Speaker
Dr
Martin Krause
(Max-Planck-Institut für extraterrestrische Physik)
Description
With sizes from below 100 pc to just above 1kpc, superbubbles are structuring the ISM on scales in between the larger scale spiral arms and the smaller, turbulent molecular cloud scales. With 3D hydrodynamics simulation of the entire stellar evolution of and the interaction between an ensemble of massive stars we are able to explain at least some of the apparent width of observed bubbles via the Vishniac instability and the X-ray properties via an interplay between supernova heating and cooling via Rayleigh-Taylor-induced mixing. We investigate the effective energy input into the ISM which increases with stronger clustering. Applied to galaxy scale, we show that the expansion of superbubbles into gaseous halos of Lyman-break galaxies is able to produce the observed absorption systems at the correct column densities and velocities. In the Milky Way, we have recently measured the kinematics of hot bubble content over the entire galactic plane via Gamma-ray line tracers (26Al). Our results are consistent with young superbubbles located in the inner spiral arms of the Milky Way and having a global blow-out preference into the direction of Galactic rotation, away from the arms into the inter-arm region.
Author
Dr
Martin Krause
(Max-Planck-Institut für extraterrestrische Physik)