黑子半影内偶极运动磁特征的Hinode观测研究  

Hinode Observations of Bipolar Moving Magnetic Features in Sunspot Penumbra

作　　者：李珂君[1,2] 申远灯[1,2] 杨丽恒[1,2] 姜云春[1] 

机构地区：[1]中国科学院国家天文台/云南天文台,昆明650011 [2]中国科学院研究生院,北京100049

出　　处：《天文学报》2009年第3期289-300,共12页Acta Astronomica Sinica

基　　金：国家自然科学基金(10573033);云南省自然科学运用基金(2007A112M)资助

摘　　要：利用Hinode卫星观测的单色像和磁图,对出现在黑子半影内的35对偶极运动磁特征进行形态特征、运动速度以及低层太阳大气响应3方面的研究,得出以下结论: (1)偶极运动磁特征正负两极成对出现在黑子半影较垂直的磁场之间并向着半影外边界运动,间接验证了偶极运动磁特征起源于黑子半影水平磁场,在2—8小时的时间间隔内,同一位置上会反复出现形态特征和运动速度相似的偶极运动磁特征,为海蛇状磁力线模型提供了证据支持。(2)光球和色球在偶极运动磁特征向外运动过程中会出现增亮,说明偶极运动磁特征会加热中低层太阳大气。(3)偶极运动磁特征的出现位置和半影磁场结构分布符合非梳子状黑子半影结构特征。35 obvious bipolar moving magnetic features （MMFs）, which appear in sunspot penumbra, are investigated by analyzing filtergrams and magnetograms from Hinode. From analyzing their changes of the configuration, speed and the brightening response of the low solar atmosphere, the following results are obtained： （1） Bipolar MMFs appear in middle penumbra, occur between penumbral filaments with enhanced longitudinal magnetic signals. Both polarities of bipole move radially outward. This indirectly supports the idea that the bipolar MMFs originate from the horizontal magnetic field of the penumbra. There are more than one pair of bipolar MMFs appearing at the same position in 2-8 hours. This provides the evidence of sea-serpent field lines model. （2） The brightening response in photosphere and chromospheres indicates that the motion of the bipoles could heat the low solar atmosphere. （3） The position of bipolar MMFs and the magnetic field distribution of the penumbra provide another support in favor of the uncombed structure of penumbral magnetic fields.

关 键 词：太阳 太阳黑子 太阳 磁场 太阳 光球 太阳 色球 太阳 活动性 

分 类 号：P182[天文地球—天文学]