GeV flares from PSR B1259-63/LS 2883 were seen starting around 30 days after the two periastron passages in 2010 and 2014. The flares are clearly delayed compared to the occurrence of the X-ray and TeV flux peaks during the post-periastron disk crossing. While several attempts have been put forward to explain this phenomenon, the origin of these GeV flares remains a puzzle. Here we present a detailed analysis of the observational data taken by the Fermi and Swift observatories over the 2017 September periastron passage. For the first time, we find short-lived but powerful GeV flares on time scales of down to three hours. The onset of the GeV flaring period in 2017 is also delayed compared to those seen in 2011 and 2014. Supplemented by a re-analysis of previous data, we compare the Fermi/LAT, Swift/XRT and Swift/UVOT light curves in 2017 with those taken over the 2010 and 2014 periastrons, and difference in UVOT light curves are noted.
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