1. Observation and Data Analysis of Solar Radio Telescope at Huairou Observatory, Beijing
Chengming Tan
National Astronomical Observatories
Chinese Academy of Sciences, Beijing , China

2. Main contents Instruments Observation and Solar Physics
Data analysis and archive
Conclusion

3. 1.0-2.0 GHz Under reconstruction Huairou Solar Radio Telescopes
1. Instruments
GHz Under reconstruction
2840 MHz Polarimeter
GHz
GHz
Huairou Solar Radio Telescopes

4. Main performance parameters
Bandwidth
2840MHz±5MHz
GHz
GHz
GHz
Observe Period
2010Dec.-Now
1996-Now
1999-Now
Diameter
2 m
7.3 m
3.2 m
Share with GHz
Time Cadence 1s
1msec
100msec(2002)
1.25msec(2002)
8msec
5msec
Spectral resolution
20MHz (2002)
4MHz (2002)
10MHz
20MHz
Num. of Channels 1
240
120
Circular
Polarization Accuracy
No polarization
10%
Data Amount
64 Mb/10h
170Mb～6.6Gb/10h
82 Mb～2.1Gb/10h
82 Mb ～ 3.4 Gb/10h

5. Observation and Solar Physics
The 2840 MHz polarimeter observe the sun and obtain the total coming flux at 2840 MHz radio frequency.
Solar radio dynamic spectrometers observe the sun and obtain the circular-polarization flux at series of radio frequency (neighboring narrow band).
The observed data can be calibrated to standard flux data in solar flux unit (s.f.u). 1 s.f.u=10-22 W m-2 Hz-1
Solar radio observation helps to understand the characterization of acceleration sites, mechanism and evolution of energetic electrons.
Combined radio and X-ray observation helps to understand the flare and eruptive phenomena.
Radio diagnostics allowing to measure the coronal magnetic field.
Radio bursts have good relationship with flare and CMEs (ICMEs). Thus might forecast the arrive time of shocks at the earth as well as on Space Weather studies. (type IV, type II or complex type III)

6. Solar radio burst and geomagnetic storms
Type IV event
Probability of a flare to be associated with a SSC versus its radio importance, i.e. the energy radiated at 2.8 GHz (adapted from Caroubalos 1964)

7. The energy of radio burst and the transit time of SSC

8. Radio Spectral Observation and Studies
The Apr. 10, 2001 event Fu, Q. et al. 2004, ChJAA
Drift Pulsation Structure (DPS) -3~-5MHz/s
DCIM
Type IV
DPS
ZPS
X2.3, UT

9. The Apr. 10, 2001 event Velocity=2411km/s 32 hours later
X2.3 Flare/CME event in NOAA 9415
The Apr. 10, 2001 event
Velocity=2411km/s
DPS
ZPS
DCIM
Also spike
32 hours later

10. Study of Spectrum of Fine Structures
Type M&N Ning, Z. et al.2001,A&A

11. Zebra and Fiber Yan, Y. et al, 2002 ESASP

12. Zebra Tan,C 2004,CHJAA

13. Fish Group Huang, J.et al. 2007,AdSR

14. Hand like Huang, J. et al. 2007,AdSR

15. pulsation
Tan, B. et al，2010，APJ

16. Observation of MHz

17. One day observation at 2840 MHz

18. Data archive and analysis method
The data processing software was written in IDL language.
Some event supplied data or figure on the web site. It can be download.
All the data (if there’s observation) can be download by request now since large amount of data:
The 2840 MHz data can be processed real time and download on the internet. (To be done).
Calibration, Clean (normalize, wavelet, remove noise)

20. Conclusion
The dynamic solar radio spectrometers located at Huairou were put into good operation since While 2840 MHz polarimeter, earlier than 1977.
They are valuable instrument for the study of solar bursts in microwaves, and supplied large amount of observation data for studying the relationship with flare, CMEs (ICMEs), MC (SSCs) et al.