Figure 6 from Asteroseismic Determination of Obliquities of the Exoplanet Systems Kepler-50 and Kepler-65

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Asteroseismic Determination of Obliquities of the Exoplanet Systems Kepler-50 and Kepler-65

Authors: W. J. Chaplin, R. Sanchis-Ojeda, T. L. Campante, R. Handberg, D. Stello, J. N. Winn, S. Basu, J. Christensen-Dalsgaard, G. R. Davies, T. S. Metcalfe, L. A. Buchhave, D. A. Fischer, T. R. Bedding, W. D. Cochran, Y. Elsworth, R. L. Gilliland, S. Hekker, D. Huber, H. Isaacson, C. Karoff, S. D. Kawaler, H. Kjeldsen, D. W. Latham, M. N. Lund, M. Lundkvist, G. W. Marcy, A. Miglio, T. Barclay, and J. J. Lissauer

Chaplin et al. 2013 The Astrophysical Journal 766 101.

Provider: AAS Journals

Caption: Figure 6.

Intensity perturbations for l = 1 mode components, at a phase corresponding to extreme displacement of the oscillations. Plotted are patterns for m = 1 (left-hand column) and m = 0 (right-hand column) modes viewed at different angles, i _s = 90° (top row), 60° (second row), 30° (third row), and 0° (bottom row). The filled circles mark the pole of the rotation axis and the lines the stellar equator.

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