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Explosive nucleosynthesis in neutrino-driven, aspherical Pop. III supernovae

Explosive nucleosynthesis in neutrino-driven, aspherical Pop. III supernovae. Shin-ichiro Fujimoto (Kumamoto NCT, Japan) collaboration with M. Hashimoto (Kyusyu Univ.) , M. Ono (Kyoto Univ.), & K. Kotake (NAOJ). IAU Symposium 279 Death of massive Stars: SNe and GRBs

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Explosive nucleosynthesis in neutrino-driven, aspherical Pop. III supernovae

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  1. Explosive nucleosynthesis in neutrino-driven, aspherical Pop. III supernovae • Shin-ichiro Fujimoto • (Kumamoto NCT, Japan) • collaboration with • M. Hashimoto (Kyusyu Univ.), • M. Ono (Kyoto Univ.), • & K. Kotake (NAOJ) IAU Symposium 279 Death of massive Stars: SNe and GRBs Nikko, Japan, March 17, 2012

  2. Outline • Introduction • Observed abundance ratios of Metal-poor stars (MPSs) • Spherical models of Pop. III SNe for abundances of MPSs • Hydrodynamics simulations of aspherical Pop. III SNe driven by neutrino • Explosive nucleosynthesis in the Pop. III SNe • Comparison of the estimated abundances with the observed abundances of MPSs

  3. Observed [X/Fe] of MPSs Observed [X/Fe] Lai+08 Eu Z=30 Samples: 28MPSｓ [Fe/H]=-4.0 : 1 star -4<[Fe/H]<-3 : 8 stars -3<[Fe/H]<-2.6 : 4 stars [Fe/H]>-2.6 : 15 stars CNO Sr,Y,Zr Ba,La [X/Fe] Atomic number Dispersion C,N,O : large Na to Zn : small Sr,Y,Zr : large Ba,La,Eu : very large CNO Z=30 Na to Zn Sr,Y,Zr Ba,La [X/Fe] Eu Small dispersion Average with dispersion Atomic number Propeties of SNe during early phase of Galaxy

  4. -2.7< [Fe/H] < -2 IMF-averaged [X/Fe]: SNe Heger&Woosley10 ●: average MPSs（Lai08) ▲: IMF averaged Best Fit 10-100Msun, 1.2FOE 1D model with artificial mixing K, Sc,Ti: underproduced Na,Cu: overproduced [X/Fe] 1D Pop. III SN model for [X/Fe] of MPSs IMF-averaged [X/Fe]: SNe+HNe Tominaga07 ●: averaged ratios: MPSs（Cayrel+04) □: IMF average Z=0 1D model SNe: 13,15,18 Msun (1FOE) + HNe: 20,25,30,40,50 Msun (>10FOE) with mixing-fallback N, K, Sc,Ti, Mn: underproduced [X/Fe] Mixing is required for both models

  5. 1987A (HST) 800km x 800km Hwang+00 Si-rich, Fe-poor Jets 1600km x 1600km continuum Si Cas A (Chandra) Ca Fe Aspherical explosion in supernovae Simulation of Aspherical explosion in 2D 15Msun, entropy Marek & Janka 2009 Aspherical effects are important for successful explosion Aspherical explosion couldbe universal in SNe.

  6. Present work • Multi-D model of nucleosynthesis • in SASI-aided, neutrino-driven, aspherical SNe of Pop. III stars • based on 2D hydrodynamic simulations from the core collapse to the explosion of the stars • Explosion energy,Mass cut, & Mixing • evaluated from the hydrodynamic simulations • Neutrino luminosities & temperatures: Parameters • Proto neutron star is not included in numerical domain Abundances of nuclei from C to Zn in SN ejecta Compared with observed abundances of metal poor stars (MPSs) c.f.) Kifonidis+06 and Fujimoto+11for 15Msun star with Zsun Abundances of Solar system and SN1987A

  7. 2.8 Neutrino heating & cooling Model parameters 1.2 Change in Ye due to e-,e+ cap. & neutrino abs. pNS Isotropic emission 1200 50000 5000 Computational region Hydrodynamic simulations of SNe Simulations from the core collapse to the explosion of Pop. III stars with11-40Msun(HW10) using ZEUS2D code (Ohnishi+06) Non-rotating, zero B-fields stars

  8. Models with Explosion Models with Lnue <= Lnue_min w.o. exp. do not explode, While SN explodes promptly and quasi-spherically for Lnue > Lnue_max For progenitors heavier than 20Msun, we have searchedmore carefully the boundary whether the star explode or not, compared with lighter stars △= (Lnue_min /Lnue_max w.o.exp.) -1

  9. Sc production in high entropy bubbles 15Msun,1.00FOE [X/Mg] Entropy per baryon Enhanced via mixing Aspherical, l=1,2 modes dominant High entropy ejecta with s > 20kB Sc and Ti are produced in high entropy bubbles, driven by SASI-induced mixing Aspherical effects are essential for the enhancement 10000km x 20000km

  10. M(Fe) VS Explosion energy of ejecta M(Fe) HNe Faint SNe M(Fe) correlate with the explosion energies, Eexp Faint SNe for 11 and 15 Msun Hypernovae (HNe) for 25 and 40Msun

  11. Cayrel+04 Cayrel+04 w. NLTE Preston+06 Observed [X/Fe] of MPSs ▲ ■ ● [Mg/Fe] VS Explosion energy of ejecta [Mg/Fe] HNe [Mg/Fe] are anti-correlate with Eexp Quasi-spherical Pop. III HNe might be excluded Low mass Pop. III SNe could be faint SNe

  12. CEMP-no? [C/Fe] [Fe/H] -4 -3 C-enhanced MPS is a faint SN? [C/Fe] Ito 2011 Ito 2011 [Ba/Fe] CEMP only CEMP -s C-enhanced MPSs (CEMP) CEMP-no [Fe/H] 20% MPSs = CEMP stars Large fraction of CEMP stars = s-element rich CEMP stars (CEMP-s star) CEMP-s stars C & Ba from AGB companion in binary

  13. [X/Fe] IMF-averaged abundances ○: Case1 (Eexp～1FOE or Eexp = Eexp_min) □: Case2 (lower Eexp for lower Mms) ■: Cayrel+04+NLTE effects Explosion energy of adopted models [X/Fe] Atomic number Observed [X/Fe] are reproduced with IMF-averaged [X/Fe] for both sets, other than Na, K, and Ti Salpeter IMF

  14. Summary We have examined nucleosynthesis in neutrino-driven, aspherical Pop. III SNe, based on 2D hydrodynamic simulations of SNe for Pop. III progenitors of 11-40Msun Multi-D effects are important for nucleosynthesis Sc and Ti, which are underproduced in 1D spherical models, are abundantly produced in high entropy bubbles IMF-averaged [X/Fe] of the ejecta are consistent with observed [X/Fe] of metal-poor stars, other than K, which is underproduced by 0.8dex Low mass, Pop III SNe could be faint SNe Observed [X/Fe], in particuler [Mg/Fe] with small dispersion Origin of C-enhanced metal-poor starsw.o s-elements ?

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