Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.4903d&link_type=abstract
American Astronomical Society Meeting 208, #49.03; Bulletin of the American Astronomical Society, Vol. 38, p.124
Astronomy and Astrophysics
Astronomy
Scientific paper
The Local and Loop I superbubbles are the closest and best investigated SN generated bubbles and serve as test laboratories for observations and theories of the ISM. The morphology and dynamical evolution of bubbles depend on the density and pressure distributions of the ambient medium into which they are expanding. Hence, a realistic modelling of the galactic environment is crucial for a detailed comparison with observations. We have performed 3D high resolution (down to 1.25 pc on a kpc-scale grid) MHD and HD simulations of the Local Bubble (LB), jointly with the dynamical evolution of the neighbouring Loop I superbubble in a realistic inhomogeneous background ISM, disturbed by SN explosions at the Galactic rate for 200 Myr. The LB is the result of about 19 SNe occurring in moving groups, passing through the present day local HI cavity. With our detailed simulations we can reproduce (i) the column density of Ovi in absorption within the LB in agreement with Copernicus and FUSE results, giving N(OVI)<2 x 10^{13}$ and $<7x10^{12}$ cm$^{-2}$, respectively, (ii) the observed size of the Local and Loop I superbubbles, (iii) the interaction shell with Loop I, discovered with ROSAT, (iv) constrain the age of the LB to vary between 14 and 15.1 Myr, (v) predict the merging of the two bubbles in about 3 Myr, when the interaction shell starts to fragment, and, (vi) the generation of blobs like the Local Cloud as a consequence of a dynamical instability. We find that evolving superbubbles strongly deviate from idealised self-similar solutions due to ambient pressure and density gradients, as well as due to turbulent mixing and mass loading. Hence, at later times the hot interior can break through the surrounding shell, which may also help to explain the puzzling energy ``deficit'' in observed bubbles in the LMC.
Breitschwerdt Dieter
de Avillez Miguel A.
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