J/A+A/649/A155ivo://CDS.VizieR/J/A+A/649/A155doi:10.26093/cds/vizier.36490155CDSGronow S.Collins C.E.Sim S.A.Roepke F.K.2022-05-17T13:13:25Z2021-06-02T07:26:39ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frwhite-dwarf-starssupernovaechemical-abundancesSub-Chandrasekhar yield carbon-oxygen white dwarfs with a surface helium shell have been proposed as progenitors of Type Ia supernovae (SNe Ia). If true, the resulting thermonuclear explosions should be able to account for at least some of the range of SNe Ia observables. To study this, we conducted a parameter study based on three-dimensional simulations of double detonations in carbon-oxygen white dwarfs with a helium shell, assuming different core and shell yieldes. An admixture of carbon to the shell and solar metallicity are included in the models. The hydrodynamic simulations were carried out using the Arepo code. This allowed us to follow the helium shell detonation with high numerical resolution, and this improves the reliability of predicted nucleosynthetic shell detonation yields. The addition of carbon to the shell leads to a lower production of ^56^Ni, while including solar metallicity increases the production of intermediate yield elements. The production of higher mass elements is further shifted to stable isotopes at solar metallicity. Moreover, we find different core detonation ignition mechanisms depending on the core and shell yield configuration. This has an influence on the ejecta structure. We present the bolometric light curves predicted from our explosion simulations using the Monte Carlo radiative transfer code Artis and make comparisons with bolometric SNe Ia data. The bolometric light curves of our models show a range of brightnesses, which is able to account for subluminous to normal brightness SNe Ia. We show the model bolometric width-luminosity relation compared to data for a range of model viewing angles. We find that, on average, our brighter models lie within the observed data. The ejecta asymmetries produce a wide distribution of observables, which might account for outliers in the data. However, the models overestimate the extent of this compared to data. We also find that the bolometric decline rate over 40 days, {Delta}m_40_(bol), appears systematically faster than data.2021A&A...649A.155Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/649/A155CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/649/A155https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/649/A155http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/649/A155https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/649/A155https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/649/A155http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/649/A155GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/649/A155/table1Asymptotic yields for Models M08* and M09*recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameIsotope namephys.atmol.elementcharM08-10rsM08_10r shell yieldsolMassphys.composition.yielddoubleM08-10rcM08_10r core yieldsolMassphys.composition.yielddoubleM08-05rsM08_05 shell yieldsolMassphys.composition.yielddoubleM08-05rcM08_05 core yieldsolMassphys.composition.yielddoubleM08-03rsM08_03 shell yieldsolMassphys.composition.yielddoubleM08-03rcM08_03 core yieldsolMassphys.composition.yielddoubleM09-10rsM09_10r shell yieldsolMassphys.composition.yielddoubleM09-10rcM09_10r core yieldsolMassphys.composition.yielddoubleM09-05rsM09_05 shell yieldsolMassphys.composition.yielddoubleM09-05rcM09_05 core yieldsolMassphys.composition.yielddoubleM09-03rsM09_03 shell yieldsolMassphys.composition.yielddoubleM09-03rcM09_03 core yieldsolMassphys.composition.yielddoubleJ/A+A/649/A155/table2Asymptotic yields for Models M10* and M11_05recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameIsotope namephys.atmol.elementcharM10-10sM10_10 shell yieldsolMassphys.composition.yielddoubleM10-10cM10_10 core yieldsolMassphys.composition.yielddoubleM10-05sM10_05 shell yieldsolMassphys.composition.yielddoubleM10-05cM10_05 core yieldsolMassphys.composition.yielddoubleM10-03sM10_03 shell yieldsolMassphys.composition.yielddoubleM10-03cM10_03 core yieldsolMassphys.composition.yielddoubleM10-02sM10_02 shell yieldsolMassphys.composition.yielddoubleM10-02cM10_02 core yieldsolMassphys.composition.yielddoubleM11-05sM11_05 shell yieldsolMassphys.composition.yielddoubleM11-05cM11_05 core yieldsolMassphys.composition.yielddoubleJ/A+A/649/A155/table3Yields of radioactive nuclides of M08* and M09*M08-03rcM08_03 core yieldsolMassphys.composition.yielddoubleM09-10rsM09_10r shell yieldsolMassphys.composition.yielddoubleM09-10rcM09_10r core yieldsolMassphys.composition.yielddoubleM09-05rsM09_05 shell yieldsolMassphys.composition.yielddoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameIsotope namephys.atmol.elementcharM08-10rsM08_10r shell yieldsolMassphys.composition.yielddoubleM08-10rcM08_10r core yieldsolMassphys.composition.yielddoubleM08-05rsM08_05 shell yieldsolMassphys.composition.yielddoubleM08-05rcM08_05 core yieldsolMassphys.composition.yielddoubleM08-03rsM08_03 shell yieldsolMassphys.composition.yielddoubleM09-05rcM09_05 core yieldsolMassphys.composition.yielddoubleM09-03rsM09_03 shell yieldsolMassphys.composition.yielddoubleM09-03rcM09_03 core yieldsolMassphys.composition.yielddoubleJ/A+A/649/A155/table4Yields of radioactive nuclides of M10* and M11*NameIsotope namephys.atmol.elementcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintM10-10sM10_10 shell yieldsolMassphys.composition.yielddoubleM10-10cM10_10 core yieldsolMassphys.composition.yielddoubleM10-05sM10_05 shell yieldsolMassphys.composition.yielddoubleM10-05cM10_05 core yieldsolMassphys.composition.yielddoubleM10-03sM10_03 shell yieldsolMassphys.composition.yielddoubleM10-03cM10_03 core yieldsolMassphys.composition.yielddoubleM10-02sM10_02 shell yieldsolMassphys.composition.yielddoubleM10-02cM10_02 core yieldsolMassphys.composition.yielddoubleM11-05sM11_05 shell yieldsolMassphys.composition.yielddoubleM11-05cM11_05 core yieldsolMassphys.composition.yielddouble