Population III Supernovae

Class providing models of supernovae from Population III (metal-free) stars—the first generation of stars formed from primordial gas at high redshift. Very massive Population III stars (\(M \gtrsim 100 \mathrm{M}_\odot\)) may explode as pair-instability supernovae with enormous energy output (\(\sim 10^{53}\) erg), while lower-mass Population III stars undergo core-collapse. The cumulative energy input from Population III supernovae contributes to the reionization and early metal enrichment of the IGM.

Default implementation: supernovaePopulationIIIHegerWoosley2002

Methods

energyCumulative → double precision

Return the cumulative energy input from Population III supernovae from stars of given initialMass, age and metallicity.

• double precision, intent(in ) :: initialMass, age, metallicity

supernovaePopulationIIIHegerWoosley2002

A Population III supernovae class that computes the energies of pair instability supernovae from the results of Heger and Woosley (2002).

(Default implementation)

supernovaePopulationIIIZero

A Population III supernovae class that has zero population III supernovae.