2005/01/21 by Miguel A. de Avillez, Dieter Breitschwerdt, de Avillez, Miguel A. +2
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics (astro-ph) #Atmospheric Ozone and Climate #FOS: Physical sciences #Ionosphere and magnetosphere dynamics #Solar and Space Plasma Dynamics #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0501466
3 Pages, 3 figures (including 1 jpg image and 3 plots); poster paper to appear in "Astrophysics in the Far Ultraviolet: Five Years of Discovery with FUSE", 2005, ASP Conference Series, eds. G. Sonneborn, H. W. Moos, and B-G Andersson
openalex publication_date 2005/01/21 · arxiv created 2005/01/28 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The Local Bubble (LB) is an X-ray emitting region extending 100 pc in radius in the Galactic plane and 300 pc perpendicular to it, and it is embedded in a somewhat larger H\sc i deficient cavity. Its origin and spectral properties in UV, EUV and X-rays are still poorly understood. We have performed 3D high resolution (down to 1.25 pc) hydrodynamic superbubble simulations of the LB and Loop I superbubble in a realistic inhomogeneous background ISM, disturbed by supernova (SN) explosions at the Galactic rate. We can reproduce (i) the size of the bubbles (in contrast to similarity solutions), (ii) the interaction shell with Loop I, discovered with ROSAT, (iii) predict the merging of the two bubbles in about 3 Myr, when the interaction shell starts to fragment, and, (iv) the generation of blobs like the Local Cloud as a consequence of a dynamical instability. The \ionO6 column densities are monitored and found to be in excellent agreement with Copernicus and FUSE absorption line data, showing LB column densities <1.7 × 1013 \rm cm-2, in contrast to other existing models.