Figure 6 from A Statistical Inference Method for Interpreting the CLASP Observations

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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 6.

Motivation for the CTR model. The physical quantities of the TR of geometrical thickness D in which the Lyα line core forms vary much faster along the local TR normal vector ﹩{\boldsymbol{n}}﹩ than along the perpendicular direction. Therefore, we approximate the line-core formation region using an inclined plane-parallel model whose normal vector ﹩{\boldsymbol{n}}﹩ makes an angle θ_n with respect to the local vertical direction Z. The quantity L is of the order of the local radius of curvature of the TR.

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