Suppression of convection around small magnetic concentrations
Suppression of convection around small magnetic concentrations
复制标题
DOI：
10.1051/0004-6361:20079029
复制
发表时间：
2008-04
影响因子：
6.5
通讯作者：
S. Morinaga;T. Sakurai;K. Ichimoto;T. Yokoyama;M. Shimojo;Y. Katsukawa
中科院分区：
文献类型：
--
作者：
S. Morinaga;T. Sakurai;K. Ichimoto;T. Yokoyama;M. Shimojo;Y. Katsukawa
目标。众所周知，光球层中的对流运动受到磁场的抑制。然而，由于可获得的空间分辨率(∼1��)，利用偏振测量来研究对流与诸如G带亮点(GBPS)或气孔等微小磁性特征之间的相互作用一直是困难的。Hinode卫星上的光谱偏振仪(SP)的出现改变了这种情况，它的偏振度为0。��3空间分辨率。方法：研究方法。我们分析了NOAA 10940中圆盘中心附近的气孔及其周围区域。通过对Stokes分布的Milne-Eddington反演求出场强和填充因子。通过线芯的移动，我们还得到了视线速度。利用这些物理参数，我们研究了抑制对流所需的物理条件。结果。我们发现，对流被抑制，而不是磁场本身的强度，而是高浓度的磁通管。我们还发现，Gbps和气孔的区别在于填充因子(F)；f�0。6f或Gbps，孔的f=0.8-0.9。
Aims. It is well known that convective motions in the photosphere are suppressed by magnetic fields. However, it has been difficult to study the interaction between convection and small magnetic features, such as G-band bright points (GBPs) or pores with polarimetric measurements, because of the available spatial resolution (∼1 �� ). This situation is changed by the advent of the SpectroPolarimeter (SP) aboard the Hinode satellite, which has 0. �� 3 spatial resolution. Methods. We analyzed the pore and its surrounding region in NOAA 10940 near the disk center. We obtained the field strength and filling factor through the Milne-Eddington inversion of the Stokes profiles. We also derived the line-of-sight velocity by the shift of the line core. Using these physical parameters, we investigated the physical conditions needed to suppress the convection. Results. We found that the convection is suppressed, not by the strength of the magnetic field itself, but by high concentration of magnetic flux tubes. We also found that GBPs and pores are distinguished in terms of the filling factor (f ); f � 0. 6f or GBPs and f = 0.8–0.9 for pores.