VECTOR MAGNETIC FIELDS OF SOLAR GRANULATION
VECTOR MAGNETIC FIELDS OF SOLAR GRANULATION
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DOI：
10.1088/0004-637x/690/1/279
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发表时间：
2008-09
期刊：
影响因子：
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通讯作者：
C. Jin;Jingxiu Wang;Mengchun Zhao
中科院分区：
文献类型：
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作者：
C. Jin;Jingxiu Wang;Mengchun Zhao
日野号航天器上的太阳光学望远镜/光谱学偏振仪对平静太阳的观测揭示了太阳光球层的磁性特征。利用三个安静区的深模观测，对太阳粒化的矢量磁场进行了统计研究。人工选择2000多个正常颗粒形成样品。我们认识到，一些颗粒的强度甚至比平均光球暗，并且颗粒的强度与多普勒速度之间存在线性相关关系。得到了颗粒的纵向和横向视磁通密度、多普勒速度和连续强度的分布，并测量了颗粒的无符号磁通。本研究采用了两种方法。首先，我们通过对所有取样颗粒的测量平均值获得了造粒的磁性。其次，基于子样本重构平均颗粒胞，得到模型颗粒胞内的视磁通密度的详细分布；并将这些结果与晶间巷和少数典型异常颗粒的结果进行了比较。我们的统计分析揭示了以下结果。(1)单个颗粒的无符号磁通量范围为1.1 × 1015 ~ 3.3 × 1018 Mx，峰值分布在1.6 × 1016 Mx。(2)颗粒的无符号纵向表观通量密度在0 ~ 212 Mx cm−2之间，平均纵向表观通量密度为12 Mx cm−2，而颗粒的横向表观通量密度在4 ~ 218 Mx cm−2之间，平均横向表观通量密度为79 Mx cm−2。颗粒的纵向表观磁通密度与横向表观磁通密度呈正相关，且颗粒的纵向表观磁通密度弱于相应的横向表观磁通密度。(3)颗粒相对于垂直于视线表面的磁倾角在4.8 ~ 76.7°范围内，峰值分布在25°处。平均而言，颗粒内的磁矢量比粒间的磁矢量更垂直。(4)安静太阳上的垂直场和水平场都倾向于位于粒间带。(5)给出了平均颗粒胞内的视通量密度、多普勒速度和连续强度的详细分布。这些分布可以用经验公式很好地表述出来。
Observations of the quiet Sun from the Solar Optical Telescope/Spectro-Polarimeter aboard the Hinode spacecraft reveal the magnetic characteristics of the solar photosphere. By making use of the deep-mode observations of three quiet regions, we have statistically studied the vector magnetic fields of solar granulation. More than 2000 normal granules are manually selected to form a sample. It is recognized that some granules are even darker than the mean photosphere in intensity, and there is a linear correlation between intensity and Doppler velocity in the granules. The distributions of longitudinal and transverse apparent magnetic flux densities, Doppler velocity, and continuum intensity of granules are obtained, and their unsigned magnetic flux measured. Two approaches are used in this study. First, we obtained the magnetic properties of granulation by averaging the measurements for all the sampling granules. Second, we reconstructed an average granular cell based on a subsample, and obtained the detailed distribution of apparent magnetic flux density within the model granular cell. All the results have been compared with those for intergranular lanes and a few typical abnormal granules. Our statistical analysis reveals the following results. (1) The unsigned magnetic flux of individual granules spans the range from 1.1 × 1015 Mx to 3.3 × 1018 Mx with a peak distribution at 1.6 × 1016 Mx. (2) The unsigned longitudinal apparent flux density of granules ranges from almost 0 to 212 Mx cm−2 with a mean longitudinal apparent flux density of 12 Mx cm−2, while the transverse apparent flux density of granules ranges from 4 to 218 Mx cm−2 with a mean transverse apparent flux density of 79 Mx cm−2. The longitudinal and transverse apparent magnetic flux densities of granules are positively correlated, and the longitudinal apparent flux density of granules is weaker than the corresponding transverse apparent flux density. (3) The magnetic inclination of granules with respect to the surface that is perpendicular to the line of sight falls in the range of 4.8–76.7 degrees with a peak distribution at 25 degrees. On average, the magnetic vectors in granules are more vertical than those in the intergranular lanes. (4) There is a strong preference that both the vertical and horizontal fields on the quiet Sun reside in the intergranular lanes. (5) The detailed distributions of apparent flux density, Doppler velocity, and continuum intensity within an average granular cell are presented. These distributions can be empirically formulated well.