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A Statistical Inference Method for Interpreting the CLASP Observations

  • Authors: J. Štěpán, J. Trujillo Bueno, L. Belluzzi, A. Asensio Ramos, R. Manso Sainz, T. del Pino Alemán, R. Casini, R. Kano, A. Winebarger, F. Auchère, R. Ishikawa, N. Narukage, K. Kobayashi, T. Bando, Y. Katsukawa, M. Kubo, S. Ishikawa, G. Giono, H. Hara, Y. Suematsu, T. Shimizu, T. Sakao, S. Tsuneta, K. Ichimoto, J. Cirtain, P. Champey, B. De Pontieu, and M. Carlsson

2018 The Astrophysical Journal 865 48.

  • Provider: AAS Journals

Caption: Figure 1.

CLASP observations of the intensity (top panel), Q/I (middle panel), and U/I (bottom panel) line-center signals of the hydrogen Lyα line. Each point corresponds to a pixel along the slit of the spectrograph with its corresponding value for the cosine of the heliocentic angle, μ. The reference direction for the positive Stokes Q is the parallel to the nearest limb. The dashed curve in the middle panel shows the CLV of the Q/I line-center signal calculated by Trujillo Bueno et al. (2011) in the semi-empirical model C of Fontenla et al. (1993), while the dotted curve shows the CLV of the ﹩\langle Q\rangle /\langle I\rangle ﹩ line-center signal calculated by Štěpán et al. (2015) in the 3D MHD model of Carlsson et al. (2016; with the symbol ﹩\langle ...\rangle ﹩ meaning spatial average at each μ position). We note that the standard deviation of the observed Q/I and U/I signals due to the presence of noise is σ = 0.05%, i.e., comparable to the vertical size of the data markers in the plot.

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