High rigidity cosmic rays in the TeV range offer a unique tool in the exploration of the magnetic field structure close to the Sun. TeV protons are essentially unmodulated at Earth’s orbit but can be significantly deflected by the strong magnetic fields near the Sun. Cosmic rays hitting the Sun are absorbed and create a cosmic ray shadow that has been detected and studied in detail by air-shower observations in the multi TeV range. Cosmic rays can also interact with matter near the solar surface and create gamma rays that are observed by the Fermi LAT instrument. Both the Sun’s shadow and solar gammas exhibit a marked solar cycle dependence sharing some common features. In this work we perform numerical simulations to estimate the energy dependence of cosmic ray flux near the Sun that can create gammas to be seen at Earth from different solar latitudes. We consider particle transport in a simple model of the Sun including regions of open and closed magnetic fluxes.