Modeling of the Vela complex including the Vela supernova remnant, the binary system γ2?Velorum, and the Gum nebula

摘要

We study the geometry and dynamics of the Vela complex including the Vela supernova remnant (SNR), the binary system γ2?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?×?1050???erg 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 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 γ2?Velorum system. We show that the size and kinematics of γ2?Velorum SWB agree with predictions of numerical calculations for the evolution of the SWB of Mini?=?35???M⊙ star. The low initial mass of the WR star in γ2?Velorum implies that the luminosity of the nuclear line of 26Al, produced by γ2?Velorum, is below the sensitivity of existing gamma-ray telescopes.