Feedback by massive stars and the emergence of superbubbles (Corrigendum)
II. X-ray properties
Max-Planck-Institut für extraterrestrische Physik,
2 Excellence Cluster Universe, Technische Universität München, Boltzmannstrasse 2, 85748 Garching, Germany
Key words: ISM: bubbles / ISM: structure / galaxies: ISM / hydrodynamics / instabilities / errata, addenda
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.
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