The bright, dusty aftermath of giant eruptions & H-rich supernovae. Late interaction of supernova shocks & dusty circumstellar shells

Abstract

The late-stage evolution of massive stars is marked by intense instability as they approach core-collapse. During these phases, giant stellar eruptions lead to exceptionally high mass-loss rates, forming significant amounts of dust. However, the survival of these dust grains is challenged by the powerful shock waves generated when the progenitor explodes as a supernova (SN). We explore the impact of hydrogen-rich SN explosions from 45, 50, and 60 M$_\odot$ progenitors on dust formed after these eruptions, focusing on interactions with circumstellar shells occurring from a few years to centuries after the event. Using 3D hydrodynamical simulations, we track the evolution of dust particles in a scenario that includes the progenitor's stellar wind, a giant eruption, and the subsequent SN explosion, following the mass budgets predicted by stellar evolution models. For a standard SN ejecta mass of 10 M$_\odot$ and kinetic energy of $10^{51}$ erg, only 25% of the dust mass survives 250 years post-explosion in a spherical circumstellar medium (CSM), while merely 2% remains a century after the explosion in a bipolar CSM. If the SN follows the eruption within a dozen years, 75% of the dust survives for a standard explosion, dropping to 20% for more massive ejecta (15-20 M$_\odot$) with kinetic energy of $5 \times 10^{51}$ erg. The geometry of the CSM and the early transition of the SN remnant into a radiative phase significantly influence dust survival. As the shock wave weakens and efficiently converts kinetic energy into thermal radiation (up to half of the injected kinetic energy) the likelihood of dust survival increases, affecting not only pre-existing dust in the CSM but also SN-condensed dust and ambient interstellar dust. Contrary to expectations, a larger fraction of the dust mass can survive if the SN occurs only a few years after the eruption.