  Deep-sea archives all over the world show an enhanced concentration of the
radionuclide $^{60}$Fe, isolated in layers dating from about 2.2 Myr ago. Since
this comparatively long-lived isotope is not naturally produced on Earth, such
an enhancement can only be attributed to extraterrestrial sources, particularly
one or several nearby supernovae in the recent past. It has been speculated
that these supernovae might have been involved in the formation of the Local
Superbubble, our Galactic habitat. Here, we summarize our efforts in giving a
quantitative evidence for this scenario. Besides analytical calculations, we
present results from high-resolution hydrodynamical simulations of the Local
Superbubble and its presumptive neighbor Loop I in different environments,
including a self-consistently evolved supernova-driven interstellar medium. For
the superbubble modeling, the time sequence and locations of the generating
core-collapse supernova explosions are taken into account, which are derived
from the mass spectrum of the perished members of certain, carefully
preselected stellar moving groups. The release and turbulent mixing of
$^{60}$Fe is followed via passive scalars, where the yields of the decaying
radioisotope were adjusted according to recent stellar evolution calculations.
The models are able to reproduce both the timing and the intensity of the
$^{60}$Fe excess observed with rather high precision. We close with a
discussion of recent developments and give future perspectives.
