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We study the relation between luminosity and spin-period change in X-raybinary pulsars using long-term light curve obtained by the MAXI/GSC all-skysurvey and pulse period data from the Fermi/GBM pulsar project. X-ray binaries,consisting of a highly magnetized neutron star and a stellar companion,originate X-ray emission according to the energy of the accretion matter ontothe neutron star. The accretion matter also transfers the angular momentum atthe Alfven radius, and then spin up the neutron star. Therefore, the X-rayluminosity and the spin-up rate are supposed to be well correlated. We analyzedthe luminosity and period-change relation using the data taken by continuousmonitoring of MAXI/GSC and Fermi/GBM for Be/X-ray binaries, GX 304$-$1, A0535$+$26, GRO J1008$-$57, KS 1947$+$300, and 2S 1417$-$624, which occurredlarge outbursts in the last four years. We discuss the results comparing theobtained observed relation with that of the theoretical model by Ghosh \& Lamb(1979).

Study of luminosity and spin-up relation in X-ray binary pulsars with long-term monitoring by MAXI/GSC and Fermi/GBM