ИСТИНА

The article by Zhilkin and Bisikalo describes the MHD modelling of magnetospheres of hot Jupiters located near the Alfvén point of the stellar wind of their host stars, where the Alfvén Mach number is equal to 1. In particular, the authors model the magnetosphere of the exoplanet HD 209458 b, also known by the unofficial name Osiris. Since this exoplanet lies in the boundary region between regimes of stellar wind flow with Alfvén Mach numbers greater and less than one, both super-Alfvénic and sub-Alfvénic cases are considered correspondingly. Previously, we conducted a simulation of the magnetosphere of HD 209458 b using the analytical paraboloid magnetospheric model, so it is reasonable to compare the results obtained with the paraboloid model to those presented by Zhilkin and Bisikalo MHD simulations. Despite methodological differences, the results show overall agreement in the large-scale structure of the magnetosphere of HD 209458 b. The paraboloid model provides a qualitative presentation of the geometry and orientation of magnetospheric magnetic field structure, serving as a convenient tool for preliminary analysis, while the MHD approach allows for a deeper investigation of physical processes related to plasma flow redistribution and the emergence of local instabilities.