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

TL;DR

This study uses advanced 3D hydrodynamic simulations and stellar data to link radioisotope influxes on Earth to past supernovae, shedding light on the formation of the Local Bubble and the solar system's history.

Contribution

It introduces a new Monte Carlo approach for supernova progenitor trajectories and models radioisotope transport, aligning simulations with observed isotope data and solar system history.

Findings

Simulations match observed 60Fe, 26Al, 53Mn, and 244Pu isotope peaks.

Stellar winds influence isotope distribution and Local Bubble dynamics.

The solar system entered the Local Bubble about 4.6 million years ago.

Abstract

Measurements of long-lived radioisotopes provide a means, completely independent of other observational channels, to draw conclusions about near-Earth supernovae (SNe) and thus the origin of the Local Bubble (LB). First and foremost in this context is 60Fe, which has already been detected across the 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 the Sco-Cen OB association. The timing of these explosions was obtained by us through interpolation of rotating stellar evolution tracks via the initial masses of the already exploded massive stars. We further developed a new Monte Carlo-type approach for deriving the trajectories of the SN progenitors. We then performed 3D hydrodynamic simulations based on these initial conditions to explore the evolution of the LB in an inhomogeneous local interstellar medium and the transport of radioisotopes to Earth. The simulations include the stellar winds from the SN progenitors and additional radioisotopes (26Al, 53Mn, and 244Pu) besides 60Fe. We find that (i) our simulations are consistent with measurements of 60Fe, in particular, a peak 2-3 Myr before present, as well as 26Al, 53Mn, and 244Pu data, (ii) stellar winds contribute to the distribution of 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 of 60Fe can be naturally explained by turbulent radioisotopic transport. Our simulations not only support the recent hypothesis that the LB triggered star formation in the solar vicinity through its expansion, but also suggest that the second, separate 60Fe peak measured at 6-9 Myr ago was generated by the passage of the SS through a neighboring superbubble (SB), possibly the Orion-Eridanus SB, prior to its current residence in the LB.