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Astronomical data analysis depends on the accumulation of data, including integrity of data in observing location, time, and diversity of data. We are now developing a reorganization project of solar physics history data of China. There are 90 years, 44 kinds of solar observing data in China. In the project, we will finish imagination, digitalization and standardization of these data. This article introduces the project framework, data, data processing, and how to share.

The properties, structure and performance of a Solar Radio Spectrometer working at 5.2–7.6 GHz developed by National Astronomical Observatories/Beijing and Hebei Semiconductor Research Institute are described. The spectrometer has a spectral resolution of 20 MHz and a temporal resolution of 5 ms, with an instantaneous detectable range from 2% to 10 times flux of the quiet Sun. It can measure both left and right circular polarizations with an accuracy of 10% of polarization degree. Some results of preliminary observations are presented.

On August 9, 2011, there was an X6.9 flare event occurred near the west limb of solar disk. From the observation obtained by the spectrometer of the Chinese Solar Broadband Radio Spectrometer in Huairou (SBRS/Huairou) around the flare, we find that this powerful flare has only a short-duration microwave burst of about only 5 minutes, and during the short-duration microwave burst, there are several kinds of fine structures on the spectrogram. These fine structures include very short-period pulsations, millisecond spike bursts, and type III bursts. The most interesting is that almost all of the pulses of very short-period pulsation (VSP) are structured by clusters of millisecond timescales of spike bursts or type III bursts. And there exists three different kinds of frequency drift rates in the VSP: the frequency drift rates with absolute value of about 55 - 130 MHz s^{-1} in the pulse groups, the frequency drift rates with absolute value of about 2.91 - 16.9 GHz s^{-1} on each individual pulse, and the frequency drift rates with absolute value of about 15 - 25 GHz s$^{-1}$) at each individual spike burst or type III burst., Comment: 5 pages, 3 figures

Based on the joint-observations of the radio broadband spectral emissions of solar eclipse on August 1, 2008 at Jiuquan (total eclipse) and Huairou (partial eclipse) at the frequencies of 2.00 -- 5.60 GHz (Jiuquan), 2.60 -- 3.80 GHZ (Chinese solar broadband radiospectrometer, SBRS/Huairou), and 5.20 -- 7.60 GHz (SBRS/Huairou), the authors assemble a successive series of broadband spectrum with a frequency of 2.60 -- 7.60 GHz to observe the solar eclipse synchronously. This is the first attempt to analyze the solar eclipse radio emission under the two telescopes located at different places with broadband frequencies in the periods of total and partial eclipse. With these analyses, the authors made a new semiempirical model of the coronal plasma density of the quiet Sun and made a comparison with the classic models., Comment: 10 pages, 4 figures, published on Sci. China Ser. G, 2009, Vol.52, page 1765-1772