Using the Meteor M2 low-orbit satellite, the dynamics of the boundaries of the auroral oval on the nightside during the magnetic storm observed from May 27 to 29, 2017, was studied. The dependence of the position of the boundaries during different phases of the storm on the state of the magnetosphere as well as interplanetary medium was studied. The experimentally obtained data on the boundaries of the auroral electron precipitation region were compared with data calculated using a statistical model developed independently and determining the position of the oval depending on the magnitude of the AL index. It was found that, during the initial phase of the storm, the main factor that influenced the further dynamics of the oval was a powerful prolonged pulse of solar wind pressure, which, in combination with a stable southward interplanetary magnetic field (IMF), led to compression of the magnetosphere and a decrease in the area of the polar cap and expansion of the equatorial oval boundaries. During the main and recovery phases of the storm, the solar wind pressure returned to prestorm levels, and the dynamics of the oval boundaries was associated with substorm activity and changes in the Bz components of the interplanetary magnetic field: the southward direction of the IMF during the main phase led to a shift of the oval to lower latitudes, and a gradual decrease in the modulus of the southward component caused a poleward shift of the oval in the recovery phase. It is shown that the polar boundary of the oval directly responds to changes in the solar wind, while the dynamics of the equatorial boundary contains features associated with geomagnetic activity and with the development of magnetospheric current systems indirectly controlled by the parameters of the interplanetary medium, in particular, by the intensity of large-scale convection.