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LS I +61 303 is one of the most studied X-ray binary systems because of itstwo peculiarities: On the one hand being the probable counterpart of thevariable gamma ray source 2CG 135+01 (Gregory and Taylor 1978; Tavani et al.1998) and on the other hand being a periodic radio source (Taylor and Gregory1982). The recent discovery of a radio emitting jet extending ca. 200 AU atboth sides of a central core (Massi et al. 2004) in all evidence has shown theoccurrence of accretion/ejection processes in this system. However, the radiooutbursts do not occur at periastron passage, where the accretion is at itsmaximum, but several days later. In addition, when the gamma-ray emission of2CG 135+01 is examined along the orbital phase of LS I +61 303 one sees thatthis emission seems to peak at periastron passage (Massi 2004). Here in detailwe analyse the trend of the gamma-ray data versus orbital phase and discuss thedelay between peaks at gamma-rays and in the radio band within the framework ofa two-peak accretion/ejection model proposed by Taylor et al. (1992) andfurther developed by Marti' and Paredes (1995).Comment: To be published in the proceedings of the Symposium on High-Energy  Gamma-Ray Astronomy, Heidelberg, July 26-30, 2004 (AIP Proceedings Series

The gamma-ray emitting microquasar LS I +61 303