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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 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 Solar Tower (since 1980) Multi-wavelength 2-Dimensional Spectrograph H Ca II (K, 8642) He I 10830 Highlights of the Achievements 1. 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 From Nanjing to Kunming 31.8 km Fuxian Lake 撫仙湖 New Site: Fuxian Lake Location: E102º57´, N24º38´ (60 km from Kunming) Altitude: 1722 m Total area: 212 km2 Second deepest lake in China, mean depth is 87m. Main Components Three Tubes H 6563 He I 10830 White light Designed by NIAOT Name of the Telescope ONSET: Optical and NIR Solar Eruption Tracer H Filtergraph H center, ±0.5 Å 275mm 1-120 frames per minute Credit: BBSO He I 10830 Filtergraph He I 1083.0nm center 275mm 1 frame per minute Credit: MLO White Light Filtergraph Λ360.0 nm and 425.0 nm 200mm 1-4 frames per minute Credit: BBSO 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, … Flare Ribbons and Dynamics H-1.3 Å Ribbon motion recon. rate Qiu et al. (2004) Fast fluctuations: elementary bursts Wang, H. et al. (2000) To derive non-thermal parameters and dynamical processes of flares through ground-based and space observations! White Light Flare Patrol Since 1859, only ~110 WLFs have been observed. 1. They are short-lived; 2. Few telescopes tailored for that purpose. Hudson (2005): All flares are WLFs. (Trace …) A catalog including types I & II WLFs (Fang & Ding 1995) will be provided. Flare-associated Sprays, Surges, … H center, ±0.5 Å Kurokawa et al. (1987) left-handed right-handed Jibben & C. Canfield (2004) Handedness distribution, Helicity transport, … Filament Eruptions near CME Onset H center, ±0.5 Å Morimoto & Kurokawa (2003) LOS velocity 1. To monitor the onset of filament eruptions; Chen & Shibata (2000) Zhang et al. (2001) 2. To clarify the relationship btw CMEs and flares. CME-associated Waves/Brightenings EIT waves Thompson et al. (1998) He waves Gilbert et al. (2004) Coronal waves Harra & Sterling (2003) Moreton Waves Chen et al. (2002, ApJ, 572, L99) H+0.8Å Credit: Kyoto University colleagues H ± 0.4 Å may be the best Chen, Fang, Ding (2005, Space Sci. Rev.) Ha+0.4 Å Ha-0.4 Å Moreton, EIT, X-ray and He Waves will be recorded, which is crucial for understanding CMEs 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) 250 km/s 775 km/s Coordinated observations will finally resolve the dispute Ellerman Bombs, Microflares, Dark points, Coronal Holes, … EBs, MF Chen et al. (2001, ChJAA, 1, 177) Harvey (1984) DPs He 10830 CHs Fang et al. (2006, ApJ, in press) SXR 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 Filament Oscillations -0.8 Å H core +0.8 Å Eto et al. (2002) Prominence seismology will be enhanced! 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 Introduction of SMESE (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 Main Scientific Objectives To observe the solar flares and CMEs for the next solar maximum 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) SMESE Payload Guide Telescope DESIR LYOT HEBS MYRIAD 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 Prospects Coordinated observations with solar-B will greatly contribute to the study of solar flares and CMEs Summary 1. ONSET can monitor the onset of CMEs, detect various activities with different scales, conduct the H, He and Wight light patrol, …… 2. 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! 谢 谢! Thanks!