# Presentation: 478430

## Nucleosynthesis in Core-Collapse Supernovae

- Nucleosynthesis in Core-Collapse Supernovae

- Ken Nomoto (U. of Tokyo)

## B2FH  1957  October

**Fe-peak**

**Solar Abundances**

**SN1987A**

## Line -rays from SN1987A

**Line ********-rays from SN1987A**

**E(MeV)**

**counts/sec**

## 56Co-decay

## SN 1987A vs 1997D

**SN 1987A vs 1997D**

- Turatto, Mazzali, Young, Nomoto, Iwamoto et al. (1998)

- 1997D

- 1987A

- 1987A

- 1997D

- LBOL

- Mms~20M

- Mms~ 25-30M  R   ≤  300R

- M(56Ni)
-           0.07M
-  0.002M

- E~4×1050erg                 narrow lines

## The First Stars ?

**The First Stars ?**

## Metal Poor Stars 

- Mega Metal Poor (MMP):        [Fe/H] < -6
- Hyper Metal Poor (HMP):        [Fe/H] < -5
- Ultra Metal Poor (UMP):          [Fe/H] < -4
- Extremely Metal Poor(EMP) :  [Fe/H] < -3
- Very Metal Poor (VMP):           [Fe/H] < -2
- Metal Poor (MP) :                     [Fe/H] < -1
- Solar:                                        [Fe/H] ~ 0
- Super Metal Rich(SMR):          [Fe/H] > +0.5
-                                                                         [Fe/H]=log(Fe/H)-log(Fe/H)
-                                (Beers & Christlieb 2005)

## Hyper Metal-Poor Star (SUBARU)

- Frebel, Aoki, et al.

- [Fe/H] = -5.6

- [Fe/H] = -3.7

- [Fe/H] = -3.2

## Hyper Metal-Poor Stars

- Frebel, Aoki, et al.

## Metal-Poor Stars

**Metal-Poor Stars**

## 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.

## Kobayashi, Umeda, Nomoto et al. 2006

## GRB-associated Supernovae

| SNe Ic |  |
| --- | --- |
| SN | GRB |
| 1998bw | 980425 |
| 1997ef | (971115) |
| 2002ap |  |
| 2003dh | 030329 |
| 2003lw | 031203 |
|  |  |
|  |  |
|  |  |

- GRB 980425

## 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**

## 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

## Diversity

**GRB-SN**

**XRF-SN**

**Non-GRB HN**

## XRF-SN

**SN1994I**

**SN2006aj**

**SN2003lw**

**SN1997ef**

**SN2002ap**

**SN2003dh**

**SN1998bw**

**XRF-SN**

## Non-GRB HN

**SN1994I**

**SN2006aj**

**SN2003lw**

**SN1997ef**

**SN2002ap**

**SN2003dh**

**SN1998bw**

**Non-GRB HN**

## SN Ib 2005bf

## SNe (Mms-E relation)

- SNe (Mms-E relation)

- broad line SNe

- GRB-HNe

- Hypernovae

- faint (dark) SNe/HNe

## faint (dark) SNe/HNe

- Hypernovae

## Slide 28

## 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**

- Maeda et al. (2002, 2005)
- Mazzali et al. (Science 2005)

**Hypernova:**
**    ****Bipolar Explosion**** **

- 56Fe

- 16O

- [OI] 6300A (SUBARU)

## Element Distribution                 in Bipolar  Explosion  

**Element Distribution                 in Bipolar  Explosion  **

- Zn

- Mn

- Mn

- Zn

**Maeda & Nomoto (2003), ApJ, 598, 1163**

## Spherical               25M, E51=1

- Jet               25M, E51=7

- [Cr/Fe]

- [Mn/Fe]

- [Co/Fe]

- [Zn/Fe]

- 1

- 0

- -1

- 1

- 0

- -1

- [Fe/H]

- 4

- 2

- 0

- 4

- 2

- 0

## 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)

## Hyper Metal Poor Star

- Frebel et al. (2005)

## 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?

## Hyper Metal Poor (HMP) stars

**Iwamoto et al. (Science 2005)**

##  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**

## Hyper Metal Poor (HMP) stars

- Co

- Ti

## 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. 07
- ApjL in press)

- 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.

## [C/Fe]

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

- .

- HMP stars

- CEMP stars

- EMP stars

**[C/Fe]**

**HMP**

**CEMP**

**EMP**

**UMP**

**[Fe/H]**

## CEMP stars

- (Depagne et al. 02)
- M(56Ni)~8x10-4M

- EMP stars
- (Cayrel et al. 04)
- M(56Ni)~0.2M

- HMP stars
- (Christlieb et al. 02)
- (Frebel et al. 05)
- M(56Ni)~3x10-6M

## Possible Types of SN-HN  

**Type Ib Hypernova ? (Helium in mixed WR)**
**Type II Hypernova ?**
- Rotating Black-Hole + H-rich Envelope (low metallicity?)
**Faint SN Ibc ?**
- Small 56Ni (fallback) + No Shock Heating
**Faint Hypernovae (fallback of ****56****Ni) ******** **
**Dark SN/HN****  (****Long GRB + no SN****) **

**(Nomoto @ Venice conf., 2006 June 5-9: astro-ph/0702472)**

- Della Valle et al. 2006

**non-SN GRB**

**GRB 060614**

- GRB060614

- Fynbo et al. 2006

**non-SN GRB**

## SN-GRB Connection

- GRB-HN

- Magnetar

- Non-SN GRB

## SN 2006gy

- 06gy R

- 02ic bol

- 98bw bol

- M(56Ni)~13M
- or
- CSM interaction

- M(56Ni)~0.4M

- CSM interaction

## Pair Instability Supernovae (130M-300M)

## SN2006gy vs PISN

**PISN**

##      The First Star Candidates 
M > 105M:SMS (Super Massive Stars)
      GR instability         Collapse
M ~ 300-105M: CVMS
      Collapse (& Explosion )
              IMBH   ICM, IGM      ○     
M ~ 130-300M:
   Pair  Instability        Nuclear Explosion
       [Zn/Fe]   <  -0.8
          [C/Fe]     <   0        too much Fe
M ~ 8-130M:
      Core Collapse

- M > 105M:SMS (Super Massive Stars)
-       GR instability         Collapse
- M ~ 300-105M: CVMS
-       Collapse (& Explosion )
-               IMBH   ICM, IGM      ○
- M ~ 130-300M:
-    Pair  Instability        Nuclear Explosion
-        [Zn/Fe]   <  -0.8
-           [C/Fe]     <   0        too much Fe
- M ~ 8-130M:
-       Core Collapse

**Hypernovae****     **
**SNe ****II****                  **

## 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**

## 56Ni

- 56Ni
- O

- Tominaga et al.

## Neutron-rich Nucleosynthesis  

**Nucleosynthesis in Disk Wind **(McFayden, Pruet et al.)
**    **- Fe, K, Sc, ,,  r-process ?  (Ye, entropy)
**r-process cite**
- Rotating Black-Hole + H-rich Envelope (low metallicity?)
**r+s stars ?**  (ONeMg core-collapse?)
**Nucleosynthesis in Super Metal-Rich stars**
**    **planet-host ?