VECTOR MAGNETIC FIELDS OF A SOLAR POLAR REGION
VECTOR MAGNETIC FIELDS OF A SOLAR POLAR REGION
复制标题
太阳极区的矢量磁场
DOI：
10.1088/0004-637x/732/1/4
复制
发表时间：
2011-04
影响因子：
4.9
通讯作者：
Wang, Jingxiu
中科院分区：
文献类型：
--
作者：
Jin, Chunlan;Wang, Jingxiu
利用太阳光学望远镜和分光偏振计的观测资料，研究了太阳极区的矢量磁场。为了更好地理解极磁特性，我们将观测到的极场与在边缘（QRL）和盘中心（QRD）的两个太阳安静区以及低纬度冕洞（EHD）的极场进行了比较。结果表明：（1）PR的平均垂直通量密度为16 G，平均水平通量密度为91 G;如果我们假设观测到的极区在偏振测量中遭受与太阳宁静区相同的临边减弱，则极区的平均无符号通量密度将为54 G，比CHR强60%。（2）PR中的kG场占该区域的6.7%。PR中的磁填充因子的特征在于双峰分布，其分别出现在接近100 G和1000 G的场强处。(3)对于网络元素，垂直和水平通量密度之间存在相关性，这表明观察到的更强的垂直和水平分量表现出相同的物理实体。(4)少数极性的磁通量与主极性的磁通量之比约为0.5，这意味着PR中只有1/3的磁通量通向行星际空间。通过对观测到的磁场进行准线性无力外推，我们发现光球开放通量并不总是与强垂直磁性元素相关。
We study the vector magnetic fields of a solar polar region (PR) based on Solar Optical Telescope/Spectro-Polarimeter measurements. To better understand the polar magnetic properties, we compare the observed polar field with that in two solar quiet regions at the limb (QRL) and the disk center (QRD), and with that in a region of a low-latitude coronal hole (CHR). The following results are discussed: (1) The average vertical flux density of PR is 16 G, while the average horizontal flux density is 91 G. If we assume that the observed polar field suffers the same amount of limb weakening in polarization measurements as the Sun's quiet region, the average unsigned flux density in the pole would be 54 G, 60% stronger than that in the CHR. (2) The kG field in the PR occupies 6.7% of the region. The magnetic filling factor in the PR is characterized by a two-peak distribution, which appears at a field strength close to 100 G and 1000 G, respectively. (3) For the network elements, a correlation holds between the vertical and horizontal flux densities, suggesting the same physical entity is manifested by the observed stronger vertical and horizontal components. (4) The ratio of the magnetic flux in the minority polarity to that in the dominant polarity is approximately 0.5, implying that only 1/3 of the magnetic flux in the PR opens to the interplanetary space. Exemplified with CHR by a quasi-linear force-free extrapolation of the observed magnetic field, we find that the photospheric open flux is not always associated with strong vertical magnetic elements.
登录
查看更多内容
DOI：
10.1017/cbo9780511546037.011
发表时间：
2000-04
期刊：
--
影响因子：
--
作者：
C. Schrijver;C. Zwaan
通讯作者：
C. Schrijver;C. Zwaan
影响因子：
1.8
作者：
Z. Fan;J. Ma;X. Z. N. A. Observatories;Chinese Academy of Sciences
通讯作者：
Z. Fan;J. Ma;X. Z. N. A. Observatories;Chinese Academy of Sciences
DOI：
10.1088/0004-637x/719/1/131
发表时间：
2008-12
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Hiroaki Ito;S. Tsuneta;D. Shiota;M. Tokumaru;K. Fujiki
通讯作者：
Hiroaki Ito;S. Tsuneta;D. Shiota;M. Tokumaru;K. Fujiki
影响因子：
6.5
作者：
A. Vögler;S. Shelyag;M. Schüssler;F. Cattaneo;T. Emonet;T. Linde
通讯作者：
A. Vögler;S. Shelyag;M. Schüssler;F. Cattaneo;T. Emonet;T. Linde
影响因子：
56.9
作者：
C. Tu;Cheng Zhou;E. Marsch;L. Xia;Liang Zhao;Jingxiu Wang;K. Wilhelm
通讯作者：
C. Tu;Cheng Zhou;E. Marsch;L. Xia;Liang Zhao;Jingxiu Wang;K. Wilhelm