Electromagnetic energy flux from the solar wind in to the Earth's magnetosphere

There are well-known functions of the solar wind - magnetosphere coupling of type F(Xi) where Xi are the observed (measured) parameters which can presumably influence on energy and impulse transferred into the magnetosphere from the solar wind. Some of the functions give estimates of the energy flux (thereinafter Poynting flux, e), e.g., e=ea is the Poynting flux from [1]. The various functions F(Xi) use wide set of the observed parameters Xi but even the best of these functions are not sufficient. In this connection, the authors of this study suggest a new method of calculation of the Poynting flux e=e*, based on the parameters 4> and BL, which are available presently from the ground-based and satellite measurements, but were not used earlier. Here 4> and BL are the magnetic flux through the polar cap and the magnetic field in the tail lobe, respectively. The first tests of the new method gave the promising results: a) the correlation of e* with appropriate observed data was found to be higher than that of ea; b) the calibrating coefficient in equation for e*, in contrast to those for ea, can be calculated as the function of the variable boundary and intra-magnetosphere conditions.