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We present the Neil Gehrels Swift Observatory (Swift), Fermi Large AreaTelescope (Fermi-LAT), and Karl G. Jansky Very Large Array (VLA) observationsof the gamma-ray binary PSR J2032+4127/MT91 213, of which the periastronpassage has just occurred in November 2017. In the Swift X-ray light curve, theflux was steadily increasing before mid-October 2017, however, a sharp X-raydip on a weekly time-scale is seen during the periastron passage, followed by apost-periastron X-ray flare lasting for ~20 days. We suggest that the X-ray dipis caused by (i) an increase of the magnetization parameter at the shock, and(ii) the suppression due to the Doppler boosting effect. The 20-daypost-periastron flare could be a consequence of the Be stellar disk passage bythe pulsar. An orbital GeV modulation is also expected in our model, however,no significant variability is seen in the Fermi-LAT light curve. We suspectthat the GeV emission resulted from the interaction between the binary'smembers is hidden behind the bright magnetospheric emission of the pulsar.Pulsar gating technique would be useful to remove the magnetospheric emissionand recover the predicted GeV modulation, if an accurate radio timing solutionover the periastron passage is provided in the future.

The X-ray modulation of PSR J2032+4127/MT91 213 during the Periastron Passage in 2017