摘要
The fast rotation of sunspot group 5395 ( first, it exhibited inverse clockwise rotation, then clockwise rotation, the rotative angle was the lagrest 1-2 days before proton flare.) the stronger emission of SVC and the spectral maximun (near 8800MHz) of both the SVC and peak fluxes of the bursts et al are close correlated with occurrence of proton flares. Flares often generated in the regions of emerging or disappearing of new magnetic flux with opposite polarity, of the faster and more complex variation of the gradient and configuration of magnetic field, and of the neck and tail of magnetic gulf.
The fast rotation of sunspot group 5395 ( first, it exhibited inverse clockwise rotation, then clockwise rotation, the rotative angle was the lagrest 1-2 days before proton flare.) the stronger emission of SVC and the spectral maximun (near 8800MHz) of both the SVC and peak fluxes of the bursts et al are close correlated with occurrence of proton flares. Flares often generated in the regions of emerging or disappearing of new magnetic flux with opposite polarity, of the faster and more complex variation of the gradient and configuration of magnetic field, and of the neck and tail of magnetic gulf.
出处
《天文研究与技术》
CSCD
1990年第4期86-90,共5页
Astronomical Research & Technology
