1. Department of Astronomy, Nanjing University, Nanjing 210093, China C. Fang, M. D. Ding, P. F. Chen Possible collaboration between Solar-B and the facilities of Nanjing University

2. Outline 1.Observation History in Nanjing University 2.Introduction to the New Telescope 3.Scientific Objectives and Possible Collaborations 4.SMESE- a Franco-Chinese Small Satellite 5.Summary

3. Solar Tower (since 1980) Multi-wavelength 2-Dimensional Spectrograph H  Ca II (K, 8642) He I 10830

4. Highlights of the Achievements 1.More accurate atmospheric models for solar flares Liu, Ding, Fang, : 2001, ApJ, 563, L169 Li & Ding, 2004, ApJ, 606, 583 2. A near infrared WLF 3. Nonthermal signatures Ding & Fang: 1995, A&AS, 563, L169

5. From Nanjing to Kunming Fuxian Lake 撫仙湖 31.8 km

6. New Site: Fuxian Lake Location: E102º57´, N24º38´ (60 km from Kunming) Altitude: 1722 m Total area: 212 km 2 Second deepest lake in China, mean depth is 87m.

7. Main Components Three Tubes  H  6563  He I 10830  White light Designed by NIAOT

8. Name of the Telescope ONSET: Optical and NIR Solar Eruption Tracer

9. H  Filtergraph H  center, ±0.5 Å  275mm 1-120 frames per minute Credit: BBSO

10. He I 10830 Filtergraph He I 1083.0nm center  275mm 1 frame per minute Credit: MLO

11. White Light Filtergraph  200mm 1-4 frames per minute Credit: BBSO Λ 360.0 nm and 425.0 nm

12. Scientific Objectives and Possible Collaborations Flare dynamics H  and high-T flares, WLF patrol, … CME onset and wave survey He wave/brightening, Moreton waves, EIT wave, filament eruptions, … Structures and evolution of various activities Coronal holes, small activities, microflares, filament oscillation, …

13. Flare Ribbons and Dynamics Ribbon motion  recon. rate Fast fluctuations: elementary bursts Wang, H. et al. (2000) H  -1.3 Å Qiu et al. (2004) To derive non-thermal parameters and dynamical processes of flares through ground-based and space observations!

14. White Light Flare Patrol Since 1859, only ~110 WLFs have been observed. There should be more! 1.They are short-lived; 2.Few telescopes tailored for that purpose. Hudson (2005): All flares are WLFs. (Trace …) Need be checked carefully! A catalog including types I & II WLFs ( Fang & Ding 1995 ) will be provided.

15. Flare-associated Sprays, Surges, … Kurokawa et al. (1987) Jibben & C. Canfield (2004) Handedness distribution, Helicity transport, … right-handed left-handed H  center, ±0.5 Å

16. Filament Eruptions near CME Onset H  center, ±0.5 Å LOS velocity Morimoto & Kurokawa (2003) Chen & Shibata (2000) Zhang et al. (2001) 1.To monitor the onset of filament eruptions; 2.To clarify the relationship btw CMEs and flares.

17. CME-associated Waves/Brightenings He waves Gilbert et al. (2004) EIT waves Thompson et al. (1998) Coronal waves Harra & Sterling (2003)

18. Moreton Waves H  +0.8 Å Credit: Kyoto University colleagues Ha+0.4 Å Ha-0.4 Å H  ± 0.4 Å may be the best Chen, Fang, Ding (2005, Space Sci. Rev.) Chen et al. (2002, ApJ, 572, L99) Moreton, EIT, X-ray and He Waves will be recorded, which is crucial for understanding CMEs

19. Dispute on EIT wave mechanism Fast-mode wave model Non-wave model Thompson et al. (1998) Wang, Y. -M. (2000) Wu et al. (2001) …… Delannee & Aulannier (2000) Chen et al. (2002, ApJ, 572, L99) 775 km/s 250 km/s Coordinated observations will finally resolve the dispute

20. Ellerman Bombs, Microflares, Dark points, Coronal Holes, … EBs, MF CHs DPs Harvey (1984) Chen et al. (2001, ChJAA, 1, 177) Coordinated observations with SOT, XRT and EIS will be very useful to understand the mechanism for small scale activities and magnetic reconnection in the solar atmosphere and the source of the fast solar wind He 10830SXR Fang et al. (2006, ApJ, in press)

21. Filament Oscillations Eto et al. (2002) -0.8 Å H  core +0.8 Å Prominence seismology will be enhanced!

22. Operations Partner in construction and operations: YNO: NAOC/ Yunnan Observatory Commencement: 2008 Data Policy: open Observation Modes  Partial Disk Mode (PDM, better than 1“, FOV:10’)  Full Disk Mode (FDM)

23. Introduction of SMESE ( SMall Explorer for Solar Eruptions ) Institut d ’ Astrophysique Spatiale, CNRS, France Observatoire de Paris, LESIA, France Purple Mountain Observatory, CAS, China Nanjing University, China Center for Space Research and applied Research, CAS, China National Astronomical Observatory, CAS, China A Franco-Chinese small satellite

24. To observe the solar flares and CMEs for the next solar maximum Main Scientific Objectives

25. Lyman-alpha disc imager (up to 1.15R ¤ ) Lyman-alpha coronograph (1.1-2.5R ¤ ) EUV (FeXII 19.5 nm) disc imager Far Infrared telescope (35 & 150  m) X-ray spectrometer (10-300 keV) Gamma-ray spectrometer (0.2-600 MeV) Instruments

26. MYRIAD DESIR LYOT HEBS Guide Telescope SMESE Payload

27. Main parameters  Total weight of payloads: 56 kg  Total power consumption: 90 watt  Data rate: 31Gb per day  Dawn-dusk sun-synchronous orbit  Altidute: 700 Km  Launch time: 2010 - 2011

28. Prospects Coordinated observations with solar-B will greatly contribute to the study of solar flares and CMEs

29. Summary 1.ONSET can monitor the onset of CMEs, detect various activities with different scales, conduct the H , He and Wight light patrol, …… 3. Coordinated observations with SOT, XRT and EIS will be greatly desirable! 4. Data center will be installed in Nanjing University and IAS in France. You are encouraged to use the data! 2.SMESE can provide Lyαimages, Lyαcoronagraphs, EUV images, HXR and γ-ray flux with high temporal resolution.

30. 谢 谢！ Thanks ！