GASEOUS ENVELOPES OF HOT JUPITERS
Hot Jupiter, i.e., exoplanet with masses comparable to the mass of the Jupiter, and semimajor axis of the orbit less then 0.1 a. u., are a unique class of objects, since the formation of their gas envelopes strongly influenced by the parent star gravity. The atmospheres of planets of this type usually fills its Roche lobes, leading to powerful outflow of matter from the planet to the star. The energetics of this process is so high that it is determinative in the gas envelope formation. From the presented analytical estimates and the results of three-dimensional calculations, follows that the gaseous envelope of hot Jupiter can be substantially non-spherical, while remaining stationary and long-lived. The presented results are important for the interpretation of the observational data, because the asymmetry of the envelope requires the involvement of new approaches to the estimation of the properties of the atmospheres of hot Jupiter.