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To observationally study spin-period changes of accreting pulsars caused bythe accretion torque, the present work analyzes X-ray light curves of 12 Bebinary pulsars obtained by the MAXI/GSC all-sky survey and their pulse periodsmeasured by the Fermi/GBM pulsar project, both covering more than 6 years from2009 August to 2016 March. The 12 objects were selected because they areaccompanied by clear optical identification, and accurate measurements ofsurface magnetic fields. The luminosity $L$ and the spin-frequency derivatives$\dot{\nu}$, measured during large outbursts with $L\gtrsim 1\times 10^{37}$erg s$^{-1}$, were found to approximately follow the theoretical relations inthe accretion torque models, represented by $\dot{\nu} \propto L^{\alpha}$($\alpha\simeq 1$), and the coefficient of proportionality between $\dot{\nu}$and $L^{\alpha}$, agrees, within a factor of $\sim 3$, with that proposed byGhosh & Lamb (1979). In the course of the present study, the orbital elementsof several sources were refined.

Correlation between the luminosity and spin-period changes during outbursts of 12 Be binary pulsars observed by the MAXI/GSC and the Fermi/GBM