Type Ia supernovae and stellar winds in relativistic bubbles driven by active galactic nuclei

Details Type Ia supernovae and stellar winds in relativistic bubbles driven by active galactic nuclei Type Ia supernovae and stellar winds in relativistic bubbles driven by active galactic nuclei

Jun 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011mnras.414..879c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 414, Issue 2, pp. 879-887.

Astronomy and Astrophysics

Astronomy

Galaxies: Clusters: Intracluster Medium

Scientific paper

We analyse the behaviour of the stellar winds of evolved stars and the outcome of Type Ia supernova (SN) explosions in a relativistic bubble driven by active galactic nuclei (AGNs). We find that the expansion of wind shells is efficiently decelerated by the relativistic pressure; however, their bulk motion is preserved, so they cross the bubble together with the parent star. The wind material occupies a small fraction of the bubble volume and does not substantially affect the expansion of SN remnants. The estimated maximal radius of a SN remnant in the bubble is 30-40 pc, if the envelope keeps its integrity and remains spherical. A fragmentation of the SN shell as a result of Rayleigh-Taylor instability can alleviate the propagation of the SN material so the ejecta fragments are able to cross the relativistic bubble. Outside the bubble, wind shells and SN fragments are decelerated in the intracluster medium at close range off the bubble boundary. The deposited SNe Ia material can enrich the intracluster gas with metals in a thin layer at the boundary of the relativistic bubble. This process may lead to a rim of enhanced line emission. In contrast, when the fragmentation of the SN remnant is moderate or absent, the SNe Ia matter is advected by the relativistic plasma and may leave the central region of the bright cluster galaxy together with buoyantly moving bubbles.

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