Metallicity-dependent nucleosynthetic yields of Type Ia supernovae originating from double detonations of sub-M\(_{\text{Ch}}\) white dwarfs

• Published in: arXiv.org
• Main Authors: Gronow, Sabrina, Cote, Benoit, Lach, Florian, Seitenzahl, Ivo R, Collins, Christine E, Sim, Stuart A, Roepke, Friedrich K
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 01.09.2021
• Subjects: Astronomical models; Chemical evolution; Detonation; Galactic evolution; Iron; Isotopes; Manganese; Massive stars; Metallicity; Nickel; Physics - High Energy Astrophysical Phenomena; Solar neighborhood; Stellar evolution; Supernovae; White dwarf stars
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2103.14050

Double detonations in sub-Chandrasekhar mass carbon-oxygen white dwarfs with helium shell are a potential explosion mechanism for a Type Ia supernova (SNe Ia). It comprises a shell detonation and subsequent core detonation. The focus of our study is on the effect of the progenitor metallicity on the nucleosynthetic yields. For this, we compute and analyse a set of eleven different models with varying core and shell masses at four different metallicities each. This results in a total of 44 models at metallicities between 0.01\(Z_\odot\) and 3\(Z_\odot\). Our models show a strong impact of the metallicity in the high density regime. The presence of \(^{22}\)Ne causes a neutron-excess which shifts the production from \(^{56}\)Ni to stable isotopes such as \(^{54}\)Fe and \(^{58}\)Ni in the \(\alpha\)-rich freeze-out regime. The isotopes of the metallicity implementation further serve as seed nuclei for additional reactions in the shell detonation. Most significantly, the production of \(^{55}\)Mn increases with metallicity confirming the results of previous work. A comparison of elemental ratios relative to iron shows a relatively good match to solar values for some models. Super-solar values are reached for Mn at 3\(Z_\odot\) and solar values in some models at \(Z_\odot\). This indicates that the required contribution of SNe Ia originating from Chandrasekhar mass WDs can be lower than estimated in orevious work to reach solar values of [Mn/Fe] at [Fe/H]\(=0\). Our galactic chemical evolution models suggest that SNe Ia from sub-Chandrasekhar mass white dwarfs, along with core-collapse supernovae, could account for more than 80% of the solar Mn abundance. Using metallicity-dependent SN Ia yields helps to reproduce the upward trend of [Mn/Fe] as a function of metallicity for the solar neighborhood. These chemical evolution predictions, however, depend on the massive star yields adopted in the calculations.