SISSI: Supernovae in a stratified, shearing interstellar medium. II. Star formation near the Sun is quenched by expansion of the Local Bubble

Abstract: The age of the Local Bubble (LB) can be used to constrain the timescales, on which the interstellar medium in the solar neighborhood is evolving. Previous estimates have put the age of the LB at $\gtrsim 14\,\text{Myr}$, and suggested that its expansion was powered by $\sim 15-20$ SNe, yet in a companion paper we have seen hints that this age might be too high. Following up on these hints, we aim to place new constraints on the age of the LB. We reconstruct the geometry and momentum of the LB using publicly available 3D dust maps to compare its geometry to that of the high-quality sample of simulated supernova remnants in the SISSI project. We find that, in contrast to previous estimates, $\gtrsim 20$ SNe over $\sim 4\,\text{Myr}$ are required to explain both the momentum and the size of the LB. The julia source-code for our analysis is made available at https://doi.org/10.5281/zenodo.17054923. Previous estimates of the age of the LB have seemingly overestimated its age and underestimated the number of SNe powering its expansion. Our results are in tension with the assumption that the LB is powered solely by SNe associated with the nearby Scorpius-Centraurus OB association, which appears to have stopped forming stars at about the same time as the LB began to expand. In light of this new evidence, our results cast serious doubts on the claim that star formation in the solar neighborhood was driven by the expansion of the LB, and might have instead quenched it.