From Kepler’s third law for two-body motion,
\[
T=2\pi\sqrt{\frac{a^{3}}{\mu}},
\]
where $T$ is the orbital period, $a$ the semi-major axis, and $\mu$ Earth’s gravitational parameter. $T$ depends only on $a$ (for a given central body), not on eccentricity or inclination. Hence (A).