  We study the interior spacetimes of stars in the Palatini formalism of f(R)
gravity and derive a generalized Tolman-Oppenheimer-Volkoff and mass equation
for a static, spherically symmetric star. We show that matching the interior
solution with the exterior Schwarzschild-De Sitter solution in general gives a
relation between the gravitational mass and the density profile of a star,
which is different from the one in General Relativity. These modifications
become neglible in models for which $\delta F(R) \equiv \partial f/\partial R -
1$ is a decreasing function of R however. As a result, both Solar System
constraints and stellar dynamics are perfectly consistent with $f(R) = R -
\mu^4/R$.
