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Evidence for Reality of Rapid Solar Radio Fluctuation

Published online by Cambridge University Press:  12 April 2016

Fu Qijun ,
Hu Chumin ,
Zhao Bing ,
Jin Shenzhen ,
Yu. Yurovsky ,
A. Stepanov ,
A. Magun  and
E. Schanda
Fu Qijun
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China
Hu Chumin
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China
Zhao Bing
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China
Jin Shenzhen
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China
Yu. Yurovsky
Affiliation:
Crimea Astrophysical Observatory, RT-22, Katzively, Crimea 334247, Ukraine
A. Stepanov
Affiliation:
Crimea Astrophysical Observatory, RT-22, Katzively, Crimea 334247, Ukraine
A. Magun
Affiliation:
Institute for Applied Physics, University of Bern, CH-3012 Bern, Switzerland
E. Schanda
Affiliation:
Institute for Applied Physics, University of Bern, CH-3012 Bern, Switzerland

Extract

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Since fast fine structures (FFS) superimposed on microwave bursts were found with high time resolution observations, they have been observed in extensive frequency range (Slottje 1978; Fu, et al. 1986; Stähli and Magun 1986; and Stepanov and Yurovsky 1991), and these results make understanding of the emission deepening. But, at the same time, the puzzling problem, these phenomena originate from sun or are only artificial, is often concerned and disputed (Benz and Fürst 1987). As it was pointed out by Benz and Fürst (1987), “the only really reliable way to study solar microwave fluctuation is to use two or more widely separated radio telescopes”.

In this paper, some of FFS events superimposed on microwave bursts simultaneously obtained at Beijing Astronomical Observatory (BAO), Crimea Astrophysical Observatory (CAO) and Institute of Applied Physics, University of Bern (IAP), are presented at first time. It is a conclusive evidence of rapid radio fluctuation originating from sun and associated with flare appearance.

Type
Session 6. Flares and Transients
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 355 - 358
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

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