The iron yield of core-collapse supernovae

by Dr. Ósmar Rodríguez

TAU

at Astrophysics and Cosmology Seminar

Wed, 27 Apr 2022, 11:10
Sacta-Rashi Building for Physics (54), room 207

Abstract

Core-collapse supernovae (CC SNe) are the result of the collapse of massive stars. They are spectroscopically separated into two classes: hydrogen-rich (Type II) and stripped-envelope (SE) SNe. CC SNe synthesize the bulk of all the alpha-elements in the Universe, while their contribution to the cosmic iron budget is comparable to that of thermonuclear SNe. The empirical estimate of the SN iron yield is a critical ingredient for studies of cosmic and Galactic chemical enrichment. In addition, estimating the nickel mass of SNe II and SE SNe is important for testing the various progenitor scenarios and explosion mechanisms that have been proposed for these SN types. I will present the nickel masses of ~100 SNe II and ~200 SE SNe, computed from the luminosity in their radioactive tails and/or in their maximum light, and an updated value for the mean iron yield of core-collapse SNe. The analysis, based on data from the literature and from the Zwicky Transient Facility Bright Transient Survey, includes improved methods for the determination of explosion epochs, host galaxy reddenings, and bolometric corrections, along with alternative techniques for measuring nickel masses.

Created on 24-04-2022 by Zitrin, Adi (zitrin)
Updaded on 24-04-2022 by Zitrin, Adi (zitrin)