EDP Sciences
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This article is an erratum for: [this article]

Volume 570, October 2014
Article Number C3
Number of page(s) 1
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201423871e
Published online 30 October 2014

1. Corrected extent of the mixing region

In Fig. 2 of Krause et al. (2014), we showed the density in a simulated superbubble as a function of radius averaged over the solid angle as seen from the geometrical centre of the main bubble. This plot was misleading as it implied an extent of the mixing region – responsible for much of the X-ray emission discussed in this paper – twice as large as it actually is. The reason is that due to the averaging over the solid angle, side cavities from other massive stars influence the plot. The true extent of the mixing region just before the first supernova explosion is 10 pc, and it extends from X = 40 pc to X = 50 pc as shown in Fig. 1. The contact surface is thus still resolved. The results and conclusions of the article are not affected by this, because the synthetic emission is derived from the numerical grid directly.

thumbnail Fig. 1

This figure replaces Fig. 2 of the original publication. It shows the run of the density on a linear slice along the positive X-axis for run 3S1-hr at time 4.598 Myr, i.e. 2139 yr before the central most massive star (at X = 0) explodes. Each “+”-Symbol shows the value of the density in one grid cell. The mixing region is resolved with about 20 cells, and extends from 40 to 50 pc.

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© ESO, 2014

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