Evolution of Dust in Primordial Supernova Remnants: Can Dust Grains Formed in the Ejecta Survive and be Injected into the Early Interstellar Medium?

TL;DR

This study examines how dust formed in Population III supernovae evolves and survives through reverse shocks, influencing early interstellar medium enrichment and subsequent star formation.

Contribution

It provides detailed modeling of dust processing in primordial supernova remnants, highlighting the dependence on progenitor envelope, grain size, and ambient medium conditions.

Findings

Small grains (<0.05 micron) are destroyed by sputtering.

Large grains (>0.2 micron) survive and are ejected into the ISM.

Dust destruction varies from 20% to 100% depending on explosion energy and environment.

Abstract

We investigate the evolution of dust that formed at Population III supernova (SN) explosions and its processing through the collisions with the reverse shocks resulting from the interaction of the SN ejecta with the ambient medium. In particular, we investigate the transport of the shocked dust within the SN remnant (SNR), and its effect on the chemical composition, the size distribution, and the total mass of dust surviving in SNR. We find that the evolution of the reverse shock, and hence its effect on the processing of the dust depends on the thickness of the envelope retained by the progenitor star. Furthermore, the transport and survival of the dust grains depend on their initial radius, a_{ini}, and composition: For Type II SNRs expanding into the interstellar medium (ISM) with a density of n_{H,0}=1 cm^{-3}, small grains with a_{ini} < ~ 0.05 micron are completely destroyed by sputtering in the postshock flow, while grains with a_{ini}= 0.05--0.2 micron are trapped into the dense shell behind the forward shock. Very large grains of a_{ini} > ~ 0.2 micron are ejected into the ISM without decreasing their sizes significantly. We find that the total mass fraction of dust that is destroyed by the reverse shock ranges from 0.2 to 1.0, depending on the energy of the explosion and the density of the ambient ISM. The results of our calculations have significant impact on the abundance pattern of subsequent generation of stars that form in the dense shell of primordial SNRs.