  PSR B1259-63/SS2883 is a binary system which consists of a 48-ms radio pulsar
and a massive star in a highly eccentric orbit with a period of about 3.4
years. Non-pulsed and non-thermal emissions from this binary have been reported
in the radio, X-ray and TeV gamma-ray energy ranges. Light curves in the radio
and X-ray bands showed characteristic double-peaked features which can be
attibuted to the interactions of the pulsar wind and the Be disk during the
crossings by the pulsar. The TeV light curves around periastron differ between
2004 and 2007 observations, and the feature is not conclusive. We report a
detection of GeV gamma-ray emission around the periastron passage in December
2010 with Fermi-LAT.
