| Literature DB >> 24027782 |
M Amenomori1, X J Bi, D Chen, T L Chen, W Y Chen, S W Cui, L K Ding, C F Feng, Zhaoyang Feng, Z Y Feng, Q B Gou, Y Q Guo, K Hakamada, H H He, Z T He, K Hibino, N Hotta, Haibing Hu, H B Hu, J Huang, H Y Jia, L Jiang, F Kajino, K Kasahara, Y Katayose, C Kato, K Kawata, G M Le, A F Li, H J Li, W J Li, C Liu, J S Liu, M Y Liu, H Lu, X R Meng, K Mizutani, K Munakata, H Nanjo, M Nishizawa, M Ohnishi, I Ohta, H Onuma, S Ozawa, X L Qian, X B Qu, T Saito, T Y Saito, M Sakata, T K Sako, J Shao, M Shibata, A Shiomi, T Shirai, H Sugimoto, M Takita, Y H Tan, N Tateyama, S Torii, H Tsuchiya, S Udo, H Wang, H R Wu, L Xue, Y Yamamoto, Z Yang, S Yasue, A F Yuan, T Yuda, L M Zhai, H M Zhang, J L Zhang, X Y Zhang, Y Zhang, Yi Zhang, Ying Zhang, X X Zhou.
Abstract
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.Year: 2013 PMID： 24027782 DOI： 10.1103/PhysRevLett.111.011101
Source DB: PubMed Journal: Phys Rev Lett ISSN： 0031-9007 Impact factor: 9.161