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PSR J2032+4127/ MT91 213 was identified as a pulsar/Be-star binary through radio and gamma-ray timing observations (Lyne et al. MNRAS 451 581 2015 Ho et al. MNRAS 464 1211H 2017). It has recently enhanced flux across the spectrum from Optical to TeV gamma-ray that are apparently associated with the upcoming periastron passage. The orbit of of PSR J2032+4127/ MT91 213 is highly eccentric (45 yrs < p < 50 yrs and 0.96 < e < 0.99) and is expected to reach periastron sometime around November 2017. Enhanced activity is expected before and after the periastron passage and flaring events are also expected as the pulsar moves through the stellar disk. This system is near in the sky to unknown gamma-ray source TeV J2032+4130 which is thought to be the pulsar wind nebulae (PWN) counterpart of PSR J2032+4127 (Aliu et al. ApJ 783 16 2014). This rare event may help to determine if the TeV source is associated with a component in this binary system.Recent TeV gamma-ray observations from VERITAS and MAGIC have been summarized in an Astronomers Telegram on October 2 2017 (http://www.astronomerstelegram.org ATel #10810). The recent optical/UV/x-ray observations from Swift-XRT Swift-UVOT and 2m Liverpool Telescope are summarized in an Astronomers Telegram on October 15 2017 (ATel #10851). Observations taken prior to July 2017 by VERITAS did not detect the binary system and the x-ray flux detected by Swift-XRT has been slowly increasing over the past year (Bird et al. arXiv:1708.04718 and Li et al. ApJ 843 85L 2017). More recent observations in September 2017 by VERITAS show that the flux measured in TeV gamma-rays has doubled to 4.2e-12 photons/cm2/s (above 200 GeV) resulting in a significant detection at the location of the pulsar and is expected to increase further. More recent observations from Swift-XRT in October 2017 show that the x-ray flux (0.3-10keV) has increased at least 5 times average fl [truncated! Please see actual data for full text]