  In order to examine the pulse profile from a pulsar, we derive the formula
for describing the flux from antipodal hot spots with any static, spherically
symmetric spacetime. We find that the pulse profiles are almost independent of
the gravitational geometry outside the star when the compactness of neutron
stars is low enough, e.g., the stellar mass and radius are $1.4M_\odot$ and 14
km, respectively. On the other hand, the pulse profiles depend strongly on the
gravitational geometry when the compactness of neutron stars is so high, e.g.,
the stellar mass and radius are $1.8M_\odot$ and 10 km, respectively. Thus, one
may probe the spacetime geometry outside the star and even distinguish
gravitational theories via the observation of pulse profile with the help of
another observations for the stellar compactness, if the compactness of central
object is high enough. We also derive the 1st and 2nd order approximation of
the flux with respect to a parameter defined by the radio of the gravitational
radius of considered spacetime to the stellar radius. Then, we find that the
relative error from full order numerical results in the bending angle becomes
$\sim 20-30\%$ with the 1st order and $\sim 5-10\%$ with the 2nd order
approximations for a typical neutron star, whose mass and radius are
$1.4M_\odot$ and 12 km, respectively. Our results with the 1st order
approximation for the Schwarzschild spacetime are different from those obtained
in the literature, which suggests that the 1st order approximation has been
misunderstood to yield highly accurate prediction.
