Nucleosynthesis in population iii supernovae and abundance patterns of hyper metal poor stars
Download
1 / 28

Nucleosynthesis in Population III Supernovae and Abundance Patterns of Hyper Metal-Poor Stars - PowerPoint PPT Presentation


  • 141 Views
  • Uploaded on

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

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about ' Nucleosynthesis in Population III Supernovae and Abundance Patterns of Hyper Metal-Poor Stars' - arawn


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
Nucleosynthesis in population iii supernovae and abundance patterns of hyper metal poor stars

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
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



Metal poor stars
Metal-Poor Stars

[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
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 supernovae1
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

Mass Cut Mcut

Explosion and Mass Cut

Shock Propagation

Post-shock T

T∝R-3/4E1/4

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

Nomoto et al. 2003 (astro-ph/0308136)

Hypernova Branch

Faint SN Branch


Comparison with abundance patterns of observed stars
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)



EMP Stars

-4.2<[Fe/H]<-3.5

Hypernova

Model: M=25M☉, 2×1052erg

Tominaga et al. 2005


Mixing fallback model
Mixing-Fallback Model

Mixing region

Fallback

Fe

BH

Mixing Region

f : ejection factor

Mixing

Umeda & Nomoto 2002

Fallback


EMP Stars

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

CS29498-043

f~10-3

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
Conclusion (Mixing-Fallback model)

Faint SN

Normal SN

+ Hypernova

Faint SN

Hypernova

~

~



Massive stars explosion
Massive Stars Explosion

  • Massive stars (M>25M8)

    • Spherical explosion

      • Never succeeded, except for Wilson 1985

    • Jet-like explosion

      • Collapsar Model (MacFadyen, Woosley, & Heger 2001)

BH/NS


Jet induced explosion
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
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
Fallback-Ejection

1D: ejection factor f

2D: Ejet

.

He

Jet materials :

O/C

Jet

fallen-back materials

ejected as jets

O/Mg

Si

stellar materials :

Fallback

Fe

materials outside

the fallback region


After explosion 100sec
After explosion (100sec)

log scale

Jet materials

12

Fe

Density structure

11

Fe

Stellar materials

linear scale

Fallback

10

10

10.5

11

11.5

12

log10(R)


Dependence e jet

.

.

Ejet↓: Fallback↑

M(Fe)↓

[X/Fe]↑

Dependence: Ejet

.

.

Ejet,51=Ejet/1051erg/s

.

.

Ejet,51=15

Ejet,51=0.3

He

O/C

O/Mg

Si

Fallback

Fallback

Fe


Dependence e jet1

.

.

Ejet,51=1

C-rich EMP stars

CS29498-043

Dependence: Ejet

.

EMP stars

Ejet,51=15

-4.2<[Fe/H]<-3.5


Conclusion
Conclusion

(Jet Model)

C-rich EMP

Abundance ratio [X/Y]

.

  • 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

.

.

HMP

Ejet,51

EMP

.

M(Fe)star

M(Fe)jet

EMP

UMP

Fe Mass [M8]

.

Few stars

.

HMP

.

Ejet,51


Summary
Summary

  • Both of the 1D & 2D models can reproduce the observations.

.

.

.

.

  • 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.

.

.


ad