# A successful 3D core-collapse supernova explosion model

## Author(s): Vartanyan, David; Burrows, Adam S.; Radice, David; Skinner, M Aaron; Dolence, Joshua

To refer to this page use: http://arks.princeton.edu/ark:/88435/pr1w688
DC FieldValueLanguage
dc.contributor.authorVartanyan, David-
dc.contributor.authorSkinner, M Aaron-
dc.contributor.authorDolence, Joshua-
dc.date.accessioned2019-04-10T19:30:49Z-
dc.date.available2019-04-10T19:30:49Z-
dc.date.issued2019-01en_US
dc.identifier.citationVartanyan, David, Burrows, Adam, Radice, David, Skinner, M Aaron, Dolence, Joshua. (2019). A successful 3D core-collapse supernova explosion model. \mnras, 482 (351 - 369. doi:10.1093/mnras/sty2585en_US
dc.identifier.urihttp://arks.princeton.edu/ark:/88435/pr1w688-
dc.description.abstractIn this paper, we present the results of our three-dimensional, multigroup, multineutrino- species radiation/hydrodynamic simulation using the state-of-the-art code FORNAX of the terminal dynamics of the core of a non-rotating 16 M stellar progenitor. The calculation incorporates redistribution by inelastic scattering, a correction for the effect of many-body in- teractions on the neutrino–nucleon scattering rates, approximate general relativity (including the effects of gravitational redshifts), velocity-dependent frequency advection, and an imple- mentation of initial perturbations in the progenitor core. The model explodes within ∼ 100 ms of bounce (near when the silicon–oxygen interface is accreted through the temporarily stalled shock) and by the end of the simulation (here, ∼ 677 ms after bounce) is accumulating explo- sion energy at a rate of ∼ 2.5 × 10 50 erg s − 1 . The supernova explodes with an asymmetrical multiplume structure, with one hemisphere predominating. The gravitational mass of the resid- ual proto-neutron star at ∼ 677 ms is ∼ 1.42 M . Even at the end of the simulation, explosion in most of the solid angle is accompanied by some accretion in an annular region at the wasp-like waist of the debris field. The ejecta electron fraction ( Y e ) is distributed between ∼ 0.48 and ∼ 0.56, with most of the ejecta mass proton-rich. This may have implications for supernova nucleosynthesis, and could have a bearing on the p- and ν p-processes and on the site of the first peak of the r-process. The ejecta spatial distributions of both Y e and mass density are predominantly in wide-angle plumes and large-scale structures, but are nevertheless quite patchy.en_US
dc.format.extent351 - 369en_US
dc.language.isoen_USen_US
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_US
dc.rightsAuthor's manuscripten_US
dc.titleA successful 3D core-collapse supernova explosion modelen_US
dc.typeJournal Articleen_US
dc.identifier.doidoi:10.1093/mnras/sty2585-
dc.date.eissued2018-09-24en_US
pu.type.symplectichttp://www.symplectic.co.uk/publications/atom-terms/1.0/journal-articleen_US

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