Using the PPMLR‐MHD global simulation model, we examined the Kelvin‐Helmholtz (K‐H) instability at the low‐latitude boundary layer (LLBL) under northward interplanetary magnetic field (IMF) conditions with various solar wind speeds (400, 600, and 800 km/s). The spatial distribution of the K‐H wave power in the equatorial plane shows two distinct power populations, referring to the two modes of K‐H surface waves. The spatial evolution of K‐H instability at the boundary layer is classified into four phases: quasi‐stable, exponential growth, linear growth, and nonlinear phases. The boundary layer is quasi‐stable near the subsolar point region. The K‐H instability starts at about 30° longitude, and grows exponentially with a spatial growth rate of 0.28∼0.87 RE−1until ∼45° longitude where the vortices fully develop. At larger longitudes, the instability grows linearly, while the vortices grow in size. From ∼80° longitude to the distant magnetotail, the K‐H instability develops nonlinearly and the vortices roll up. The wave frequency, wavelength, and phase speed are given at various spatial points. Model results show that the higher solar wind speed generates K‐H waves with higher frequency under the northward IMF, and the wavelengths and the phase speeds increase with the increase of the longitude. Moreover, we made a comparison of the K‐H wave periods on Earth's, Mercury's and Saturn's magnetopauses by a proposed prediction method.