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We study the geometry and dynamics of the Vela complex including the Velasupernova remnant (SNR), the binary system gamma2 Velorum and the Gum nebula.We show that the Vela SNR belongs to a subclass of non-Sedov adiabatic remnantsin a cloudy interstellar medium (ISM), the dynamics of which is determined bythe heating and evaporation of ISM clouds. We explain observablecharacteristics of the Vela SNR with a SN explosion with energy 1.4 x 10^50ergs near the step-like boundary of the ISM with low intercloud densities (~10^{-3} cm^{-3}) and with a volume-averaged density of clouds evaporated byshock in the north-east (NE) part about four times higher than the one in thesouth-west (SW) part. The observed asymmetry between the NE and SW parts of theVela SNR could be explained by the presence of a stellar wind bubble (SWB)blown by the nearest-to-the Earth Wolf-Rayet (WR) star in the gamma2 Velorumsystem. We show that the size and kinematics of gamma2 Velorum SWB agree withpredictions of numerical calculations for the evolution of the SWB of M_ini =35M* star. The low initial mass of the WR star in gamma2 Velorum implies thatthe luminosity of the nuclear line of 26Al, produced by gamma2 Velorum, isbelow the sensitivity of existing gamma-ray telescopes.

Modeling of the Vela complex including the Vela supernova remnant, the binary system gamma2 Velorum, and the Gum nebula