Volume 561, January 2014
|Number of page(s)||8|
|Published online||27 January 2014|
Modelling of the radio emission from the Vela supernova remnant
1 Centre for Space Research, North-West University, Potchefstroom Campus, 2531 Potchefstroom, South Africa
2 Astronomical Observatory of Ivan Franko National University of Lviv, 79005 Lviv, Ukraine
3 Humboldt Universität zu Berlin, Institut für Physik, 12489 Berlin, Germany
4 Astronomical Observatory of Taras Shevchenko National University of Kyiv, 04053 Kyiv, Ukraine
Received: 30 August 2013
Accepted: 28 November 2013
Supernova remnants (SNRs) are widely considered to be sites of Galactic cosmic ray (CR) acceleration. Vela is one of the Galactic composite SNRs closest 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 estimates of various physical parameters such as distance and age. Therefore, it is a perfect object for a detailed study of physical processes in SNRs. The Vela SNR expands into the highly inhomogeneous cloudy interstellar medium (ISM) and its dynamics are 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 star γ2 Velorum causing one part of the remnant to expand 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 almost uniform distribution of relativistic particles inside the remnant. We calculate the synchrotron radio emission within the framework of the new hydrodynamical model that 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 radio morphology of the source.
Key words: ISM: supernova remnants / ISM: clouds / ISM: individual objects: Vela SNR
© ESO, 2014
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