IAGA Huang

Solar and Space Progress in China associated with IHY : 

Solar and Space Progress in China associated with IHY Xueshang Feng1& Fengsi Wei1 Guangli Huang2, Mei Zhang3 & Yihua Yan3 1. Lab. for Space Weather, Center for Space Science and Applied Research, CAS, Beijing, China 2. Purple Mountain Observatory, CAS, Nanjing, China 3.   National Astronomical Observatories, CAS Beijing, China

Optical and Radio Telescopes in Huairou Station (http://sun.bao.ac.cn/smct/intro_smct2_e.html) (http://srg.bao.ac.cn/radiospectr.html): 

Optical and Radio Telescopes in Huairou Station (http://sun.bao.ac.cn/smct/intro_smct2_e.html) (http://srg.bao.ac.cn/radiospectr.html) optical radio Huairou Reservoir

Solar Telescopes in Yunnan Astronomical Observatory (http://www.ynao.ac.cn): 

Solar Telescopes in Yunnan Astronomical Observatory (http://www.ynao.ac.cn)

Solar Telescopes in Purple Mountain Observatory (http://www.pmo.ac.cn): 

Solar Telescopes in Purple Mountain Observatory (http://www.pmo.ac.cn) Purple Mountain Observatory

News 1: French-Chinese Project (SMESE) small satellites for exploring solar eruptions (http://www.pmo.ac.cn): 

News 1: French-Chinese Project (SMESE) small satellites for exploring solar eruptions (http://www.pmo.ac.cn) Payload (69 kg): Lyman-alpha Heliograph, 121nm, 1.1 R, 27 kg EUV Heliograph, 195 Å, 1.4 R, 27 kg Lyman-alpha Coronagraph, 1.15-2.5 R, 27 kg IR Telescope, 150-35 μm, full Sun, 10 kg X-ray Spectrograph, 1-500 keV, 5%, 5 kg γ-ray Spectrograph, 300 keV-600 MeV, 7%, 27 kg Scientific Objectives: BOTH of Flares and CMEs Proposal in 2005, Phase A in 2006, Launch in 2010

News 2: 1-m IR Solar Telescope in YNAO (http://www.ynao.ac.cn): 

News 2: 1-m IR Solar Telescope in YNAO (http://www.ynao.ac.cn) Located in Fuxian Lake near by Kunmin Wavelength: 0.3-2.5 μm Resolution: 0.3 arcsec Accuracy: 10-4 Stokes Open in 2006

News 3: Chinese Solar Radio Heliograph(http://srg.bao.ac.cn/radiospectr.html): 

News 3: Chinese Solar Radio Heliograph (http://srg.bao.ac.cn/radiospectr.html) Location: near by Beijing (NAO) Freq resolution: 30 MHz (1-5 GHz) 100 Hz (5-15 GHz) Space resolution: 1.3-20 arcsec Time resolution: 100 ms Antennas: 100 0f 3-m, 3km baseline Progress: 2 elements in 2005 100 elements in 2007. Exp Sun

Solar Research Groups in China: 

Solar Research Groups in China Solar Spectrograph, Prof. Fang C., Nanjing University Huairou Station (optical), Dr. Zhang H.Q., NAOs Huairou Station (radio), Dr. Yan Y.H., NAOs Solar Magnetism and Activity, Dr. Zhang J., NAOs Solar Predictions, Dr. Wang H.N., NAOs Solar Eruptions and CMEs, Dr. Lin J., YNAO/NAOs Solar High-Energy Physics, Dr. Gan W.Q., PMO Solar Activities, Dr. Huang G.L., PMO Plasmas in the Sun and Solar System, Dr. Wu D.J., PMO

The magnetic evolution of the Sun and the helioshere: 

The magnetic evolution of the Sun and the helioshere The ratio of magnetic shear and current helicity provides information on the non-potentiality of solar flare-producing regions (Zhang, et al., MNRAS, 2001; 2002; ApJL, 2001) The solution of a local parameter λ is justified and applied for a closed-form non-constant-α force-free field with finite energy content in free space around the Sun (Yan et al., ApJL, 2001; Space Sci. Rew., 2003; Li et al., MNRAS, 2004) The mapping of circular polarization in a filament may provide a supplementary diagnosis of the filament magnetic field, in addition to the mapping of linear polarization via the Hanle effect (Wang et al., Solar Phys., 2003)

The initiation of transient events (flares and CMEs - observations): 

The initiation of transient events (flares and CMEs - observations) The initial disturbance in the filament and the initial brightening around the filament took place at the cancellation sites. The repeated flare-CME activities are triggered by the continuous emergence of moving magnetic features (Zhang et al., ApJ, 2001a,b, 2002; Song et al., Solar Phys., 2003) High-cadence and high-resolution time sequences of far H-alpha off-band images provide a unique tool to study the evolution of the fine structure of flare kernels (Ji et al., ApJ, 2003, 2004) The radio signature of magnetic reconnection is obtained, such as the bi-directional type III drift pairs and type II-like, and the twisted magnetic ropes (Huang et al., New Astronomy, 2003; Solar Physics, 2003; JGR, 2004)

The initiation of transient events (flares and CMEs - theories): 

The initiation of transient events (flares and CMEs - theories) When the reconnection-favored emerging flux appears either within or on the outer edge of the filament channel, the flux rope would lose its equilibrium. A piston-driven shock is formed along the envelope of the expanding CME. The legs of the shock may produce Moreton waves. A slower moving wavelike structure, with an enhanced plasma region ahead, corresponds to observed EIT waves (Chen et al., EP&S, 2001; AdSpR, 2002; ApJ, 2002). Solar observations show that magnetic reconnection can occur in the weakly ionized lower atmosphere. 2 and 3-D solutions of steady state magnetic reconnection derived in incompressible, partially ionized plasmas (Ji et al., Solar Physics, 2001; ApJ, 2001a,b).

The acceleration and propagation of solar energetic particles: 

The acceleration and propagation of solar energetic particles The emissions in the wings of H-alpha exhibit fast fluctuations, related to small-scale injection of high-energy electrons (Fang et al., IAU Symp219, 2003; Ding et al., ApJ, 2001; 2002; Liu et al., ApJL, 2001). 54 BATSE/CGRO hard X-ray events are fitted by power-law electrons with a lower energy cutoff from 45 to 97 keV (Gan et al., ApJ, 2001; Solar Phys, 2002; CJAA, 2002). The low cutoff energy are estimated in two solar microwave and hard X-ray bursts (Huang et al., New Astron, 2004). Three very hard photon spectra of Yohkoh/HXT events may result from superposition of a strong Compton backscattering component. The joint effects of Compton backscattering and low-energy cutoff are calculated. (Zhang&Huang, ApJL, 2003; Solar Phys, 2004) .

The processes responsible for heating the different types of the corona: 

The processes responsible for heating the different types of the corona In a low-β plasma such as coronal holes, kinetic dissipation of Alfvén waves can directly lead to electron heating. In the main body of the dense plume, which is embedded in a uniformly magnetized coronal hole, the dissipation of the wave energy can provide an additional local electron heating that is enough to balance the extra radiative loss of the dense bright plume (Wu et al., ApJ 2003) . A dissipative nonlinear inertial Alfvén wave is proposed as the formation of the strong electric spikes in the auroral ionosphere and magnetosphere as well as the field_aligned electron acceleration. The effective acceleration region for auroral electrons with energies of the order of keV (Wu et al., Physical Review E, 2003; JGR, 2004).

The energy transport mechanisms from the solar interior: 

The energy transport mechanisms from the solar interior Under solar interior conditions, the equation of state of the thermodynamic functions of partly ionized and weakly coupled plasmas includes a detailed account of electron degeneracy, Coulomb coupling and pressure ionization (Bi et al., A&A, 2000a,b) The turbulent viscosity exerts a non-negligible influence on the solar p-mode oscillations (Bi et al., A&A, 2000). For the radial modes we find that the Reynolds stress produces signification modifications in structure and p-mode spectrum (Bi et al., ApSS, 2003). The mode frequency is sensitive to the effect of magnetic fields, it can be used as a diagnostic tool for the presence of turbulent magnetic fields in the convection zone (Bi et al., A&A, 2000)

Solar Predictions: 

Solar Predictions Long-term predictions The asymmetry of solar active prominences, sunspot groups in different latitudes and hemispheres (Li et al., ApJ, 2001; New Astronomy 2003; Solar Physics, 2002, 2003) Short-term predictions Some important parameters, such as vertical currents, current helicity, magnetic separatrix, position of singular points are related to pre-status of solar events (Wang et al., 34th COSPAR Scientific Assembly, 2002) Area, magnetic class, net magnetic flux, Carrington longitude and tilt angle of AR may serve to predict the AR producing hazarded space weather (Tian et al., Solar Phys, 2002; 2003; A&A, 2003a,b)

SPACE OBSERVATION IN CHINA —— several examples: 

SPACE OBSERVATION IN CHINA —— several examples The ionosonde and digisonde Chain consists of Mohe, Beijing, Xinxiang, Wuhan, Hainan and Zhongshan stations. This chain is being constructed and improved Recorded data and inverted electron density profile at Hainan station

The Laser-lidar Chain: 

The Laser-lidar Chain Consists of Beijing, Wuhan, Hainan and Antarctic Zhongshan stations and is being constructed. Some trial observations of Laser-lidar have been made in Wuhan Institute of Physics and Mathematics, Chinese Academy of Sciences (CAS) and Wuhan University, respectively.

Geomagnetic Meridian Station Chain: 

Geomagnetic Meridian Station Chain Consists of the fourteen stations Mohe (MHE), Manzhouli (MZL), Changchun (CNH), Beijing (BJI), Zhengzhou (ZZH), Wuhan (WHN), Shaoyang (SYN), Guangzhou (GZH), Qiongzhong (QZH), Sanya (SYN), Zhongshan (ZSH) and so on.

The Double Star Project mission (http://dsp-china.spaceweather.ac.cn/): 

The Double Star Project mission (http://dsp-china.spaceweather.ac.cn/) The Double Star Project is China's first purely scientific space mission and its first collaboration with the European Space Agency Double Star is designed for magnetospheric research, using two Chinese spacecraft, TC-1 and TC-2, which each have a payload consisting of both Chinese and European experiments. The TC-1 spacecraft is in a near-equatorial orbit and TC-2 in a polar orbit. The vehicle was a Chinese Long March 2C . TC-1 launched successfully on 27 December 2003, TC-2 on 25 July 2004. The Double Star mission was designed with collaboration with ESA's Cluster mission in mind. The mission design allows the six spacecraft together to address science questions that neither Cluster nor Double Star could address alone.

Meridian Project: 

Meridian Project Meridian Project stands for “Meridian Chain of Comprehensive Ground-Based Space Environment Monitors in the Eastern hemisphere in China

Meridian Project Framework: 

Meridian Project Framework 1. Space environment monitor system Radio Geomagnetic Optical Rocket 2.Data and Communication System 3. Research & Forecast System International Center Domestic user

INSTRUMENTS in Meridian Project: 

INSTRUMENTS in Meridian Project Incoherent scatter radar MST radar in Wuhan Univ. VHF radar to be constructed in Zhongshan station Rocket site at Hainan Province

SPACE RESEARCHES IN CHINA —— several examples: 

SPACE RESEARCHES IN CHINA —— several examples A new numerical procedure of asymmetric corona with multi-streamer structures - named the magnetic field fitting-modification method Coincidence between SOHO/LASCO obs. and the simulated results is better qualitatively both in the brightness and the magnetic field configurations (Li, J., Wei, F. and Feng, X: 2001, Geophys. Res. Lett. 28(7), 1359.)

MHD coupling model for corona-interplanetary space (Feng et al., 2005): 

MHD coupling model for corona-interplanetary space (Feng et al., 2005) Initial-boundary conditions constrained to solar observations from WSO and HAO K-coronal brightness & Parallel Implementation with Fortran MPI. Three-dimensional combined numerical MHD model of TVD Lax-Friedrich with MacCormack II together with calculation regional decomposition from 1 to 20Rs and 18Rs-1AU

Numerical study of Bz temperoal Behavior during 1997 Junuary Event: 

Numerical study of Bz temperoal Behavior during 1997 Junuary Event The temporal behavior of BZ at 1AU (the upper the observation by WIND and the bottom simulation) Shi, We and Feng, Sci in China, 2000

Study of the prediction method for geomagnetic disturbance - A so-called ISF method has been adopted for 24 events: 

Study of the prediction method for geomagnetic disturbance - A so-called ISF method has been adopted for 24 events Initial time T, its relative errors: △Tpred/ Tobs≤10% for 45.8% of all events, ≤30% for 78.3%, of all events, < 43% for 100%. of all events. Amplitude of the geomagnetic disturbances, ∑Kp take no account of Bz of IMF, Its relative errors: △Σ Kp, pred /ΣKp, obs≤10% for 12.5% of all events, ≤30% for 75% of all events, <50% for 100% of all events. take account of Bz of IMF △Σ Kp, pred /ΣKp, obs≤10% for 41.6% of all events, ≤30% for 87.5% of all events, ≤45% for 100% of all events. Wei Fengsi, Xuya, Feng, Science in China, 2002, 45(5), 525; Wei Fengsi, Cai Hongchang, Feng Xueshang, Adv. Space Res. Vol. 31, No. 4, pp. 1069-1073.2003

A fully-nonlinear global dynamical model for the middle and upper atmosphere is developed : 

A fully-nonlinear global dynamical model for the middle and upper atmosphere is developed Spatial distributions of average wave energy density of the wave packet Zhang, S. and Yi, F.: 1999, J. Geophys. Res. 104(D12), 14261.

Regional properties of traveling ionospheric disturbances (Wan et al.: 1998, Geophys. Res. Lett. 25, 3775): 

Regional properties of traveling ionospheric disturbances (Wan et al.: 1998, Geophys. Res. Lett. 25, 3775) Whether there is certain relation between the TIDs observed in Central China and some violent weather processes produced by the bulging topography of the Qinghai-Tibet plateau Around the east part of Qinghai-Tibet Plateau the distribution of the vortex occurrence shapes (the down) very like that of the TID source occurrence (the up)

Slide29: 

Space Weather Research Plan Exploration New Conceptions & New Principles Research Scientific frontier Application Human Activity New conception for space weather satellite series New explorative principles & methods Plasma Basic theory Solar drive sources geospace weather Interplanetary weather Influence to information system Influence to space life Influence to space material Cause-effect Chain model &comprehensive prediction method Space Weather Research Program by National Natural Science Foundation of China/Department of Earth Sciences

Other Space Missions under Plan: 

Other Space Missions under Plan KuaFu Mission by Prof. Tu Chuanyi (2012-2015) KuaFu A: to observe the solar explosives, halo CME and its propagation in interplanetary space. KuaFu B1+B2: to observe the geoeffectiveness of solar activities at polar orbit

What we can do for IHY?: 

What we can do for IHY? The Chinese solar and space instruments can be used for IHY Some instruments can be organized for global measurements of ionospheric and heliospheric phenomena Some datasets with more instruments can be used for the scientific objectives of IHY The problem is how to ask Chinese solar and space people to pay much attention to IHY