KuaFu Team Various Insitituions C.Y. Tu, S.Y. Fu

1. KuaFu Mission Solar Storm, Aurora and Space Weather Explorer KuaFu Team Various Insitituions C.Y. Tu, S.Y. Fu Institute of Space Physics and Applied Technology School of Earth and Space Sciences Peking University

2. Milestones of KuaFu • Jan. 2003---- First proposed by Prof. Chuanyi Tu • Sep. 2003---- Mission is named “KuaFu” • ……… Presented in many conferences and meetings • Sep. 2004---- Supported by CNSF for concept study • Dec. 2004---- First group meeting, Frankfurt, Germany • Dec. 2004---- Listed in the ILWS-missions • May 2005---- First international workshop on KuaFu, Beijing. • Sep. 2005---- Selected as the potential space mission by CNSA. • Jan. 2006---- First science working group meeting in MPS, Lindau, Germany

3. General Concept Developing Group Chuan-Yi Tu Peking University, Beijing, China Yong-Wei Zhang DFH Satellite Co. LTD, Beijing, China Jing-Song Wang Peking University, Beijing, China （China Meteorological Administration） Li-Dong Xia U. Science and Technology of China, Hefei, China Rainer Schwenn MPS, Lindau, Germany Eric Donovan University of Calgary, Calgary, Canada Eckart Marsch MPS, Lindau, Germany Zuo Xiao Peking University, Beijing, China Feng-Si Wei Chinese Academy of Sciences, Beijing, China

4. Space Weather

5. Our Beautiful Sun

6. Interaction with the Earth

7. 1. The first step is to find the composition of the Sun-Earth system. Photosphere, corona, solar wind, magnetic cloud, bow shock, magnetopause, plasma sheet, etc. This cartography is largely done. 2. The second step is to observe the correlations and interactions between two phenomena, between CME and Flare, magnetic cloud and sub-storm, et al. 3. The third step is to explore the complex global behavior. The space storms, such as CMEs and sub-storm and magnetic storms are all multiscale phenomena, i.e., interactions occur simultaneously on several distinct scales. KuaFu Mission concentrates on exploring the complex global behavior of the Sun- Earth system Sun-Earth System Exploration

8. Chain of solar terrestrial disturbance ‘Bastille Day’ event in the year of 2000

9. Possible Precursors of CME • What are the real prosses between these precursors and CMEs? • How does CMEs propergate in the interplanetary space? • What is the geo-effect of CMEs? Can we forcast the space weather? blast wave flare dimming eruption SOHO/EIT

10. L1 + Polar Triple Spacecraft Project

11. Space Weather Science Objectives • To observe continually the complete chain of actions/reactions from the solar atmosphere to geo-space • : • Solar Source of the disturbances • Solar flares, CMEs, Energetic particles • Transportation of the disturbances • interplanetary clouds, radio waves, • shock waves, solar energetic particles • Geo-effectiveness • aurora activities, sub-storms, • magnetic storms,

12. Solar Science Objectives • How is the mass supplied to CMEs? • How is the mass supplied to the solar wind? • How is the mass supplied from the cromosphere to the corona? • What are the precursors of CMEs? • How is the relation between flares and CMEs? • How are the CMEs accelerated? • How the mass losses from the corona?

13. Geo-space Science Objectives • How does the central plasma sheet (CPS) feeds particles into the ring current? What is the role of sub-storms in storms? • Pole-ward boundary intensifications (PBIs) simultaneously in the conjugate hemispheres will give information on time and location of reconnection and also the rates and the associated plasma flows. • The energy flux of electrons and protons can be obtained. The source/sink monitoring by KuaFu allows quantitative assessment of geo-effectiveness that is otherwise impossible. • KuaFu B integrated imaging provides a natural way to test our modeling capabilities in geo-space science.

14. KuaFu-A • Imaging the Source region • Solar EUV emission (195A) • Lyman-alpha Disc imager up to 1.1Rs • Tracing the CMEs, etc • Lyman-alpha coronagraph 1.1-2.5 Rs • White light coronagraph 2.5-15 Rs • Radio wave measurement (1Rs-L1) • In situ • Local plasma and magnetic field (L1) • High energy particles (L1)

15. A LASCO C2 "running difference" image showing a "halo" CME blast beginning its journey towards Earth on 7 April 1997 Lyman-alpha Disc imager up to 1.1Rs Lyman-alpha coronagraph 1.1-2.5 Rs White light coronagraph 2.5-15 Rs

16. Basic Concept of KuaFu-B

17. KuaFu-B • Imager • UV imagers (primarily electron aurora) 24 hours. • Lyman-alpha imaging spectrograph (24 hours) • Wide FOV perigee imager for conjugate (perigee) imaging. • Energetic Neutral Atoms (ENA) imager for ring current • observations (24 hours). • In situ • 5. Fluxgate Magnetometer ( FGM). • 6. High energy proton observations (HEPS) • 7. Plasma Spectrometer(FPI/IMS)

19. The complete chain of disturbance from the solar atmosphere to the geo-space Disk Lyman α chromosphere Disk 195Ǻ corona MF, Plasma High energyparticle Auroral image 24 hours/day Ionosphere Kuafu A Kuafu B1 Kuafu B2 2.5 Rs 15 Rs Lyman α Coronagraph White Light Coronagraph Radio Wave measurement Energetic Neutron Atom (ENA) 24 hours Auroral image conjugate Ground base Auroral measurement Phenomena Filament eruptions Flares CMEs Shock waves M. Clouds Substorm PBS Storm New science objectives: Precursor of Eruption Origin and development of flares and CMEs Tail Reconnection Energy sink during storm and substorm 3D geometry expansion of CMEs (synthesized with Solar Orbitor and Sentinels)

21. Possible Synergic Observations with 14 Satellites

22. Review of the Assessment Report The overall mission report achieved a simple average score of 3.3 out of a maximum of 4.0. (4 – excellent, 3 – very good)--- William Liu(Chair ILWS Steering Committee)

23. "The SSWG (Solar System Working Group, ESA) found the described mission concept is good and noted a widespread interest within the relevant scientific community in Europe. The SSWG therefore endorses payload participation by national agencies in this mission … Endorsement for KuaFu Payload ------ Prof. Dr. Robert F. Wimmer-Schweingruber, University of Kiel

24. Payload of KuaFu-A (updated in Jan. 2006)

25. KuaFu-A Group L.-D. Xia University of Science and Technology of China (Convener) R. Schwenn Max Planck Institute for Solar System Research, Germany E. Marsch Max Planck Institute for Solar System Research, Germany P. Rochus University of Liege, Belgium P. Lamy Laboratoire d'Astrphysique de Marseille, France J.-L. Bougeret Centre National de la Recherche Scientifique, France U. Schühle Max Planck Institute for Solar System Research, Germany R. Wimmer-Schweingruber Kiel University, Germany K.-H. Glassmeier Braunschweig University, Germany C. M. Carr Imperial College London, United Kindom W.-Q. Gan Chinese Academy of Sciences, China J. Chang Chinese Academy of Sciences, China S.-J.Wang Chinese Academy of Sciences, China

26. Payload of KuaFu-B (updated in Jan. 2006)

27. KuaFu-B Group Jing-Song Wang Peking University, China (Convener) E. Donovan University of Calgary, Canada Trond S. Trondsen University of Calgary, Canada M. Lester Leicester University, United Kindom T. –L. Zhang Austrian Academy of Sciences, Austria S. McKenna-Lawlor National University of Ireland, Ireland M. Dunlop Rutherford Appleton Laboratory, United Kindom C. Jamar University of Liege, Belgium S.-Y. Fu Peking University, China H.-F. Chen Peking University, China L. Xie Peking University, China J. Wu China Research Institute of Radiowave Propagation, China D.-H. Zhang Peking University, China

28. Where are we now? • The "comprehensive review" of the KuaFu project supported by CNSA started beginning 2006 • …… • …… • Launch in 2012 ( SolarMax)

29. KuaFu-An ancient Chinese myth One day Mr.KuaFutried to catch up with the sun and to enter into it. As he was terribly thirsty, he went to drink in the Yellow River and the Wei River ,but the water in the two rivers was not enough for him, so he turned northward to the sea. Before he could reach there he died of thirst. And his stick was lost in the wild field and it grew up into a forest (Deng-Lin)." Stamp Published on Sept 25th,1987, by Beijing Stamp Printers.