摘要
本文研究结果表明：同一黑子群在日面期间的顺或反时针方向的旋转运动会先后并存．质子耀斑前1～2无，黑子群的旋转角速度达到极大．耀斑后，磁绳的松弛，黑子群可能会反向旋转，强的剪切过程和质子耀斑可能会再度出现．强质子耀斑活动区的共同特征是：（1）形态为单个团状结构δ型黑子，即众多异极性本影核紧锁在同一黑子半影中；（2）黑子面积＞1000×10－6半球面积，日面跨度＞10°；（3）黑子群都有快速的旋转运动．这类活动区，如果在日面西部活动性明显地增强，那么这个活动区在未来转到日面边缘及其背后、或再次从日面东边缘转出时，定能再次爆发耀斑和伴随较强质子事件。
The studying results indicate that before and after proton flares, clockwise and counter clockwise rotation of the sunspot groups are early or late exist for the same a sunspot group on the solar disk. The rotative angle of the sunspot group reach the largest within 1-2 days before the proton flare, after flare, due to magnetic flux ropes are slackened, therefore, the rotation of the sunspot groups are decelerated continually and finally rotate in the opposite direction, and a strong magnetic shear configurations and strong proton flares can occur once again. The common characteristics of the active regions of the strong proton flares are shown as follows: (1) The morphology of the spot is a single granular structure b type spot, that is many umbras with opposite magnetic polarities locked tightly in a singIe penumbra, and once they lock together, they never separate; (2) The area of the sunspot is greater than 1000×10-6hemi, the span of the sunspot groups on solar disk is greater than10°; (3)Sunspot groups had fast motion of the rotation. If the activity of the above active regions is already stronger when they moves to the west of the Sun, then when they turns to the western limb and back of the Sun or again crosses the solar disk, will produce more large proton flares.
基金
国家自然科学基金!49391400
中国科学院光学天文联合实验室资助
天文委员资助
