Probe of the Solar Magnetic Field Using the "Cosmic-Ray Shadow" of the Sun
M. Amenomori, X. J. Bi, D. Chen, T. L. Chen, W. Y. Chen, S. W. Cui,, Danzengluobu, 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
TL;DR
This study uses the Sun's shadow in 10 TeV cosmic-ray flux over a solar cycle to evaluate coronal magnetic field models, finding the CSSS model aligns better with observations.
Contribution
First successful evaluation of coronal magnetic field models using the Sun's shadow in TeV cosmic-ray flux over a solar cycle.
Findings
Sun's shadow varies with the solar cycle
CSSS model better reproduces observed shadow variation
Shadow intensity is sensitive to magnetic field structure
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 (PFSS) 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.
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