Decades of Chinese Solar and Geophysical Data

2018 ◽  
Vol 13 (S340) ◽  
pp. 71-72 ◽  
Author(s):  
Yan Yan ◽  
Zhan-Le Du ◽  
Hua-Ning Wang ◽  
Han He ◽  
Juan Guo ◽  
...  
Keyword(s):  
Solar Flares ◽  
Data Exchange ◽  
Astronomical Observatory ◽  
Geophysical Data ◽  
Radio Bursts ◽  
Ionospheric Storm ◽  
Solar Radio Bursts ◽  
Chinese Academy Of Sciences ◽  
Forecast Data ◽  
Academy Of Sciences

AbstractThe Chinese Solar and Geophysical Data (CSGD) was first issued at the Beijing Astronomical Observatory, Chinese Academy of Sciences (now the headquarter of the National Astronomical Observatories, Chinese Academy of Sciences) in 1971, when China’s satellite-industry was booming. CSGD covers the observational data (observations of the sunspots, solar flares, solar radio bursts, ionospheric storm and geomagnetic storm) from a couple of domestic observatories and the forecast data. The compiler of CSGD still keeps the data exchange with other institutes worldwide. The type of the dataset includes texts, tables, figures and so on. Up to now, we have electronized all the historic archives, making them easily accessible to people who are interested in them.

scholarly journals Recent Results of Meter-decameter Wave Observations of Solar Flares

1989 ◽  
Vol 104 (2) ◽  
pp. 185-189
Author(s):  
N. Copalswamy ◽  
M. R. Kundu
Keyword(s):  
Solar Flares ◽  
Solar Radio ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Type Iii ◽  
Type Iv

AbstractWe present recent results from meter-decameter imaging of several classes of solar radio bursts: Preflare activity in the form of type III bursts, correlated type IIIs from distant sources, and type II and moving type IV bursts associated with flares and CMEs.

scholarly journals Separation of solar radio bursts in a complex spectrum

2010 ◽  
Vol 6 (S274) ◽  
pp. 150-152
Author(s):  
Hana Mészárosová ◽  
Ján Rybák ◽  
Marian Karlický ◽  
Karel Jiřička
Keyword(s):  
Radio Emission ◽  
Current Sheet ◽  
Solar Flares ◽  
Solar Radio ◽  
Radio Spectrum ◽  
New Method ◽  
Complex Spectrum ◽  
Radio Bursts ◽  
Solar Radio Bursts ◽  
Fine Structures

AbstractRadio spectra, observed during solar flares, are usually very complex (many bursts and fine structures). We have developed a new method to separate them into individual bursts and analyze them separately. The method is used in the analysis of the 0.8–2.0 GHz radio spectrum of the April 11, 2001 event, which was rich in drifting pulsating structures (DPSs). Using this method we showed that the complex radio spectrum consists of at least four DPSs separated with respect to their different frequency drifts (−115, −36, −23, and −11 MHz s−1). These DPSs indicate a presence of at least four plasmoids expected to be formed in a flaring current sheet. These plasmoids produce the radio emission on close frequencies giving thus a mixture of superimposed DPSs observed in the radio spectrum.

scholarly journals Space Weather Study through Analysis of Solar Radio Bursts detected by a Single Station CALLSTO Spectrometer

2021 ◽  
Author(s):  
Theogene Ndacyayisenga ◽  
Ange Cynthia Umuhire ◽  
Jean Uwamahoro ◽  
Christian Monstein
Keyword(s):  
Space Weather ◽  
Solar Flares ◽  
Solar Radio ◽  
Low Cost ◽  
Radio Bursts ◽  
Solar Dynamics Observatory ◽  
Solar Radio Bursts ◽  
Type Iii ◽  
Type Iv ◽  
Single Station

Abstract. This article summarizes the results of an analysis of solar radio bursts detected by the e-Compound Astronomical Low cost Low-frequency Instrument for spectroscopy and Transportable Observatory (e-CALLISTO) spectrometer hosted by the University of Rwanda, College of Education. The data analysed were detected during the first year (2014–2015) of the instrument operation. The Atmospheric Imaging Assembly (AIA) images on board the Solar Dynamics Observatory (SDO) were used to check the location of propagating waves associated with type III radio bursts detected without solar flares. Using quick plots provided by the e-CALLISTO website, we found a total of 202 solar radio bursts detected by the CALLISTO station located in Rwanda. Among them, 5 are type IIs, 175 are type IIIs, and 22 type IVs radio bursts. It is found that all analysed type IIs and ∼37 % of type III bursts are associated with impulsive solar flares while Type IV radio bursts are poorly associated with flares. Furthermore, all of the analysed type II bursts are associated with CMEs which is consistent with the previous studies, and ∼44 % of type IIIs show association with CMEs. On the other hand it is observed that the majority of type IV radio bursts are believed to be originated from CME-driven shocks. Findings from this study confirms that solar radio bursts (SRBs) from ground observation and analysis constitute a clue to diagnose the space weather phenomena such as solar flare and CMEs and to some extent, they may serve as the advance warning of the related severe space weather hazards.

scholarly journals Radio Data and Computer Simulations for Shock Waves Generated by Solar Flares

1980 ◽  
Vol 91 ◽  
pp. 251-255
Author(s):  
Alan Maxwell ◽  
Murray Dryer
Keyword(s):  
Shock Waves ◽  
Solar Corona ◽  
Computer Simulations ◽  
Solar Flares ◽  
Solar Radio ◽  
Radio Bursts ◽  
Type Ii ◽  
Fast Mode ◽  
Solar Radio Bursts ◽  
Radio Data

Solar radio bursts of spectral type II provide a prime diagnostic for the passage of shock waves, generated by solar flares, through the solar corona. In this investigation we have compared radio data on the shocks with computer simulations for the propagation of fast-mode MHD shocks through the solar corona. The radio data were recorded at the Harvard Radio Astronomy Station, Fort Davis, Texas. The computer simulations were carried out at NOAA, Boulder, Colorado.

scholarly journals A brief history of Regional Warning Center China (RWC-China)

2018 ◽  
Vol 9 (1) ◽  
pp. 41-47 ◽  
Author(s):  
Han He ◽  
Huaning Wang ◽  
Zhanle Du ◽  
Xin Huang ◽  
Yan Yan ◽  
...  
Keyword(s):  
Astronomical Observatory ◽  
Space Environment ◽  
Short Term ◽  
Activity Prediction ◽  
International Space ◽  
Chinese Academy Of Sciences ◽  
History Of ◽  
Academy Of Sciences ◽  
Environment Service ◽  
Terrestrial Data

Abstract. Solar-terrestrial prediction services in China began in 1969 at the Beijing Astronomical Observatory (BAO), Chinese Academy of Sciences (CAS). In 1990, BAO joined the International URSIgram and World Days Service (IUWDS) and started solar-terrestrial data and prediction interchanges with other members of IUWDS. The short-term solar activity prediction service with standard URSIgram codes began in January 1991 at BAO, and forecasts have been issued routinely every weekday from then on. The Regional Warning Center Beijing (RWC-Beijing) of IUWDS was officially approved in China in 1991 and was formally established in February 1992. In 1996, the IUWDS was changed to the current name, the International Space Environment Service (ISES). In 2000, the RWC-Beijing was renamed RWC-China according to ISES requirements. In 2001, the National Astronomical Observatories, CAS (NAOC) was established. All the solar-terrestrial data and prediction services of BAO were taken up by NAOC. The headquarters of RWC-China is located on the campus of NAOC.

scholarly journals The Association of Solar Radio Bursts of Spectral Type III with Chromospheric Flares

1957 ◽  
Vol 10 (4) ◽  
pp. 483 ◽  
Author(s):  
RE Loughhead ◽  
JA Roberts ◽  
Marie K McCabe
Keyword(s):  
Spectral Type ◽  
Solar Flares ◽  
Solar Radio ◽  
Radio Bursts ◽  
Radio Observations ◽  
Solar Radio Bursts ◽  
Type Iii ◽  
Class 1 ◽  
Relationship Of ◽  
The Relationship

The relationship of radio bursts of spectral type III to solar flares is investigated by comparing simultaneous optical and radio observations. Over 300 flares are examined, 85 per cent. of which are microflares (class 1?). About 20 per cent. of the flares are associated with type III events, while more than 60 per cent. of the bursts recorded occur during the lifetime of a flare. These bursts tend to occur near the beginning of the flare or even to precede it slightly.

scholarly journals Type II Solar Radio Bursts in the Decimeter Band

1974 ◽  
Vol 57 ◽  
pp. 343-343
Author(s):  
Alan Maxwell
Keyword(s):  
Shock Waves ◽  
Solar Flares ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Lower Corona ◽  
Previous Discussion ◽  
Radio Equipment ◽  
Interplanetary Plasma ◽  
Radio Band

(Solar Phys.) The progress of shock waves generated by solar flares through the corona is delineated in the radio band by radio bursts of spectral type II. Previous discussion of these bursts has been mainly concerned with their characteristics at frequencies below 200 MHz. This paper discusses the characteristics of the bursts in the range 2000–200 MHz, and the information that may then be deduced about the propagation of shock waves through the lower corona. Particular attention is paid to the type II burst emitted by the flare of 1972 August 7, 1500 UT. The shock from this flare was subsequently tracked (by radio equipment on the IMP-6 satellite) through the interplanetary plasma right to the Earth.

EDITORIAL

2013 ◽  
Vol 02 (02) ◽  
pp. 3-3
Author(s):  
Kok Khoo Phua
Keyword(s):  
Astronomical Observatory ◽  
Asia Pacific ◽  
Research Institutes ◽  
Chinese Academy Of Sciences ◽  
Astronomical Research ◽  
Academy Of Sciences ◽  
Astronomy And Astrophysics ◽  
Research Institute

In this issue of the Asia Pacific Physics Newsletter (APPN), we introduce four Astronomical Research Institutes in Asia Pacific: the Australian Astronomical Observatory, National Astronomical Research Institute of Thailand, Shanghai Astronomical Observatory, Chinese Academy of Sciences and Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan.

scholarly journals The Sino-German λ6cm polarization survey of the Galactic plane

2012 ◽  
Vol 10 (H16) ◽  
pp. 394-394
Author(s):  
J. L. Han ◽  
W. Reich ◽  
X. H. Sun ◽  
X. Y. Gao ◽  
L. Xiao ◽  
...  
Keyword(s):  
Sea Level ◽  
Radio Telescope ◽  
High Frequency ◽  
Galactic Plane ◽  
Astronomical Observatory ◽  
Processing Methods ◽  
Dual Channel ◽  
Chinese Academy Of Sciences ◽  
Academy Of Sciences

After Prof. R. Wielebinski visited China in 1999, we started to plan the Sino-German λ6 cm polarization survey of the Galactic plane, using the Urumqi 25-m radio telescope of Xinjiang (formerly Urumqi) Astronomical Observatory, Chinese Academy of Sciences. It is a high-frequency complement of previous Effelsberg 21-cm and 11-cm surveys, using the same observing and processing methods. The telescope is located at an altitude of 2029 m above sea level at geographic longitude of 87°E and latitude 43°N. The dual-channel λ6 cm receiver with a polarimeter and a bandwidth of 600 MHz was designed by O. Lochner and constructed at the MPIfR in Germany with involvements by the Urumqi engineers M.Z. Chen and J. Ma. In August 2004, the receiver was installed at the secondary focus of the Urumqi 25-m telescope.

scholarly journals Shanghai Astronomical Observatory, Chinese Academy of Sciences

2013 ◽  
Vol 02 (02) ◽  
pp. 74-75
Keyword(s):  
Astronomical Observatory ◽  
Chinese Government ◽  
Chinese Academy Of Sciences ◽  
Academy Of Sciences

Shanghai Astronomical Observatory (SHAO) of the Chinese Academy of Sciences (CAS), was established in 1962 following the amalgamation of the former Xu Jiahui and Sheshan observatories, which were founded by the French Mission Catholique in 1872 and 1900, respectively. Both came under the Chinese government jurisdiction in 1950.

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