I. Sushch

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

We study the geometry and dynamics of the Vela complex including the Vela supernova remnant (SNR), the binary system γ 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 (∼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 γ 2 Velorum system. We show that the size and kinematics of γ 2 Velorum SWB agree with predictions of numerical calculations for the evolution of the SWB of M ini = 35 M ⊙ star. The low initial mass of the WR star in γ 2 Velorum implies that the luminosity of the nuclear line of 26 Al, produced by γ 2 Velorum, is below the sensitivity of existing gamma-ray telescopes.

Modelling of the radio emission from the Vela supernova remnant

Supernova remnants (SNRs) are widely considered to be sites of Galactic cosmic ray (CR) acceleration. Vela is one of the nearest Galactic composite SNRs to Earth accompanied by the Vela pulsar and its pulsar wind nebula (PWN) Vela X. The Vela SNR is one of the most studied remnants and it benefits from precise estima tes of various physical parameters such as distance and age. Therefore, it is a perfect object for a detailed study of physical proces ses in SNRs. The Vela SNR expands into the highly inhomogeneous cloudy interstellar medium (ISM) and its dynamics is determined by the heating and evaporation of ISM clouds. It features an asymmetrical X-ray morphology which is explained by the expansion into two media with different densities. This could occur if the progenitor of the Vela SNR exploded close to the edge of the stellar wind bubble of the nearby Wolf-Rayet starγ 2 Velorum and hence one part of the remnant expands into the bubble. The interaction of the ejecta and the main shock of the remnant with ISM clouds causes formation of secondary shocks at which additional particle acceleration takes place. This may lead to the close to uniform distribution of relativistic particles inside the remnant. We calculate the synchrotron radio emission within the framework of the new hydrodynamical model which assumes the supernova explosion at the edge of the stellar wind bubble. The simulated radio emission agrees well with both the total radio flux from the remnant and the complicated radi o morphology of the source.

Modeling of the spatially resolved nonthermal emission from the Vela Jr. supernova remnant

Vela Jr. (RX J0852.0

Magnetic field damping in the Vela Jr. SNR

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