2011A&A...525A.154S

We study the geometry and dynamics of the Vela complex including the Vela supernova remnant (SNR), the binary system v_LSR 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 1.4x10⁵⁰erg near the step-like boundary of the ISM with low intercloud densities (∼10^–3cm^–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 v_LSR system. We show that the size and kinematics of v_LSR SWB agree with predictions of numerical calculations for the evolution of the SWB of M_ini=35M_☉ star. The low initial mass of the WR star in v_LSR implies that the luminosity of the nuclear line of ²⁶Al, produced by v_LSR, is below the sensitivity of existing gamma-ray telescopes.