We study the dependence of the electric field at the magnetopause on the parameters of the solar wind for the southward interplanetary magnetic field. For the magnetic reconnection region, we use the Hall MHD model with Bohm-type resistivity in the diffusion region. In this case, the spatial change in resistivity is modeled by the Gaussian function. The reconnection rate was found as a decreasing function of the plasma beta parameter, which was used to match the reconnection region with the dayside magnetosheath parameters determined from a numerical MHD model of the solar wind flow around the magnetopause. The magnetosheath solution gives radial profiles of the ratio of the normal velocity to the local Alfvén speed. At the magnetopause, this ratio should be equal to the reconnection rate calculated in the diffusion region. This condition gives the magnetic field strength and electric field at the magnetopause.