PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. III. Nucleosynthesis Yields

Abstract

In a previously presented proof-of-principle study, we established a parametrized spherically symmetric explosion method (PUSH) that can reproduce many features of core-collapse supernovae for a wide range of pre-explosion models. The method is based on the neutrino-driven mechanism and follows collapse, bounce and explosion. There are two crucial aspects of our model for nucleosynthesis predictions. First, the mass cut and explosion energy emerge simultaneously from the simulation (determining, for each stellar model, the amount of Fe-group ejecta). Second, the interactions between neutrinos and matter are included consistently (setting the electron fraction of the innermost ejecta). In the present paper, we use the successful explosion models from Ebinger et al. (2018) which include two sets of pre-explosion models at solar metallicity, with combined masses between 10.8 and 120 M . We perform systematic nucleosynthesis studies and predict detailed isotopic yields. The resulting 56 Ni ejecta are in overall agreement with observationally derived values from normal core-collapse supernovae. The Fe-group yields are also in agreement with derived abundances for metal-poor star HD 84937. We also present a comparison of our results with observational trends in alpha element to iron ratios.

PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. IV. Explodability, Remnant Properties, and Nucleosynthesis Yields of Low-metallicity Stars*

“…Perego et al (2015), together with the standard calibration obtained in Ebinger et al (2019). The work presented here complements the results obtained for pre-SN models at solar metallicity presented in Ebinger et al (2019) and Curtis et al (2019).…”

“…4. We find the same trends with compactness for iron group isotopes and elements for the low/zero metallicity pre-SN series of this work as for the pre-SN series at solar metallicity discussed in Curtis et al (2019). For symmetric isotopes (e.g.…”

“…We predicted explosion properties and remnant properties in Paper II. In Curtis et al (2019) -hereafter Paper III -we made use of the simulations from Paper II to predict detailed nucleosynthesis yields. In this work, we apply the PUSH method, using the calibration obtained in Paper II, to predict explosion outcomes and nucleosynthesis yields for pre-explosion models of massive stars at low and zero initial metallicity.…”

Nucleosynthesis Constraints on the Energy Growth Timescale of a Core-collapse Supernova Explosion

“…Recently, thus, there are also a number of 'artificial-explosion' simulations, that is, the readily calculable supernova simulations in which the neutrino transfer is solved but with the neutrino luminosity calibrated to match to some well-studied SNe (e.g., Perego et al 2015;Sukhbold et al 2016). These studies, especially spherically symmetric models, can be calculated systematically for various progenitor models, from the onset of the explosion up to several hundred seconds after core bounce, and have succeeded in explaining observational properties of individual SN events (e.g., SN 1987A; Perego et al 2015), as well as the Galactic chemical evolution highlighted by the abundance patterns of extremely metal-poor (EMP) stars (e.g., Curtis et al 2019). Therefore, these simulations support that the neutrino-driven model is promising as a standard explosion mechanism of CCSNe.…”

Could Failed Supernovae Explain the High r-process Abundances in Some Low Metallicity Stars?

“…Massive stars (ZAMS ≥ 8M ⊙ ) go through all burning stages until they reach the end of their life time. We then use the results of the explosion energy predictions of the CCSN simulation suite PUSH [10][11][12][13] in order to determine whether a massive star dies in a CCSN explosion (under the ejection of metals, leaving behind a NS), or the explosion fails and the star collapses to a black hole (BH) instead.…”