摘要
We present a new sub-class of type Ⅲ solar radio burst at the highfrequencies around 6.0 GHz. In addition to a descending and an ascending branch on the dynamicspectrum, it has an inverted morphology different from the simple type U-burst. We call it 'partialN-burst' because it is interpreted as the known N-burst minus its first branch. The partial N-burstpresented here was detected among a reverse slope type Ⅲ (RS-Ⅲ) burst group prior to the type Ⅴsolar radio continuum and was simultaneously recorded by two spectrometers at the NationalAstronomical Observatories, Chinese Academy of Sciences (NAOC, 5.20-7.60 GHz) and at Purple MountainObservatory (PMO, 4.50-7.50 GHz) on 1999 August 25. After the N-burst and M-burst, the partialN-burst is a third piece of evidence for a magnetic mirror effect in solar radio observation, whenthe same electron is reflected at a pinched foot of a flare loop.
We present a new sub-class of type Ⅲ solar radio burst at the highfrequencies around 6.0 GHz. In addition to a descending and an ascending branch on the dynamicspectrum, it has an inverted morphology different from the simple type U-burst. We call it 'partialN-burst' because it is interpreted as the known N-burst minus its first branch. The partial N-burstpresented here was detected among a reverse slope type Ⅲ (RS-Ⅲ) burst group prior to the type Ⅴsolar radio continuum and was simultaneously recorded by two spectrometers at the NationalAstronomical Observatories, Chinese Academy of Sciences (NAOC, 5.20-7.60 GHz) and at Purple MountainObservatory (PMO, 4.50-7.50 GHz) on 1999 August 25. After the N-burst and M-burst, the partialN-burst is a third piece of evidence for a magnetic mirror effect in solar radio observation, whenthe same electron is reflected at a pinched foot of a flare loop.
基金
National Natural Science Foundation of China.
