  It is now established that the hot Jupiters have extensive gaseous
(ionospheric) envelopes, which expanding far beyond the Roche lobe. The
envelopes are weakly bound to the planet and affected by strong influence of
stellar wind fluctuations. Also, the hot Jupiters are located close to the
parent star and therefore the magnetic field of stellar wind is an important
factor, determining the structure their magnetosphere. At the same time, for a
typical hot Jupiter, the velocity of stellar wind plasma, flowing around the
atmosphere, is close to the Alfv\'en velocity. This should result in stellar
wind parameters fluctuations (density, velocity, magnetic field), that can
affect the conditions of formation of bow shock waves around a hot Jupiter, i.
e. to switch flow from sub-Alfv\'en to super-Alfv\'en mode and back. In this
paper, based on the results of three-dimensional numerical MHD modeling, it is
confirmed that in the envelope of hot Jupiter, which is in Alfv\'en point
vicinity of the stellar wind, both disappearance and appearance of the bow
shock wave occures under the action of coronal mass ejection. The paper also
shows that this effect can influence the observational manifestations of hot
Jupiter, including luminosity in energetic part of the spectrum.
