Probe of the solar magnetic field using the "cosmic-ray shadow" of the sun.
Probe of the solar magnetic field using the "cosmic-ray shadow" of the sun.
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DOI：
10.1103/physrevlett.111.011101
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发表时间：
2013-06
影响因子：
8.6
通讯作者：
M. Amenomori;X. Bi;D. Chen;T. Chen;W. Chen;S. Cui;Danzengluobu;L. Ding;C. Feng;Zhaoyang Feng;Z. Feng;Q. Gou;Y. Guo;K. Hakamada;H. He;Z. He;K. Hibino;N. Hotta;Haibing Hu;H. Hu;J. Huang;H. Jia;L. Jiang;F. Kajino;K. Kasahara;Y. Katayose;C. Kato;K. Kawata;Labaciren;G. Le;A. Li;H. Li;W. Li;C. Liu;J. Liu;M. Liu;H. Lu;X. Meng;K. Mizutani;K. Munakata;H. Nanjo;M. Nishizawa;M. Ohnishi;I. Ohta;H. Onuma;S. Ozawa;X. Qian;X. Qu;T. Saito;T. Saito;M. Sakata;T. Sako;J. Shao;M. Shibata;A. Shiomi;T. Shirai;H. Sugimoto;M. Takita;Y. Tan;N. Tateyama;S. Torii;H. Tsuchiya;S. Udo;Hong Wang;H. Wu;L. Xue;Y. Yamamoto;Z. Yang;S. Yasue;A. Yuan;T. Yuda;L. Zhai;H. Zhang;J. Zhang;X. Zhang;Y. Zhang;Yi. Zhang;Ying Zhang;Zhaxisangzhu;X. Zhou
中科院分区：
文献类型：
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作者：
M. Amenomori;X. Bi;D. Chen;T. Chen;W. Chen;S. Cui;Danzengluobu;L. Ding;C. Feng;Zhaoyang Feng;Z. Feng;Q. Gou;Y. Guo;K. Hakamada;H. He;Z. He;K. Hibino;N. Hotta;Haibing Hu;H. Hu;J. Huang;H. Jia;L. Jiang;F. Kajino;K. Kasahara;Y. Katayose;C. Kato;K. Kawata;Labaciren;G. Le;A. Li;H. Li;W. Li;C. Liu;J. Liu;M. Liu;H. Lu;X. Meng;K. Mizutani;K. Munakata;H. Nanjo;M. Nishizawa;M. Ohnishi;I. Ohta;H. Onuma;S. Ozawa;X. Qian;X. Qu;T. Saito;T. Saito;M. Sakata;T. Sako;J. Shao;M. Shibata;A. Shiomi;T. Shirai;H. Sugimoto;M. Takita;Y. Tan;N. Tateyama;S. Torii;H. Tsuchiya;S. Udo;Hong Wang;H. Wu;L. Xue;Y. Yamamoto;Z. Yang;S. Yasue;A. Yuan;T. Yuda;L. Zhai;H. Zhang;J. Zhang;X. Zhang;Y. Zhang;Yi. Zhang;Ying Zhang;Zhaxisangzhu;X. Zhou
我们报告了一个明确的太阳周期变化的太阳阴影在10 TeV宇宙线通量观测的西藏空气簇射阵列在一个完整的太阳周期从1996年到2009年。为了阐明观测到的太阳周期变化的物理意义，我们开发了太阳阴影的数值模拟，使用势场源表面模型和电流片源表面（CSSS）模型的日冕磁场。我们发现，模拟的太阳阴影中的强度亏损是非常敏感的日冕磁场结构，和观测到的太阳阴影的变化更好地再现了CSSS模型。这是首次利用TeV宇宙线流中观测到的太阳阴影来评估日冕磁场模型的成功尝试。
We report on a clear solar-cycle variation of the Sun’s shadow in the 10 TeV cosmic-ray flux observed by the Tibet air shower array during a full solar cycle from 1996 to 2009. In order to clarify the physical implications of the observed solar cycle variation, we develop numerical simulations of the Sun’s shadow, using the potential field source surface model and the current sheet source surface (CSSS) model for the coronal magnetic field. We find that the intensity deficit in the simulated Sun’s shadow is very sensitive to the coronal magnetic field structure, and the observed variation of the Sun’s shadow is better reproduced by the CSSS model. This is the first successful attempt to evaluate the coronal magnetic field models by using the Sun’s shadow observed in the TeV cosmic-ray flux.