<p>The nature of dark matter (DM) and its effects on Milky Way galactic evolution are outstanding problems in astrophysics, space science, and cosmology. Quantitative models for the distribution of DM in the solar system are needed to clarify the role of DM in the Milky Way and to enable and guide direct and indirect DM detection searches. The dynamics, energetics, and composition of the solar corona are important elements in the Sun-heliosphere connection. By adopting a kinetic collisionless approach, we present the first quantitative model for the spatial distribution of DM in the solar corona. Our results show that the predicted DM mass density can be a fraction of plasma mass densities predicted by models of the solar corona. We find that the DM density in the lower corona is mass-dependent with the largest DM density occurring for a DM mass on the order of several proton masses.</p>