Solar and Space Progress in China associated with IHY

1
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

2
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
3
Solar Telescopes in Yunnan Astronomical
Observatory (http//www.ynao.ac.cn)
4
Solar Telescopes in Purple Mountain Observatory
(http//www.pmo.ac.cn)
Purple Mountain Observatory
5
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
• ?-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

6
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

7
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
8
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

9
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 ? is justified
  and applied for a closed-form non-constant-a
  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)

10
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)

11
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., EPS, 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).

12
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. (ZhangHuang, ApJL, 2003
  Solar Phys, 2004) .

13
The processes responsible for heating the
different types of the corona

• In a low-ß 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).

14
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., AA,
  2000a,b)
• The turbulent viscosity exerts a non-negligible
  influence on the solar p-mode oscillations (Bi et
  al., AA, 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., AA, 2000)

15
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
  AA, 2003a,b)

16
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
  

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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.

18
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.

19
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.

20
Meridian Project

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

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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
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INSTRUMENTS in Meridian Project
Incoherent scatter radar
MST radar in Wuhan Univ.
Rocket site at Hainan Province
VHF radar to be constructed in Zhongshan
station
23
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.)

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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

25
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

26
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/ Tobs10 for 45.8 of all
  events,
• 30 for
  78.3, of all events,
• lt 43 for
  100. of all events.
• Amplitude of the geomagnetic disturbances, ?Kp
• take no account of Bz of IMF, Its relative
  errors
• ?S Kp, pred /SKp, obs10 for
  12.5 of all events,
• 
  30 for 75 of all events,
• 
  lt50 for 100 of all events.
• take account of Bz of IMF
• ?S Kp, pred /SKp, obs10 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

27
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.

28
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)

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Space Weather
Research Program by National Natural Science
Foundation of China/Department of Earth Sciences
Space Weather Research Plan
Research Scientific frontier
Exploration New Conceptions New Principles
Application Human Activity
Solar drive sources
Influence to information system
New conception for space weather satellite series
Influence to space life
Plasma Basic theory
Interplanetary weather
Influence to space material
New explorative principles methods
geospace weather
Cause-effect Chain model comprehensive
prediction method
30
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 B1B2 to observe the geoeffectiveness of
  solar activities at polar orbit

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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