Abstract:
In this letter, we report the outcomes of 1D modelling of a rotating 25 M zero-age main sequence Population III (Pop 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.
