A broadband spectrometer for decimeter and microwave radio bursts

Fu, Qijun; Qin, Zhihai; Ji, Huirong; Pei, Li-ben

doi:10.1007/bf00679098

Cited by 121 publications

(68 citation statements)

References 9 publications

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“…The events were recorded with the spectrometer at 2.6−3.8 GHz of the Beijing Astronomical Observatory (Fu et al 1995). The sampling interval of the instrument is 8 ms for the full frequency range in two polarization modes (R and L).…”

Section: Instrumentationmentioning

confidence: 99%

Discovery of unusual large group delay in microwave millisecond oscillating events

Fleishman

Huang

et al. 2002

A&A

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Abstract. Two events demonstrating periodic narrowband millisecond pulsations of radio emission both in intensity and polarization degree are analyzed. Large time delays between L-and R-polarization components are found. The radio emission is shown to be generated as unpolarized by a plasma mechanism at the second harmonic of the upper-hybrid frequency. Observed oscillations of the radiation polarization degree arise due to group delay between extraordinary and ordinary modes along the line of sight. The theoretically predicted dependence of the group delay on frequency (∼f −3 ) agrees excellently with the observed delay frequency dependence. Physical parameters of the emission source and "delay site" are determined within the proposed model.

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Section: Instrumentationmentioning

confidence: 99%

Discovery of unusual large group delay in microwave millisecond oscillating events

Fleishman

Huang

et al. 2002

A&A

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“…The observational material used was taken by the "Solar Radio Broadband Spectrometers" in the ranges 1-2 GHz and 2.6-3.8GHz of BAO with 20 MHz/100 ms and 10 MHz /8 ms resolutions, respectively (Fu et al 1995); the swept-frequency spectrographs in the ranges 40-90, 100-170, 200-400 and 400-800 MHz, with a sweep rate of 10 s-l at Tremsdorf of AlP (Mann et al 1992); and the 2-d inter-Initial Phase of Solar Radio Burst on 23 September 1998 Figure 1. The radio dynamic spectrograms during 06:52:31.7 -06:55:51.7 UT by 40-800MHz (AlP), 1-2 and 2.6-3.8 GHz (BAO) spectrometers.…”

Section: Observations and Discussionmentioning

confidence: 99%

On the Initial Phase of Solar Radio Burst Event on 23 September 1998

Yan

Auraß

et al. 2001

Symp. - Int. Astron. Union

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Abstract. On 23 September 1998 there was a 3B/M7.1 flare event starting at 06:40 UT with more than 100 minute duration radio bursts of 1134 sfu peak flux at 2840 MHz and accompanying a CME. In this paper, the event is analyzed with the data observed by Beijing Astronomical Observatory (BAG), OSRA-Tremsdorf (AlP) and SSRT-ISTP. In particular, we compare the fine structures (FS) during the triggering phase revealed in different regimes and discuss their implications.

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“…Since 1994, a broadband solar radio spectrometer had been developed in China, with a frequency coverage of 0.7-7.6 GHz, a frequency resolution of 1-10 MHz, and a temporal resolution of 1-10 ms (Fu, et al (2004b)). This instrument is composed of multibands spectrometers and the three spectrometers at 1.0-2.0 GHz, 2.6-3.8 GHz, and 5.2-7.6 GHz are located at Huairou Solar Observing Station of National Astronomical Observatories, Chinese Academy of Sciences (NAOC).…”

Section: Instruments and Observationsmentioning

confidence: 99%

“…Table 1 shows the description of the spectrometers at Huairou (Ji, et al (2000), Ji, et al (2003), Fu, et al (2004b). …”

Section: Instruments and Observationsmentioning

confidence: 99%

“…(Bastian et al 1998). The Solar Radio Broadband Dynamic Spectrometer (SRBS) of China is the first instrument in microwave to acquire dynamic spectrums of solar bursts with the combination of wide frequency coverage (0.7-7.6 GHz), high temporal resolution, high spectral resolution, and high sensitivity (Fu et al 2004b). We compare the occurrence of FSs in 1-7.6 GHz range with flare/CME events.…”

Section: Introductionmentioning

confidence: 99%

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Occurrence of Solar Radio Burst Fine Structures in 1–7.6 GHz Range Associated with CME Events

et al. 2004

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Abstract. The solar radio bursts and accompanying fine structures recorded by spectrometers at Huairou, Beijing during 1999-2003 are presented. The spectrometers are with high temporal (5-10 ms) and spectral (4-20 MHz) resolutions. We found 91 radio burst events that occurred within half hour of the onset of the CME events which cause solar energetic particle events. The associations of radio fine structures with CME events are discussed.

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A broadband spectrometer for decimeter and microwave radio bursts

Cited by 121 publications

References 9 publications

Discovery of unusual large group delay in microwave millisecond oscillating events

Discovery of unusual large group delay in microwave millisecond oscillating events

On the Initial Phase of Solar Radio Burst Event on 23 September 1998

Occurrence of Solar Radio Burst Fine Structures in 1–7.6 GHz Range Associated with CME Events

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