Observation and Data Analysis of Solar Radio Telescope at Huairou Observatory, Beijing Chengming Tan Email: Tanchm@nao.cas.cn National Astronomical Observatories Chinese Academy of Sciences, Beijing 100012, China

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

1.0-2.0 GHz Under reconstruction Huairou Solar Radio Telescopes 1. Instruments 1.0-2.0 GHz Under reconstruction 2840 MHz Polarimeter 2.6-3.8 GHz 5.2-7.6 GHz Huairou Solar Radio Telescopes

Main performance parameters Bandwidth 2840MHz±5MHz 1.0-2.0GHz 2.6-3.8GHz 5.2-7.6GHz Observe Period 1977-2007 2010Dec.-Now 1994-2006 1996-Now 1999-Now Diameter 2 m 7.3 m 3.2 m Share with 2.6-3.8 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

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)

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)

The energy of radio burst and the transit time of SSC

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, 0506-0526-0542 UT

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

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

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

Zebra Tan,C 2004,CHJAA

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

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

pulsation Tan, B. et al，2010，APJ

Observation of 2840 MHz

One day observation at 2840 MHz

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 E-mail request now since large amount of data: tanchm@nao.cas.cn. The 2840 MHz data can be processed real time and download on the internet. (To be done). Calibration, Clean (normalize, wavelet, remove noise)

Conclusion The dynamic solar radio spectrometers located at Huairou were put into good operation since 1994. 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.