workshop on iter simulation, beijing, 2006 kuafu team various insitituions c.y. tu, s.y. fu...

Workshop on ITER Simulation, Beijing, 2006

KuaFu TeamVarious InsitituionsC.Y. Tu, S.Y. Fu

Institute of Space Physics and Applied TechnologySchool of Earth and Space Sciences

Peking University

KuaFu MissionSolar Storm, Aurora and Space Weather Explorer


Milestones of KuaFu

Jan. 2003---- First proposed by Prof. Chuanyi TuSep. 2003---- Mission is named “KuaFu”……… Presented in many conferences and meetingsSep. 2004---- Supported by CNSF for concept studyDec. 2004---- First group meeting, Frankfurt, GermanyDec. 2004---- Listed in the ILWS-missionsMay 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


General Concept Developing Group

Chuan-Yi Tu Peking University, Beijing, ChinaYong-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, GermanyEric Donovan University of Calgary, Calgary, CanadaEckart Marsch MPS, Lindau, Germany

Zuo Xiao Peking University, Beijing, China Feng-Si Wei Chinese Academy of Sciences, Beijing, China


Space Weather


Our Beautiful Sun


Interaction with the Earth


Sun-Earth System Exploration

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 storm

s 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


Day of Year, Start time 12:00UT,on July15,2000

‘Bastille Day’ event in the year of 2000

Chain of solar terrestrial disturbance

POLAR: New Views of the

Aurora


dimming

blast waveflare

eruption

SOHO/EIT

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?


L1 + Polar Triple Spacecraft Project


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,

Space Weather Science Objectives


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?


1. How does the central plasma sheet (CPS) feeds particles into the ring current? What is the role of sub-storms in storms?

2. 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.

3. 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.

4. KuaFu B integrated imaging provides a natural way to test our modeling capabilities in geo-space science.

Geo-space Science Objectives


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)

KuaFu-A


Lyman-alpha coronagraph 1.1-2.5 Rs

Lyman-alpha Disc imager up to 1.1Rs

White light coronagraph 2.5-15 Rs

A LASCO C2 "running difference" image showing a "halo" CME blast beginning its journey towards Earth on 7 April 1997


Basic Concept of KuaFu-B


Imager1. UV imagers (primarily electron aurora) 24 hours.2. Lyman-alpha imaging spectrograph (24 hours)3. Wide FOV perigee imager for conjugate (perigee) imaging.4. 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)

KuaFu-B


The complete chain of disturbancefrom the solar atmosphere to the geo-space

Lyman αCoronagraph

White Light Coronagraph

Radio Wave measurement

MF, PlasmaHigh energy particle

Auroral image24 hours/day

Ionosphere

Auroral image conjugate

Ground base Auroral measurement

Disk Lyman α chromosphere

Disk 195Ǻ corona

PhenomenaFilament eruptions

Flares CMEs Shock wavesM. Clouds

SubstormPBS

Storm

New science objectives:Precursor of Eruption

Origin and developmentof flares and CMEs

3D geometry expansionof CMEs (synthesized with Solar Orbitor and Sentinels)

Tail Reconnection

Energy sink during storm and substorm

Energetic Neutron Atom(ENA) 24 hours

Kuafu AKuafu B1Kuafu B2

15 Rs2.5 Rs


Possible Synergic Observations with 14 Satellites


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)


Endorsement for KuaFu Payload

"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 …

------ Prof. Dr. Robert F. Wimmer-Schweingruber, University of Kiel


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

Instrument Mass(kg)

PIs

EUV/FUV disk imager (EDI),including a Lyman-alpha disk imager Polarimeter

252

P. Rochus (Belgium)U. Schühle （ Germany ）

Coronal Dynamics Imager (CDI),including a Lyman-alpha coronagraph

45 P. Lamy （ France ）

Radio Burst Instrument (RBI) 11 J.-L. Bougeret （ France)

Solar Wind Instrument Package (SWIP) 67

R. Schwenn K.-H. Glassmeier(Germany)

C.M. Carr （ UK)

Solar Energetic Particle Sensor(SEPS) 6.5 R. Wimmer-Schweingruber （ Germany ）

S.-J. Wang (China ）Hard X-Ray and Gamma-Ray

Spectrometer(HXGR) 4.5 G.-W. Qun （ China ）

Solar Irradiance Measurement (SIM) 13 D.-R. Lü （ China ） W. Schmutz （ Swithzland ）

Multi-Order Solar EUV Spectrograph (MOSES) 10 L. Harra （ UK ） Total 130


L.-D. Xia University of Science and Technology of China (Convener)R. Schwenn Max Planck Institute for Solar System Research, GermanyE. Marsch Max Planck Institute for Solar System Research, GermanyP. Rochus University of Liege, BelgiumP. Lamy Laboratoire d'Astrphysique de Marseille, FranceJ.-L. Bougeret Centre National de la Recherche Scientifique, FranceU. Schühle Max Planck Institute for Solar System Research, GermanyR. Wimmer-Schweingruber Kiel University, GermanyK.-H. Glassmeier Braunschweig University, GermanyC. M. Carr Imperial College London, United KindomW.-Q. Gan Chinese Academy of Sciences, ChinaJ. Chang Chinese Academy of Sciences, ChinaS.-J.Wang Chinese Academy of Sciences, China

KuaFu-A Group


Instrument Mass(kg) Power(W) Proposal PI

Far Ultraviolet Auroral Monitoring Camera (UVAMC)

21 11Canada

E. DonovanT. S. Trondsen

FUV Imaging Spectrometer (FUVSI) 20 4.4 Belgium C. Jamar

Wide Field Auroral Imager (WFAI) 1.5 10 UK M. Lester

Fluxgate Magnetometer (FGM) 3 4.25 Austria T.-L. Zhang

High Energy Charged Particle Experiment(HECPE)

3 4China H. F. Chen

Medium-Energy Particle Imager (IEPS)

5.6 4.5UK/China

M. Dunlop/H.F. Chen

Neutral Atom Imager on KuaFu (NAIK)

6 4 Ireland/China

S. McKenna-Lawlor

Fast Plasma Pitch angle Anylazer (FPI)

6 10 UK A. Fazakerley

Ion Mass Spectrometer(IMS) 3.5 2.5 France H. Reme

Tri-Band Beacon (TBB) 3.5 1 China J. Wu

Total 73 ~56

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


KuaFu-B Group Jing-Song Wang Peking University, China (Convener)E. Donovan University of Calgary, CanadaTrond S. Trondsen University of Calgary, CanadaM. Lester Leicester University, United KindomT. –L. Zhang Austrian Academy of Sciences, AustriaS. McKenna-Lawlor National University of Ireland, IrelandM. Dunlop Rutherford Appleton Laboratory, United KindomC. Jamar University of Liege, BelgiumS.-Y. Fu Peking University, ChinaH.-F. Chen Peking University, ChinaL. Xie Peking University, ChinaJ. Wu China Research Institute of Radiowave Propagation, ChinaD.-H. Zhang Peking University, China


Where are we now?

The "comprehensive review" of the KuaFu project supported by CNSA started beginning 2006………… Launch in 2012 ( SolarMax)


Stamp Published on Sept 25th,1987,by Beijing Stamp Printers.

One day Mr. KuaFu tried 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)."

KuaFu-An ancient Chinese myth

workshop on iter simulation, beijing, 2006 kuafu team various insitituions c.y. tu, s.y. fu...

Documents

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