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Measurements of long-lived radioisotopes provide a means, completelyindependent of other observational channels, to draw conclusions aboutnear-Earth supernovae (SNe) and thus the origin of the Local Bubble (LB). Firstand foremost in this context is 60Fe, which has already been detected acrossthe Earth and on the Moon. Using Gaia EDR3, we identified 14 SN explosions,with 13 occurring in UCL/LCC, and one in V1062 Sco, all being subgroups of theSco-Cen OB association. The timing of these explosions was obtained by usthrough interpolation of rotating stellar evolution tracks via the initialmasses of the already exploded massive stars. We further developed a new MonteCarlo-type approach for deriving the trajectories of the SN progenitors. Wethen performed 3D hydrodynamic simulations based on these initial conditions toexplore the evolution of the LB in an inhomogeneous local interstellar mediumand the transport of radioisotopes to Earth. The simulations include thestellar winds from the SN progenitors and additional radioisotopes (26Al, 53Mn,and 244Pu) besides 60Fe. We find that (i) our simulations are consistent withmeasurements of 60Fe, in particular, a peak 2-3 Myr before present, as well as26Al, 53Mn, and 244Pu data, (ii) stellar winds contribute to the distributionof radioisotopes and also to the dynamics of the LB, (iii) the solar system(SS) entered the LB about 4.6 Myr ago, and (iv) the measured recent influx of60Fe can be naturally explained by turbulent radioisotopic transport. Oursimulations not only support the recent hypothesis that the LB triggered starformation in the solar vicinity through its expansion, but also suggest thatthe second, separate 60Fe peak measured at 6-9 Myr ago was generated by thepassage of the SS through a neighboring superbubble (SB), possibly theOrion-Eridanus SB, prior to its current residence in the LB.

astronomy and astrophysics

Numerical studies on the link between radioisotopic signatures on Earth  and the formation of the Local Bubble. II. Advanced modeling of interstellar  26Al, 53Mn, 60Fe, and 244Pu influxes as traces of past supernovae in the  solar neighborhood