Abstract
We explore the idea that the Type Ia supernovae (SNe Ia) rate consists of two components: a prompt piece that is proportional to the star formation rate (SFR) and an extended piece that is proportional to the total stellar mass. We fit the parameters of this model to the local observations of Mannucci and collaborators and then study its impact on three important problems. On cosmic scales, the model reproduces the observed SNe Ia rate density below z=1, and predicts that it will track the measured SFR density at higher redshift, reaching a value of 1-3.5 X 10^-4 per yr per Mpc^3 at z=2. In galaxy clusters, a large prompt contribution helps explain the iron content of the intracluster medium. Within the Galaxy, the model reproduces the observed stellar [O/Fe] abundance ratios if we allow a short (approximately 0.7 Gyr) delay in the prompt component. Ongoing medium-redshift SN surveys will yield more accurate parameters for our model
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
