PUSHing CORE-COLLAPSE SUPERNOVAE TO EXPLOSIONS IN SPHERICAL SYMMETRY
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1 PUSHing CORE-COLLAPSE SUPERNOVAE TO EXPLOSIONS IN SPHERICAL SYMMETRY Fifty-One Ergs Oregon State June 2017 Ebinger In collaboration with: Sanjana Sinha Carla Fröhlich Albino Perego Matthias Hempel
2 Outline CCSN Modeling: PUSH Best Fit of SN1987A Calibration of PUSH Lscape of Supernovae Properties of Remnants Conclusion Outlook the Poincaré Group the Poincaré Sphere 2
3 CCSNe: -driven mechanism CCSNe, among the strongest explosions in the universe Source of heavy elements Driving force of cosmic cycle of matter Collapse releases gravitational binding energy: Explosion energy: ~ Crab nebula: eso.org Prompt shock stagnation -driven mechanism: convection multi-d instabilities (e.g. Bethe&Wilson85, Janka&Müller94, Janka01, Blondin&Mezzacappa07) adapted from Janka (2001) the Poincaré Group the Poincaré Sphere 3
4 CCSN Modeling in 1D Efficiently study broad range of CCSN progenitors in 1D: Induced explosion with different methods Piston/thermal bomb Limitations: (Woosley & Weaver 95, Chieffi & Limongi 13, Thielemann+ 96, Umeda & Nomoto 08) Physics of collapse, bounce, onset of explosion Neutrinos, PNS Mass cut Explosion energy Ni yields Using Neutrinos: Light bulb (e.g. Yamamoto+13): neutrino luminosities energies Modified reactions (e.g. Fröhlich+06, Fischer+10): PNS evolution Parametrized PNS contraction (Ugliano+12, Ertl+16, Sukhbold+16): Nuclear physics (EOS, BH formation), (mapping to Kepler with piston) the Poincaré Group the Poincaré Sphere 4
5 CCSN Modeling in 1D Efficiently study broad range of CCSN progenitors in 1D: Induced explosion with different methods Piston/thermal bomb Limitations: (Woosley & Weaver 95, Chieffi & Limongi 13, Thielemann+ 96, Umeda & Nomoto 08) Physics of collapse, bounce, onset of explosion Neutrinos, PNS Mass cut Explosion energy Ni yields Using Neutrinos: This work: PUSH method, introduced in Perego, Hempel, Fröhlich, Eichler, Casanova, Liebendörfer, Thielemann15 Parmetrization of -driven mechanism: use 's to obtain explosion properties (, nucleosynthesis yields) preserve consistent evolution (no modification of - transport) Nuclear EOS PNS evolution included the Poincaré Group the Poincaré Sphere 5
6 Parametrized CCSNe: PUSH Basic idea: tap a fraction of the, luminosity inside the gain region to mimic the enhanced heating efficiency of, neutrinos due to convection late accretion (multi-d effects) Temporal evolution heating cooling PNS Typical neutrino cross section Spectral energy flux Location function the Poincaré Group the Poincaré Sphere 6
7 Parametrized CCSNe: PUSH Basic idea: tap a fraction of the, luminosity inside the gain region to mimic the enhanced heating efficiency of, neutrinos due to convection late accretion (multi-d effects) Temporal evolution: Free parameters: 50 ms 500 ms Fixed parameters: = 80 ms =1s the Poincaré Group the Poincaré Sphere 7
8 Numerical Setup of PUSH 1D progenitor models (Woosley+02, Woosley&Heger07, A. Menon private communication) General relativistic hydrodynamics: AGILE (Liebendörfer+02) EOS: - NSE: nuclear EOS HS(DD2) (Hempel&Schaffner-Bielich+02) Typel+10) - non-nse: ideal gas with approx. alpha-network Neutrino transport: IDSA/ASL (Liebendörfer+09, Perego+16) Ebinger+ in preparation the Poincaré Group the Poincaré Sphere 8
9 Progenitors compactness A crucial property of CCSN progenitors is their compactness Blue supergiants (A.Menon): 16.8, 19.8, 20.8 Metallicity: e.g. s-progenitors (WHW02) Grey region: mass range of SN1987A Introduced by O'Connor & Ott 11 the Poincaré Group the Poincaré Sphere 9
10 Best Fit of SN1987A Calibration of PUSH Best fit: reproducing SN 1987A Crab like SNe Possible BH formation Seitenzahl+ 14, Fransson & Kozma 02, Blinnikov+ 00 Best fit for SN1987A with BSG progenitor is used as constraint in the investigation of large progenitor samples Metallicity: Freedom in fitting: consistent results of nucleosynthesis yields explosion energy without fallback the Poincaré Group the Poincaré Sphere 10
11 Best Fit of SN1987A Calibration of PUSH Best fit: reproducing SN 1987A Crab like SNe Possible BH formation For higher main-sequence masses: branching in Hypernovae Faint SNe HNe: very energetic explosions, driven by fast rotation strong magnetic fields -driven SNe go into branch above ~20-25 fit of PUSH to observational properties of CCSNe for lower mass progenitors branch for higher masses the Poincaré Group the Poincaré Sphere 11
12 Best Fit of SN1987A Calibration of PUSH Best fit: reproducing SN 1987A Crab like SNe Possible BH formation Compilation of observational data: Nomoto+13, Bruenn+16 references therein the Poincaré Group the Poincaré Sphere 12
13 PUSH with Dependence on Compactness PUSH parameter function: Parabola fit is the simplest most natural fit through 3 points for the Poincaré Group the Poincaré Sphere 13
14 Supernova Lscape: Explodability, Faint branch WHW02 WH07 BH With : BH formation Lower explosion energies for small ZAMS masses Good agreement with the observational properties (explosion energy) SN1987A cidates are obtained within the two progenitor samples with solar metallicity the Poincaré Group the Poincaré Sphere 14
15 Dependence of Ni Explosion Energy Good agreement with observations the Poincaré Group the Poincaré Sphere 15
16 Ejecta as a Function of Compactness In more detail in talk of S. Sinha For symmetric nuclei we find a linear trend with compactness Mainly dependent on explosion energy More complex situation for asymmetric nuclei (neutron rich) Progenitor structure ( of innermost ejecta) the Poincaré Group the Poincaré Sphere 16
17 Ejecta WHW02 Linear trend of Ni with explosion energy (also Pejcha+15) High Ti yields Best fit of SN1987A contained in the parabola fit the Poincaré Group the Poincaré Sphere 17
18 Outlook: BHs NS birthmass distribution Preliminary: From the predicted NS masses one can compute the neutron star birth mass distribution in a galaxy, as well as the number of black holes With IMF from Salpeter (for massive stars heavier than 10 ) WHW02 WH07 gravitational neutron star mass distribution (cold neutron stars) split in the contributions of the different ZAMS masses of the progenitors the Poincaré Group the Poincaré Sphere 18
19 Conclusion Outlook Can reproduce SN1987A Fit of PUSH to larger set: observational constraints Supernova lscape, dependence of compactness Good agreement with observational properties of CCSNe below 25 with branch Observed trend of explosion energy Ni yields Influence of progenitor models Compare predicted neutron star black hole masses to observations Predicted explosion properties can be used in GCE calculations the Poincaré Group the Poincaré Sphere 19
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