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The radio and gamma-ray pulsar PSR J2032+4127 was recently found to be in adecades-long orbit with the Be star MT91 213, with the pulsar moving rapidlytowards periastron. This binary shares many similar characteristics with thepreviously unique binary system PSR B1259-63/LS 2883. Here, we describe radio,X-ray, and optical monitoring of PSR J2032+4127/MT91 213. Our extended orbitalphase coverage in radio, supplemented with Fermi gamma-ray data, allows us toupdate and refine the orbital period to 45-50 yr and time of periastron passageto 2017 November. We analyse archival and recent Chandra and Swift observationsand show that PSR J2032+4127/MT91 213 is now brighter in X-rays by a factor of~70 since 2002 and ~20 since 2010. While the pulsar is still far fromperiastron, this increase in X-rays is possibly due to collisions betweenpulsar and Be star winds. Optical observations of the Halpha emission line ofthe Be star suggest that the size of its circumstellar disc may be varying by~2 over timescales as short as 1-2 months. Multiwavelength monitoring of PSRJ2032+4127/MT91 213 will continue through periastron passage, and the systemshould present an interesting test case and comparison to PSR B1259-63/LS 2883.

Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to periastron