In the first part of my talk I will review the most important
effects and processes in the atmospheres of close-in giant extrasolar
planets which may be relevant for understanding/interpreting various
observations of transits, secondary eclipses and phase light-curves.
In the second part I will point out similarities between interacting
binary stars and stars with a close-in giant extrasolar planet. The
reflection effect is a well-known example. Although the generally accepted
treatment of this effect in interacting binaries is successful in fitting
light curves of eclipsing binaries, it is not very suitable for studying
cold objects irradiated by hot objects or extrasolar planets. Our model of
the reflection effect takes into account the reflection (scattering),
heating, and heat redistribution over the surface of the irradiated
object. The shape of the object is described by the non-spherical Roche
potential
expected for close objects. Limb and gravity darkening are included in the
calculations of the light output from the system. The model also accounts
for the orbital revolution and rotation of the exoplanet with appropriate
Doppler shifts for the scattered and thermal radiation. Subsequently,
light curves and/or spectra of several exoplanets have been modelled and
the effects of the heat redistribution, limb darkening/brightening,
(non-)gray albedo, and non-spherical shape have been studied. It was found
that departures from the spherical shape can reach 14% (WASP-12b).
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