Hypernova Nucleosynthesis

Hypernova Nucleosynthesis
GRB980425
SN1998bw
Ken Nomoto (Kavli IPMU/ U.Tokyo)
Supernova Nucleosynthesis
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Core Collapse Supernovae : C, O, Mg, Si, Ca, Fe, , ,
Thermonuclear Supernovae : Fe, Si, ,
Long Gamma-Ray Bursts --- Hypernovae ??
Short Gamma-Ray Bursts --- Kilonovae ??
Yields from Core-Collapse SNe
[X/Fe]
Z=0
20M
25M
(Nomoto, Kobayashi, Tominaga 2013 ARAA 51, 457-509)
Z = 0.02
Yields from Core Collapse Supernovae
in Metal-Poor Environment
＊Comparison with Extremely Metal-Poor Stars
Yield from an individual SN
[environment with much less contamination
less mixing]
 Yields of unusually faint & luminious SNe
＊First Stars, First SNe?
Metal Poor Stars
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Mega Metal Poor (MMP):
Hyper Metal Poor (HMP):
Ultra Metal Poor (UMP):
Extremely Metal Poor(EMP) :
Very Metal Poor (VMP):
Metal Poor (MP) :
Solar:
Super Metal Rich(SMR):
[Fe/H] < -6
[Fe/H] < -5
[Fe/H] < -4
[Fe/H] < -3
[Fe/H] < -2
[Fe/H] < -1
[Fe/H] ~ 0
[Fe/H] > +0.5
[Fe/H]=log(Fe/H)-log(Fe/H)
(Beers & Christlieb 2005)
VMP Stars vs. Normal SN II (10 - 50 M)
(-2.7 < [Fe/H] < -2.0)
(Salpeter IMF)
(Tominaga, Umeda, Nomoto 06)
EMP Stars vs. Normal SN II
(-4.2 < [Fe/H] < -3.5)
(E51=1)
(Poor fit)
Co
Zn
Tominaga,
Umeda, Nomoto (2006)
T
CEMP-no Star (nomral + fallback SN)
(Poor fit)
Si
(Tominaga et al.)
Co
(Frebel et al. 2007)
Hyper Metal-Poor (HMP) Stars
[Fe/H] < -5
[C, N, O/ Fe] > 3
[X/H]
C,N
Na,Mg,Al
Ca, Ti
Fe
Christlieb, Frebel, Aoki, et al.
McWilliam(1995), Ryan(1996)
EMP
stars
Co
Cr
trend
[Fe/H]
[Fe/H]
Mn
Zn
GRB-Supernovae
SN 1998bw
SNe Ic
SN
GRB
1998bw
1997ef
2002ap
2003dh
2003lw
980425
(971115)
030329
031203
Galama et al.
GRB 980425
GRB-SN Connection
(GRB 030329 / SN 2003dh)
Stanek et al (2003) ;Hjorth et al (2003)
Broad Lines!
Spectra of Supernovae & Hypernovae
Ic: no H,
Ia
Ib
SiII
O Ca
He
Ic
Hyper
-novae
no strong He,
94I
97ef
98bw
no strong Si
Hypernovae：
broad features
blended lines
“Large mass at
high velocities”
Patat et al. (1999)
Spectral Fitting: SN1997ef
Iwamoto et al.
(2000)
Too Narrow Features
E51=E/1051 erg
Normal SN
(E51=1)
Small Mej
Broad Features
Hypernova
(E51=20)
Large Mej
at High Vel.
CO Star Models for SNe Ic
Parameters [Mej, E, M(56Ni)]
H-rich
He
Light Curve
５６Fe
C+O
MC+O
Si
Fe
Mms/M
56Co
56Ni
Collapse
MC+O/M
~ 40
13.8
~ 35
11.0
~ 22
5.0
Spectra
τ ~ [τdyn • τdiffusion]1/2 E ∝ Mej
κ Mej 1/2
R
~ V
• Rc
∝ κ½Mej¾E
E ∝ Mej3
-¼
５６Ni
56Co-decay
GRB-SN
SN2003dh
SN2003lw
SN1998bw
SN2006aj
SN1997ef
SN1994I
SN2002ap
Hypernova – GRB Connection
Three GRB－SNe = all Type Ic Hypernovae
E > 1052 erg (～10×normal SN)
Large Mms →Black Hole Forming SNe
Aspherical
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
GRB
SN
Hypernova in Prague
SNe [Mms-E relation]
(Rapidly rotating BH?)
Nomoto et al. (2003)
SNe [Mms-M(56Ni) relation]
Nomoto et al. (2003)
Type Ibc SNe:
Bipolar Explosion
56Fe
[OI] 6300A (SUBARU)
16O
Maeda et al. (2002, 2005)
Mixing & Fallback Supernova
 Carbon Enhanced Metal Poor
(CEMP) Stars
N
 M(Fe),
M(BH)
S
(Jet-induced)
SN-GRB Connection
GRB-HN
Magnetar
Non-SN GRB
M(56Ni)
Bright HN
.
Dark HN
Smaller Edep 
smaller M(56Ni)
and
larger [C/Fe]
HMP stars
UMP stars
[C/Fe]
High E  Fallback
Tominaga et al. (2007)
EMP stars
.
Edep
CEMP stars
Dark Hypernova
non-SN GRB
GRB 060614
Della Valle et al. 2006
Fynbo et al. 2006
Gal-Yam et al. 2006
Hypernova
Nucleosynthesis
(1) M(Complete Si-burning)
(Zn, Co)/Fe
(Mn, Cr)/Fe
Fe/(O, Si)
(2) More α‐rich
Zn/Fe
entropy
64Ge
Ti/Fe
Low energy
High energy
Jet + Fallback
~ Mixing & Fallback
(3) More O burns
(Si, S, Ca)/O
EMP Stars vs. Normal SN II
(-4.2 < [Fe/H] < -3.5)
(E51=1)
(Poor fit)
Co
Zn
Tominaga,
Umeda, Nomoto (2006)
T
EMP stars vs. Hypernova (E51=10)
(-4.2 < [Fe/H] < -3.5)
(better fit)
Co
Zn
Tominaga, Umeda, Nomoto (2006)
CEMP-no-s Star (Hypernova with fallback)
(better fit)
Si
(Tominaga et al.)
Co
(Frebel et al. 2007)
UMP Star : [Fe/H] = -4.75
Hypernova model (E51=20:1D)Co
(Norris, Christlieb, et al. 2007)
HMP Stars
(Frebel et al. 2004)
( [Fe/H] < -5)
Jet-induced
SN models
(Christlieb et al. 2002)
High E 
High Co/Fe

Fallback 
Small Fe
Co
Dark Hypernova
Tominaga et al. 2007
Mega Metal-Poor Star : [Fe/H] < -7.1
[X/H]
C
Mg
Ca
Fe
pre-SN hot CNO cycle  Ca (M > 60 M) (Keller+14)
[Fe/H]
< -7.1
40Ca
Explosive O b. &
Incomplete Si-b.
 Ca
Mixing & Fallback

M(BH) ~ 5.6 M
(Ishigaki + 14)
First stars --Metal-poor stars -- GRB
connection
Hypernovae with relativistic jets
Mms ~ 20 – 130 M
Larger
.
GRBs
Metal-Poor stars
GRB-HNe
EMP stars
No-SN GRBs
UMP stars
HMP stars
Edep
Smaller
Hypernova Nucleosynthesis
• Central Engine ??
Outflow from Disk ? (McLaughlin +)
Magnetar ?
Materials in Jets: Ye ?
r-process elements ?
Correlation with
Fe-peak elements
(Zn, Co) ?

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