MODELING THE SUN’S SMALL-SCALE GLOBAL PHOTOSPHERIC MAGNETIC FIELD
MODELING THE SUN’S SMALL-SCALE GLOBAL PHOTOSPHERIC MAGNETIC FIELD
复制标题
太阳小尺度全球光球磁场建模
DOI：
10.3847/0004-637x/830/2/160
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
D. Mackay
中科院分区：
文献类型：
--
作者：
Karen A. Meyer;D. Mackay
我们提出了一个新的模型，太阳的全球光球磁场在一个深的最低限度的活动，其中没有活跃的地区出现。整个太阳表面的小尺度磁功能的出现和随后的演变进行了模拟，受到全球超颗粒流模式的影响。从视觉上看，由此产生的模拟磁图再现了在安静的太阳磁图中观察到的典型结构和尺度。定量地，模拟很快达到稳定状态，导致平均场和通量分布与观测结果一致。一个潜在的日冕磁场外推从模拟完整的太阳磁图考虑这样一个安静的光球磁场的日冕和内日球层的影响。日冕磁场的大部分在模拟的磁网络中的小尺度特征之间的短连接中关闭得非常低。只有0.1%的光球磁通量被发现在2.5 R处是开放的，比典型的日震和磁成像仪天气图观测结果小10-100倍。如果太阳上存在这样的条件，这将导致行星际磁场比目前观测到的要弱得多，因此地球上的宇宙射线通量要高得多。
We present a new model for the Sun’s global photospheric magnetic field during a deep minimum of activity, in which no active regions emerge. The emergence and subsequent evolution of small-scale magnetic features across the full solar surface is simulated, subject to the influence of a global supergranular flow pattern. Visually, the resulting simulated magnetograms reproduce the typical structure and scale observed in quiet Sun magnetograms. Quantitatively, the simulation quickly reaches a steady state, resulting in a mean field and flux distribution that are in good agreement with those determined from observations. A potential coronal magnetic field is extrapolated from the simulated full Sun magnetograms to consider the implications of such a quiet photospheric magnetic field on the corona and inner heliosphere. The bulk of the coronal magnetic field closes very low down, in short connections between small-scale features in the simulated magnetic network. Just 0.1% of the photospheric magnetic flux is found to be open at 2.5 R⊙, around 10–100 times less than that determined for typical Helioseismic and Magnetic Imager synoptic map observations. If such conditions were to exist on the Sun, this would lead to a significantly weaker interplanetary magnetic field than is currently observed, and hence a much higher cosmic ray flux at Earth.
影响因子：
2.8
作者：
Meyer K
通讯作者：
Meyer K