  Accretion models predict two ejections along the eccentric orbit of LS I +61
303: one major ejection at periastron and a second, lower ejection towards
apastron. We develop a physical model for LS I +61 303 in which relativistic
electrons are ejected twice along the orbit. The ejecta form a conical jet that
is precessing with P2. The jet radiates in the radio band by the synchrotron
process and the jet radiates in the GeV energy band by the external inverse
Compton and synchrotron self-Compton processes. We compare the output fluxes of
our physical model with two available large archives: OVRO radio and Fermi
Large Area Telescope (LAT) GeV observations, the two databases overlapping for
five years. The larger ejection around periastron passage results in a slower
jet, and severe inverse Compton losses result in the jet also being short.
While large gamma-ray emission is produced, there is only negligible radio
emission. Our results are that the periastron jet has a length of 3.0 10^6 rs
and a velocity beta ~ 0.006, whereas the jet at apastron has a length of 6.3
10^7 rs and beta ~ 0.5.
