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Fig. 1

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Difference between the transit light curves of an ellipsoidal and a spherical planet, for some real close-in planets with different inclinations and distances to the star (Table 1). The red line shows the difference obtained with our model (Eq. (19)), while the blue line is obtained for an oblate planet with a = bc, both with stellar uniform flux. The dashed line also corresponds to the difference obtained with our model, but using a quadratic stellar limb-darkening correction I(μ) /I(1) = 1−0.4830(1 − μ) − 0.2023(1 − μ)2, which corresponds to a stellar temperature of 5500 K (Sing 2010).

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