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Department of Astronomy, Nanjing University, Nanjing 210093, China

Possible collaboration between Solar-B and the facilities of Nanjing University. C. Fang, M. D. Ding, P. F. Chen. Department of Astronomy, Nanjing University, Nanjing 210093, China. Outline. Observation History in Nanjing University Introduction to the New Telescope

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Department of Astronomy, Nanjing University, Nanjing 210093, China

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

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

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

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

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

  6. New Site: Fuxian Lake Location: E102º57´, N24º38´(60 km from Kunming) Altitude: 1722 mTotal area: 212 km2 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 Λ360.0 nm and 425.0 nm • 200mm 1-4 frames per minute Credit: BBSO

  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 H-1.3 Å Ribbon motion recon. rate Fast fluctuations: elementary bursts Qiu et al. (2004) Wang, H. et al. (2000) 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! • They are short-lived; • Few telescopes tailored for that purpose. Need be checked carefully! Hudson (2005): All flares are WLFs. (Trace …) A catalog including types I & II WLFs (Fang & Ding 1995) will be provided.

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

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

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

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

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

  20. Ellerman Bombs, Microflares, Dark points, Coronal Holes, … EBs, MF Chen et al. (2001, ChJAA, 1, 177) Fang et al. (2006, ApJ, in press) Harvey (1984) DPs 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 10830 SXR CHs

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

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

  23. Introduction ofSMESE(SMall Explorer for Solar Eruptions) A Franco-Chinese small satellite 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

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

  25. Instruments • 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)

  26. Guide Telescope DESIR LYOT HEBS MYRIAD 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 • ONSET can monitor the onset of CMEs, detect various activities with different scales, conduct the H, He and Wight light patrol, …… • SMESE can provide Lyαimages, Lyαcoronagraphs, • EUV images, HXR and γ-ray flux with high temporal • resolution. 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!

  30. 谢 谢！ Thanks！

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