New Insights into the Rate of Pair-Instability Supernovae and Their Cosmic Implications
Recent research has provided new insights into the cosmic rate of Pair-Instability Supernovae (PISNe), which are significant for understanding various astrophysical phenomena, including the formation of massive stars and the chemical evolution of galaxies. The study, titled "The cosmic rate of Pair-Instability Supernovae," was conducted by Francesco Gabrielli and a team of researchers, and it presents a detailed analysis of the PISN rate as a function of redshift.
The authors utilized updated stellar evolution models from the PARSEC and FRANEC codes, combined with a semi-empirical determination of star formation rates and metallicity evolution in star-forming galaxies. Their findings indicate that the PISN rate is highly sensitive to model assumptions, particularly the criteria for identifying stars that are unstable to pair production and the upper limits of the stellar initial mass function.
A notable outcome of the study is the identification of a significant range in the PISN rate, which can vary by approximately seven orders of magnitude. This variability is primarily influenced by the maximum metallicity at which stars can explode as PISNe and the distribution of metallicities across galaxies. The research challenges the prevailing assumption that only very low-metallicity stars, known as Population III stars, are the primary progenitors of PISNe. Instead, the study suggests that stars with metallicities between approximately 10-3 and 10-2 play a crucial role in contributing to the PISN rate.
The implications of these findings are significant for future observations and models of stellar and galaxy evolution. The researchers emphasize that understanding the PISN rate can help constrain models based on potential future observations of these supernovae. This research not only enhances our comprehension of stellar evolution but also informs the broader context of cosmic chemical enrichment and black hole formation.
For further details, the paper can be accessed at arXiv:2408.16823.