already published – huge potential due to its high cadence): seismology of quasi-periodic pulsations (QPP) in flares. LYRA: statistical study of disk-averaged oscillations?

12. Joint observation of EUV waves Proba-2/SWAP: off-pointing capabilities and high-cadence observation (100s) Hinode: XRT used to identify flare in target active region, triggering EIS EIS used to get spectroscopic observations of “EUV Wave” pulse SDO/AIA: High-resolution, high- cadence observations of the low corona Work in progress

13. Bright points Bright points are small active regions Intensity of bright points fluctuates, which may be due to Periodic reconnection Magnetoacoustic waves

14. Third part: occasional campaigns Presentation on the comet Lovejoy and the Sungrazers Program for a joint observation of the Venus Transit of June 5-6.

15. Conclusion The meeting was successful, with an important participation Most of our objectives have been met The collaborative work is to be continued, with international partners, as well as with very local ones A meeting between ROB and BISA about the impact of particles on PROBA2 is planned for tomorrow …

16. Thanks!