Nucleosynthesis in Population III Supernovae

and Abundance Patterns of Hyper Metal-

Poor StarsN. Tominaga, H. Umeda, K. Maeda,

K. Nomoto (Univ. of Tokyo), N. Iwamoto (JAERI)

ContentsHyper Metal-Poor starsSupernovae of Population III starsComparison with abundance patterns of observed stars

1-Dimensinal Mixing-Fallback model2-Dimensional Jet model

Hyper Metal-Poor Stars

Metal-Poor Stars

[Fe/H] < -5[Fe/H] < -4[Fe/H] < -3[Fe/H] < -2[Fe/H] ~ 0

(Beers & Christlieb 2005)

Hyper Metal-Poor (HMP): Ultra Metal-Poor (UMP): Extremely Metal-Poor (EMP) : Very Metal-Poor (VMP): Solar:

[Fe/H]=log10(N(Fe)/N(H))-log10(N(Fe)/N(H))

Compare with results of nucleosynthesis calculations.

Reflect abundance patterns of the early Universe

The abundance patterns of ejecta from Pop III or Pop II SNe

Metal-Poor Stars-2

A gap exists between EMP stars and HMP stars.HMP

C-rich EMP

EMP

UMP[Fe/H] < -3 stars:

Individual SN yields

[Fe/H] ~ -2.5 stars: IMF integrated yield of P

opIII (or EMP) SNe

Population III Supernovae

Population III Supernovae

Pair-Instability Supernovae

Core-Collapse Supernovae

Observationally no evidenceH,He

HO

11M~130M

140~300M

BH/NS

Pop III stars

FeSi

He

Evolution

Explosion and Mass Cut

The boundary between the ejecta and the central remnant

Mass Cut Mcut

Post-shock TT R∝ -3/4E1/4

Shock Propagation

•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

Fe

Hypernova and faint SNNomoto et al. 2003 (astro-ph/0308136)

Hypernova Branch

Faint SN Branch

Comparison with Abundance Patterns of Observed StarsHMP stars

HE0107-5240 (Cristlieb et al. 2002)HE1327-2326 (Frebel, Aoki, et al. 2005)

C-rich EMP starsCS29498-043 (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

Model: M=25M ,☉ 2×1052erg

EMP Stars

Tominaga et al. 2005

-4.2<[Fe/H]<-3.5

Hypernova

Mixing

Fallback

Mixing Regionf : ejection factor

Fallback

BH

Mixing regionMixing-Fallback Model

Umeda & Nomoto 2002

Fe

-4.2<[Fe/H]<-3.5EMP Stars

Model: M=25M ,☉ 2×1052ergTominaga et al. 2005

f=0.1Hypernova

M=25M,1×1051ergNormal SN

Model: M=50M ,☉ 5×1052erg

C-rich EMP Stars

Umeda & Nomoto 2005

CS29498-043

f~10-3

Model: Z=0 IMF integrated (11~70M)

VMP Stars

Tominaga et al. 2005

-2.7<[Fe/H]<-2.0

Conclusion (Mixing-Fallback model)

Faint SN

Hypernova

Normal SN + Hypernova

Faint SN

Mass Energy(1051erg)

f M(Fe) Stars

Hypernova 25~50? 20~40 0.1 0.1~0.2 EMPFaint SN (EMP) 25~100? <1 10-3 0.01 C-rich EMPFaint SN (HMP) 25~100? <1 10-5 10-5 HMP

Normal SN 13~20 1 1 0.07 VMP

~

~

2-Dimensional Jet-induced Model

Massive Stars ExplosionM Central Remnant

<25M Neutron Star

25M< Black Hole

Massive stars (M>25M)Spherical explosion

• Never succeeded, except for Wilson 1985

Jet-like explosion• Collapsar Model (MacFadyen, Woosley, & Heger 2001)

BH/NS

Jet-induced explosionJet

BH BH

MMS=40M

Mcut (Mcut=1.75M)

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.)

Hydrodynamics of relativistic jetsNucleosynth

esisProgenitor

..

cf. Collapsar model (MacFadyen, Woosley, & Heger 2001)

Jet

Tominaga et al. 2005

Multi-dimensional relativistic hydrodynamics

Conserved quantity

(D,S1,S2,S3,τ)

ph

vhS

Dcv

ii

2

2

2/1

1

0

0

0

3

1

3

1

3

1

jj

jj

ijji

jj

i

j

jj

DvSxt

pvSxt

S

Dvxt

D

←Density←Momentum←Energy

←Equation of continuity

←Conservation ofmomentum

← Conservation of energy

←Lorentz factor

Marti & Muller 1994¨

1s after 3s after

5s after 10s after

Density

structure

Fallback-Ejection

Fallback

JetO/C

He

O/Mg

Si

Festellar materials :

Jet materials :

fallen-back materials ejected as jets

materials outside the fallback region

1D: ejection factor f2D: Ejet

.

After explosion (100sec)

10 10.5 11 11.5 12log10(R)

10

11

12

log scale

linear scale

Jet materials

Stellar materials

Fallback

Density structure

Fe

Fe

Dependence: Ejet.

Ejet,51=15

Ejet,51=Ejet/1051erg/s

Ejet,51=0.3

Fallback Fallback

Ejet↓: Fallback↑

M(Fe)↓ 　 [X/Fe]↑

... .

.

O/CHe

O/Mg

Si

Fe

Dependence: Ejet.

Ejet,51=15. EMP stars

-4.2<[Fe/H]<-3.5

Ejet,51=1.

C-rich EMP stars

CS29498-043

ConclusionMP 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

EMP

C-rich EMP

HMP

EMP

HMP

UMPFew stars

Abu

ndan

ce ra

tio [X

/Y]

Ejet,51

.

Ejet,51

.

Fe M

ass

[M]

...

.

.

M(Fe)star

M(Fe)jet

(Jet Model)

SummaryBoth of the 1D & 2D models can reproduce the observations.

1D 2DHMP 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 modelThe f in 1D model corresponds to the Ejet.

The absence of UMP stars can be understood by the narrow range of Ejet.

...

.

.