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The discovery of radionuclides like 60Fe with half-lives of million years indeep-sea crusts and sediments offers the unique possibility to date and locatenearby supernovae. We want to quantitatively establish that the 60Feenhancement is the result of several supernovae which are also responsible forthe formation of the Local Bubble, our Galactic habitat. We performedthree-dimensional hydrodynamic adaptive mesh refinement simulations (withresolutions down to subparsec scale) of the Local Bubble and the neighbouringLoop I superbubble in different homogeneous, self-gravitating environments. Forsetting up the Local and Loop I superbubble, we took into account the timesequence and locations of the generating core-collapse supernova explosions,which were derived from the mass spectrum of the perished members of certainstellar moving groups. The release of 60Fe and its subsequent turbulent mixingprocess inside the superbubble cavities was followed via passive scalars, wherethe yields of the decaying radioisotope were adjusted according to recentstellar evolution calculations. The models are able to reproduce both thetiming and the intensity of the 60Fe excess observed with rather highprecision, provided that the external density does not exceed 0.3 cm-3 onaverage. Thus the two best-fit models presented here were obtained withbackground media mimicking the classical warm ionised and warm neutral medium.We also found that 60Fe (which is condensed onto dust grains) can be deliveredto Earth via two physical mechanisms: either through individual fast-pacedsupernova blast waves, which cross the Earth's orbit sometimes even twice as aresult of reflection from the Local Bubble's outer shell, or, alternatively,through the supershell of the Local Bubble itself, injecting the 60Fe contentof all previous supernovae at once, but over a longer time range.

astronomy and astrophysics

Numerical studies on the link between radioisotopic signatures on Earth  and the formation of the Local Bubble. I. 60Fe transport to the solar system  by turbulent mixing of ejecta from nearby supernovae into a locally  homogeneous ISM