(C+O) star-neutron star close binary system is a progenitor of soft gamma-ray repeater?

We consider a close binary system with separation similar or equal to 0.2 R(x) which consists of a (C + O) star of mass similar or equal to 4 M(.) and a neutron star as a progenitor of soft gamma-ray repeater (SGR) and a high velocity pulsar. The (C + O) star was tidally locked before the supernova explosion so that it has spin angular momentum large enough to be a rapidly rotating pulsar which will make a supernova remnant a plerion. After the event of the supernova explosion, both new and old neutron stars have high relative velocity of similar or equal to 1000 km s(-1) to the center of mass of the ejecta. SGR activities can be induced by the episodic accretion of the supernova ejecta onto the old neutron star. The episodic accretion scenario onto the old neutron star predicts that SGR source should be located in the different position from the observed plerion-like object. Future observations with fine positional resolution can clarify the position ambiguity between the gamma ray and X-ray sources.