Ian Wong et al have produced a new analysis of the TESS data on previously known WASP exoplanets. Their main interest is the “phase curve”, the variation of the light around the planet’s orbit.

Two examples are the systems WASP-72 and WASP-100:

In addition to the main transit (planet passing in front of the star) the phase curves show secondary eclipses (planet passing behind the star, at phase 0.5) and a sinusoidal variation due to the heated face of the planet. By modelling the phase-curves of these and other similar planets, Wong et al make the tentative suggestion that the hotter the planet (which can be measured from the depth of the secondary eclipse) the more reflective the atmosphere of the planet is.

Here’s a similar plot for WASP-30. Note, though, that the phase-curve variation peaks at phases 0.25 and 0.75, unlike those for WASP-72 and WASP-100. That’s because WASP-30b is not a planet but a brown dwarf, with a mass of 63 Jupiters. That is massive enough for its gravity to distort the host star into an ellipsoidal shape, and so in this system the variation of the light is caused by the varying projection of the distorted star around the orbit.