1. 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)

2. 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

3. Hyper Metal-Poor Stars

4. 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.

5. 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

6. Population III Supernovae

7. 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

8. 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

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

10. Comparison with Abundance Patterns of Observed Stars
HMP stars
HE (Cristlieb et al. 2002)
HE (Frebel, Aoki, et al. 2005)
C-rich EMP stars
CS (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)

11. 1-Dimensional Mixing-Fallback Model

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

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

14. 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

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

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

17. 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 ~ ~

18. 2-Dimensional Jet-induced Model

19. 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)

20. 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.) .

21. 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

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

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

24. After explosion (100sec) log scale Jet materials Density structure12 Fe
Density structure 11 Fe
Stellar materials
linear scale
Fallback 10 10
10.5 11
11.5 12
log10(R)

25. . 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

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

27. 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

28. 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. . .