Nucleosynthesis in Population III Supernovae and Abundance Patterns of Hyper Metal-Poor Stars N. Tominaga, H. Umeda, K. Maeda, K. Nomoto (Univ. of Tokyo), N. Iwamoto (JAERI)

Contents Hyper Metal-Poor stars Supernovae of Population III stars Comparison with abundance patterns of observed stars 1-Dimensinal Mixing-Fallback model 2-Dimensional Jet model

Hyper Metal-Poor Stars

Metal-Poor Stars Hyper Metal-Poor (HMP): Ultra Metal-Poor (UMP): [Fe/H]= log10(N(Fe)/N(H)) -log10(N(Fe)/N(H))8 Hyper Metal-Poor (HMP): Ultra Metal-Poor (UMP): Extremely Metal-Poor (EMP) : Very Metal-Poor (VMP): Solar: [Fe/H] < -5 [Fe/H] < -4 [Fe/H] < -3 [Fe/H] < -2 [Fe/H] ~ 0 (Beers & Christlieb 2005) Compare with results of nucleosynthesis calculations.

Metal-Poor Stars-2 Reflect abundance patterns of the early Universe The abundance patterns of ejecta from Pop III or Pop II SNe A gap exists between EMP stars and HMP stars. HMP [Fe/H] < -3 stars: Individual SN yields [Fe/H] ~ -2.5 stars: IMF integrated yield of PopIII (or EMP) SNe UMP C-rich EMP EMP

Population III Supernovae

Population III Supernovae Pair-Instability Supernovae 140~300M8 Evolution H He Observationally no evidence H,He O Si Fe Pop III stars 11M8~130M8 BH/NS Core-Collapse Supernovae

Explosion and Mass Cut Post-shock T T∝R-3/4E1/4 High T (T>5×109K) Shock Propagation Post-shock T T∝R-3/4E1/4 Mass Cut Mcut Fe High T (T>5×109K) Fe,α,Ti,Zn,Co,V Middle T (>T>4×109K) Fe,Si,Cr,Mn Low T (>T>3×109K) Si The boundary between the ejecta and the central remnant

Hypernova and faint SN Hypernova Branch Faint SN Branch Nomoto et al. 2003 (astro-ph/0308136) Hypernova Branch Faint SN Branch

Comparison with Abundance Patterns of Observed Stars HMP stars HE0107-5240 (Cristlieb et al. 2002) HE1327-2326 (Frebel, Aoki, et al. 2005) C-rich EMP stars CS29498-043 (Aoki et al. 2004) EMP stars -4.2<[Fe/H]<-3.5 (Cayrel et al. 2004) VMP stars -2.7<[Fe/H]<-2.0 (Cayrel et al. 2004)

1-Dimensional Mixing-Fallback Model

EMP Stars -4.2<[Fe/H]<-3.5 Hypernova Model: M=25M☉, 2×1052erg Tominaga et al. 2005

Mixing-Fallback Model Mixing region Fallback Fe BH Mixing Region f : ejection factor Mixing Umeda & Nomoto 2002 Fallback

EMP Stars f=0.1 -4.2<[Fe/H]<-3.5 Hypernova M=25M8,1×1051erg Normal SN -4.2<[Fe/H]<-3.5 f=0.1 Hypernova Model: M=25M☉, 2×1052erg Tominaga et al. 2005

C-rich EMP Stars f~10-3 CS29498-043 Model: M=50M☉, 5×1052erg Umeda & Nomoto 2005

VMP Stars -2.7<[Fe/H]<-2.0 Model: Z=0 IMF integrated (11~70M8) Tominaga et al. 2005

Conclusion (Mixing-Fallback model) Faint SN Normal SN + Hypernova Faint SN Hypernova Mass Energy (1051erg) f M(Fe) Stars Hypernova 25~50? 20~40 0.1 0.1~0.2 EMP Faint SN (EMP) 25~100? <1 10-3 0.01 C-rich EMP Faint SN (HMP) 10-5 HMP Normal SN 13~20 1 0.07 VMP ~ ~

2-Dimensional Jet-induced Model

Massive Stars Explosion Central Remnant <25M8 Neutron Star 25M8< Black Hole BH/NS Massive stars (M>25M8) Spherical explosion Never succeeded, except for Wilson 1985 Jet-like explosion Collapsar Model (MacFadyen, Woosley, & Heger 2001)

Jet-induced explosion Tominaga et al. 2005 Jet Jet Hydrodynamics of relativistic jets Nucleosynthesis BH BH Progenitor cf. Collapsar model (MacFadyen, Woosley, & Heger 2001) MMS=40M8 . Mcut (Mcut=1.75M8) θjet (θjet=5°) vjet (vjet=0.98c, Γjet=5) Ejet (Ejet= Ejet×tjet=1.5×1052erg) fth (fth=Eth/ Ejet=10-3) Ejet: Energy injection rate (Rotation etc.) .

Multi-dimensional relativistic hydrodynamics ←Lorentz factor Conserved quantity (D,S1,S2,S3,τ) ←Density ←Momentum ←Energy ←Equation of continuity ←Conservation of momentum ← Conservation of energy Marti & Muller 1994 ¨

Density structure 1s after 3s after 5s after 10s after

Fallback-Ejection . 1D: ejection factor f 2D: Ejet Fallback He Jet materials : O/C Jet fallen-back materials ejected as jets O/Mg Si stellar materials : Fe Fallback materials outside the fallback region

After explosion (100sec) log scale Jet materials Density structure 12 Fe Density structure 11 Fe Stellar materials linear scale Fallback 10 10 10.5 11 11.5 12 log10(R)

. Dependence: Ejet . . . . . Ejet↓: Fallback↑ M(Fe)↓ [X/Fe]↑ Ejet,51=Ejet/1051erg/s . . Ejet,51=15 Ejet,51=0.3 He O/C O/Mg Si Fallback Fallback Fe

. Dependence: Ejet . . EMP stars C-rich EMP stars CS29498-043 EMP stars Ejet,51=15 -4.2<[Fe/H]<-3.5

Conclusion . . . . . . . (Jet Model) MP stars C-rich EMP MP stars EMP stars: Ejet,51=15 C-rich EMP stars: Ejet,51~1 HMP stars: Ejet,51=0.15 UMP stars (-5<[Fe/H]<-4) EMP stars: Ejet,51>1 HMP stars: Ejet,51<0.5 . Abundance ratio [X/Y] . . HMP Ejet,51 EMP . M(Fe)star M(Fe)jet EMP UMP Fe Mass [M8] . Few stars . HMP . Ejet,51

Summary Both of the 1D & 2D models can reproduce the observations. 1D 2D HMP f=10-5 Ejet,51<0.5 UMP 10-5<f<10-3 0.5<Ejet,51<1 C-rich EMP f=10-3 Ejet,51~1 EMP f=0.1 Ejet,51~10 . . . . The properties of 2D Jet model The f in 1D model corresponds to the Ejet. The absence of UMP stars can be understood by the narrow range of Ejet. . .