Modeling of the Vela complex including the Vela supernova remnant, the binary system gamma(2) Velorum, and the Gum nebula

We study the geometry and dynamics of the Vela complex including the Vela supernova remnant (SNR), the binary system gamma(2) Velorum and the Gum nebula. We show that the Vela SNR belongs to a subclass of non-Sedov adiabatic remnants in a cloudy interstellar medium (ISM), the dynamics of which is determined by the heating and evaporation of ISM clouds. We explain observable characteristics of the Vela SNR with a SN explosion with energy 1.4 x 10(50) erg near the step-like boundary of the ISM with low intercloud densities (similar to 10(-3) cm(-3)) and with a volume-averaged density of clouds evaporated by shock in the north-east (NE) part about four times higher than the one in the south-west (SW) part. The observed asymmetry between the NE and SW parts of the Vela 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 gamma(2) Velorum system. We show that the size and kinematics of gamma(2) Velorum SWB agree with predictions of numerical calculations for the evolution of the SWB of M-ini = 35 M-circle dot star. The low initial mass of the WR star in gamma(2) Velorum implies that the luminosity of the nuclear line of Al-26, produced by gamma(2) Velorum, is below the sensitivity of existing gamma-ray telescopes.