# Presentation: 478428

## Nucleosynthesis in Massive Pop III Stars

- Ken Nomoto (U. of Tokyo)

## Kobayashi, Umeda, Nomoto et al. 2006

## Mn

**Mn**

**Co**

**Cr**

**Zn**

**trend**

**McWilliam,  Ryan  **

**[Fe/H]**

**[Fe/H]**

## Cayrel et al. (2004)

**Notes:**
I will talk about Hyper metal-poor stars.

## Metal-Poor Stars

**Metal-Poor Stars**

**HMP**

**C-rich EMP**

**EMP**

**UMP**

## Spectra of Supernovae & Hypernovae

- Ia

- Ic

- Ib

- 94I

- 97ef

- 98bw

- He

- Ca

- O

- SiII

- Hyper  -novae

**Spectra of ****Supernovae & Hypernovae**

**Hypernovae**:
-   _broad features_
- _  _
-   blended lines
-   “_Large mass_ at _high velocities_”

**Ic**: no H,
-      no strong He,
-      no strong Si

## GRB-SN

**SN1994I**

**SN2006aj**

**SN2003lw**

**SN1997ef**

**SN2002ap**

**SN2003dh**

**SN1998bw**

**GRB-SN**

## 56Co-decay

## Supernova – GRB Connection

| GRB | SN | MCO/M | Mms/M | E/1051erg | M(56Ni)/M |
| --- | --- | --- | --- | --- | --- |
| 980425 | 1998bw | 14 | 40 | 30 | 0.4 |
| 030329 | 2003dh | 11 | 35 | 40 | 0.35 |
| 031203 | 2003lw | 16 | 45 | 60 | 0.55 |

- Three GRB-SNe = all Type Ic Hypernovae
-                                 E > 1052 erg (~10×normal SN)
-                                 Large Mms →Black Hole Forming SNe
-                              Aspherical

## Hypernova in Prague

## Hypernova in Prague

## SNe (Mms-E relation)

- SNe (Mms-E relation)

- broad line SNe

- GRB-HNe

- Hypernovae

- faint (dark) SNe/HNe

## Hypernova Nucleosynthesis

- Low energy

- High energy

- (1) M(Complete Si-burning)
- 	(Zn, Co)/Fe
- 	(Mn, Cr)/Fe
- 	Fe/(O, Si)
- (2) More ‐rich       entropy
- 	Zn/Fe             64Ge
- 	Ti/Fe
- (3) More O burns
- 	(Si, S, Ca)/O

**Hypernova Nucleosynthesis**

## EMP stars vs. Normal SN II

- EMP stars vs. Normal SN II

- T

- Tominaga, Umeda, Nomoto (2006)

## EMP stars vs. Hypernova (E51=10)

- EMP stars vs. Hypernova (E51=10)

- Tominaga, Umeda, Nomoto (2006)

## SN-induced Star Formation

-  (M, E,  mass cut)
****** ****[X/Fe]  -  [Fe/H] **

**Fe/H ∝ M(Fe)/M(H)∝ M(Fe)/E**
**M(Fe): Fe mass in SN ejecta**
**M(H): Mass of swept up H ∝ E**
**E: Explosion Energy **

**Fe, C, O, Mg, Si, Ca**

**H, He**

## Slide 17

## Hyper Metal Poor star: HE0107-5240

- Discovery:
-           (Christrieb et al. 2002)
- Red-giant   ~ 0.8 M
**[Fe/H] ~ - 5.2**
-   **[C/Fe] ~ + 4**
- Pop III (first generation) or Second generation?
- Formation of Pop III
-      low mass star?

##  M=25M, E=7×1050erg      [Fe/H]=-5.3

-  M=25M, E=7×1050erg      [Fe/H]=-5.3

- Mr (M)

- 0

- -1

- -2

- -3

- -4

- 2

- 4

- 6

- 8

**He**

**H**

**C**

**C**

**O**

**O**

**N**

**Ne**

**Mg**

**56****Fe**

**Ti**

**58****Ni**

- Log X

**ejecta**

**Fallback**

- MBH ~6M

**Umeda & Nomoto (2003)**

**Mixing**

## HMP stars: 1D Low E models (E51< 1) mixing & fallback  low [Co/Fe]

- Co

- Ti

- Iwamoto et al. (2004)

## Jet-induced Nucleosynthesis

**Jet-induced Nucleosynthesis**

**Jet**

- BH/NS

- BH

*E*dep:
- Energy deposition rate
-              (Rotation, ***B*** etc.)

- .

- cf. “Collapsar”(e.g., MacFadyen et al. 01)
-        Magnetorotational Supernovae
-                            (e.g., Moiseenko et al. 06)

**Jet**

- Special relativistic hydrodynamics (Tominaga et al.
- ApjL 2007)

- Same mass and explosion energy

- 40*M*            15x1051erg

**Notes:**
In our Jet-induced explosion model, first the central region collapses to a black hole, and jets are injected from the central region.
As the time proceeds, the materials of the horizontal region fallback to the central region. And the jets propagate the stars.
Relativistic hydrodynamical calculations are performed and then nucleosynthesis calculations are performed with the results of the hydrodynamical calculations.
In this study, we investigate the dependence on the energy injection rate, E dot jet.
The energy injection rate may vary by the rotation or the energy conversion efficiency and so on.
The other parameters like these are kept at same value.
For example, Mass Cut, the initial black hole mass, is kept at 1.75 solar mass.

## M(56Ni)

- Smaller *E*dep 
-   smaller *M*(56Ni)
-           and
-     larger [C/Fe]

- .

- HMP stars

- UMP stars

- EMP stars

- CEMP stars

**E****dep**

**[C/Fe]**

**.**

- High *E*  Fallback

## HMP Stars

- Tominaga et al. 2007

**Jet-induced **
**SN models**

**HMP Stars**

**High E** 
- High Co/Fe
- 
**Fallback** 
- Small Fe

##    UMP Star : [Fe/H] = -4.75   Hypernova model (E51=20:1D)Co

** ****  ****UMP Star : [Fe/H] = -4.75****  **** ****Hypernova model (E****51****=20:1D)********Co**

- (Norris, Christlieb, et al. 2007)

## Abundance distribution

- Mixing region

- 64Zn

- 12C

- 4He

- 1H

- 16O

- 24Mg

- 28Si

- 56Ni(Fe)

- 40Ca

## HMP/UMP/EMP stars

| Star | [Fe/H] | Features | Authors |
| --- | --- | --- | --- |
| HE0107 | -5.7 | C-rich, [Mg/Fe]~0 , Co-rich | Christlieb et al.
Bessel & Christlieb |
| HE1327 | -5.4 | C, O, Mg-rich | Frebel et al.
Aoki et al. |
| HE0557 | -4.75 | C,Ca,Sc,Ti-rich, Co-rich | Norris et al. |
| HE1300 | -3.88 | C, Si, Ca,Sc,Ti, Co-rich | Frebel et al. |
| HE1424 | -3.96 | Si,Ca,Cu-poor, Co,Mn-rich | Cohen et al. |
| CS22949 | -4.0 | C,N,O,Mg,Co,Zn-rich | Depagne et al. |
| CS29498 | -3.5 | C,N,O,Mg-rich, [Co/Fe]~0 | Aoki et al. |
| BS16934 | -2.78 | C-poor , O,Mg-rich | Aoki et al. |

## CEMP-no Star (Hypernova  Co/Fe)

**CEMP-no Star (Hypernova ******** Co/Fe)**

- (Frebel et al. 2007)

## CEMP-no Star (nomral E SN)

**CEMP-no Star (nomral E SN)**

- (Frebel et al. 2007)

## CEMP stars

- (Depagne et al. 02)

**CEMP stars**

- (1D: Hypernova model)

## Si-poor EMP Star

- (Cohen et al. 2007)

**Si-poor EMP Star**

## Jet-induced SN models

**Jet-induced SN models**

- (Si-poor)

##          
       Abundance Patterns of HMP/UMP/EMP Stars

Large [Zn, Co/Fe],  [C/Fe]  (no-s)
 Nucleosynthesis in Jet-Induced Hypernovae

*Nucleosynthesis at High Entropy , Ye  ~0.5 
            Large [Zn, Co/Fe]         (Cr, K, Sc ?)

*Energy deposition rate  Fallback
            Diversity of M(Fe),  [C/Fe] 
            HMP – UMP – EMP

*Gamma-Ray Burst Connection

**       ****Abundance Patterns of HMP/UMP/EMP Stars**
- Large [Zn, Co/Fe],  [C/Fe]  (no-s)
-  Nucleosynthesis in **Jet-Induced Hypernovae**
- *Nucleosynthesis at High Entropy , Ye  ~0.5
-             Large [Zn, Co/Fe]         (Cr, K, Sc ?)
- ***Energy deposition rate**  Fallback
-             Diversity of M(Fe),  [C/Fe]
-             HMP – UMP – EMP
- *Gamma-Ray Burst Connection
**        **
**    **

**                  **

- Della Valle et al. 2006

**non-SN GRB**

**GRB 060614**

## Metal-poor stars -- GRB connection

- GRB-HNe
- No-SN GRBs

- EMP stars
- CEMP stars
- HMP stars

*E*dep

- .

- Larger

- Smaller

**GRBs**

**Metal-poor stars**

**BH-forming SNe with relativistic jets**