The solar wind is the complex, dynamical outflow of high-energy particles that emanates from the Sun's surface and permeates the solar system, thus playing a significant role in influencing the near-Earth space environment. The processes that accelerate and heat the solar wind are a topic of vigorous debate among scientists, but it is generally acknowledged that chaotic, turbulent motions on the solar surface play a role in injecting energy into the solar atmosphere, which then becomes available to heat and accelerate the particles. This study employs observations of the magnetic field on the solar surface (the photosphere) to study the properties of turbulence at the inception of the solar wind. We show the distribution of turbulent structures of various sizes over the photosphere, and demonstrate that this spatial distribution follows mathematical laws that are also found in other turbulent systems observed in nature. These results will help researchers improve models of of the solar wind and also help us better understand the role played by turbulence in stars beyond our own Sun.