Evolution of Rotating 25 M$_{\odot}$ Population III star: Physical Properties and Resulting Supernovae

TL;DR

This study models a rotating 25 solar mass Population III star's evolution up to core collapse, revealing faint supernovae with diverse types and challenging detectability at high redshifts.

Contribution

First 1-D simulations of rotating Population III stars up to core collapse, linking stellar evolution to supernova diversity and brightness.

Findings

Pop III supernovae are significantly fainter than solar metallicity counterparts.

Rotation induces sporadic mass loss and affects supernova type.

Faintness of Pop III supernovae limits high-redshift detection.

Abstract

In this Letter, we report the outcomes of 1-D modelling of a rotating 25 M$_{\odot}$ zero-age main-sequence Population III star up to the stage of the onset of core collapse. Rapidly rotating models display violent and sporadic mass losses after the Main-Sequence stage. In comparison to the solar metallicity model, Pop III models show very small pre-supernova radii. Further, with models at the stage of the onset of core collapse, we simulate the hydrodynamic simulations of resulting supernovae. Depending upon the mass losses due to corresponding rotations and stellar winds, the resulting supernovae span a class from weak Type II to Type Ib/c. We find that the absolute magnitudes of the core-collapse supernovae resulting from Pop III stars are much fainter than that resulting from a solar metallicity star. From our simulation results, we also conclude that within the considered limits of explosion energies and Nickel masses, these transient events are very faint, making it difficult for them to be detected at high redshifts.