  A report is made on the luminosity and pulse-period evolution of the Be
binary X-ray pulsar, GX 304$-$1, during a series of outbursts from 2009 to 2013
observed by MAXI/GSC, RXTE/PCA, and Fermi/GBM. In total, twelve outbursts
repeated by $\sim$ 132.2 days were observed, which is consistent with the X-ray
periodicity of this object observed in the 1970s. These 12 outbursts, together
with those in the 1970s, were found to all recur with a well defined period of
132.189$\pm$0.02 d, which can be identified with the orbital period. The pulse
period at $\sim 275$ s, obtained from the RXTE/PCA and Fermi/GBM data,
apparently exhibited a periodic modulation synchronized with the outburst
period, suggesting the pulsar orbital motion, which is superposed on a secular
spin-up trend throughout the entire active phase. The observed pulse-period
changes were successfully represented by a model composed of the binary orbital
modulation and pulsar spin up caused by mass accretion through an accretion
disk. The orbital elements obtained from the best-fit model, including the
projected orbital semi-major axis $a_{\rm x}\sin i \simeq 500-600$ light-s and
an eccentricity $e \simeq 0.5$, are typical of Be binary X-ray pulsars.
