The presence of live 60Fe nuclei (lifetime of 3.8~Myr) in cosmic rays
detected by the ACE/CRIS instrument suggests a nearby nucleosynthesis source.
60Fe is primarily produced in core-collapse supernovae, and we aim to
clarify whether the detected 60Fe nuclei can be associated with a
particular local supernova. We consider 25 OB associations and sub-groups
located within 1 kpc of the solar system based on recent Gaia census. A model
is developed that combines stellar population synthesis within these OB
associations, cosmic-ray acceleration within associated superbubbles, and
cosmic-ray transport to the solar system. The most critical model parameter
impacting 60Fe cosmic-ray production is the explodability criterion, which
determines if a massive star ends its life as a supernova. Our study points to
the Sco-Cen OB association as the most probable origin of the observed
60Fe nuclei, particularly suggesting they were accelerated in the Sco-Cen
superbubble by a young supernova aged ≤500 kyr with a progenitor mass of
approximately 13−20M⊙. A less likely source is the supernova at the
origin of the Geminga pulsar 342 kyr ago, if the progenitor originated in the
Orion OB1 association. The contribution of local OB associations to the
cosmic-ray density of stable 56Fe is estimated to be around 20\%, with
some sensitivity to cosmic ray acceleration efficiency and diffusion
coefficient. These findings shed light on the origins of cosmic-ray nuclei,
connecting them to nucleosynthesis events within our local cosmic neighborhood