the first stars and hypernovae
DESCRIPTION
The First Stars and Hypernovae. K. Nomoto (Univ. of Tokyo). M > 10 5 M : SMS (Super Massive Stars) GR instability Collapse M ~ 300 - 10 5 M : VMO (Very Massive Objects) Nuclear Instability Pulsational Mass Loss M ~ 130 - 300M : Pair Creation Instability - PowerPoint PPT PresentationTRANSCRIPT
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The First Stars and Hypernovae The First Stars and Hypernovae
K. Nomoto (Univ. of Tokyo)
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M > 105M:SMS (Super Massive Stars) GR instability Collapse
M ~ 300 - 105M: VMO (Very Massive Objects) Nuclear Instability Pulsational Mass Loss
M ~ 130 -300M: Pair Creation Instability Collapse Nuclear Explosion
M ~ 8 -130M: Fe core Collapse
Hypernovae BH
SNe II NS
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• First Stars (Pop III Stars)
• First Supernovae (Type II, Ibc, Hypernovae, Pair)
• Early Cosmic Chemical Evolution– AGB Stars– Supernovae (Type Ia)
• Abundance Ratios @high z, low Z• EMP (Extremely Metal-Poor) Stars: Halo, dSph• DLA• ICM, …
-elements: [(O, Mg, Si, S, Ar, Ca)/Fe], [Si/O]– Fe-peak elements: [(Ti, Cr, Mn, Co, Ni, Zn)/Fe]– R-process, s-process elements
Cosmic Clock
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Galactic Chemical Evolution[Fe/H]=log(Fe/H) -log(Fe/H)
DiskHalo
Homogeneousenrichment
Fe
O,Ne,Mg....,
2.5
[Cr, Mn, Co/Fe]Inhomogenitiy for[Fe/H]<-2.5
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Mn
Co Cr
Zn
trend
McWilliam, Ryan, Spite,
[Fe/H] [Fe/H]
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C-rich EMP Stars
Aoki et al. (2002)-4 -3 -2 -1 0
[Fe/H]
[C/F
e]
2
1
0
-1
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First Generation Stars/Supernovaeand
Extremely Metal-Poor Stars• EMPs: [Fe/H] < -2.5
– Trends in [(Zn, Co, Mn, Cr)/Fe]– C, N-rich Stars
• Variation in C/Mg, Mg/Si, ...– HE0107-5240 (Christlieb et al.)
• Low mass star formation @[Fe/H]~ - 5.3?
• Core-Collapse Supernovae– Black Hole Formation M > 20-25M
Variations in Explosion energy Hypernovae Mixing & Fallback Faint SNe Jets, … Rotation? Binary?
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Ia
Ic
Ib
94I
97ef
98bw
HeCaO
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
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SNe Ic SNe IInSN GRB SN GRB
1998bw 980425 1997cy 970514
1997ef 971115 1999E 980910
1999as 1988Z
2002ap 1999eb 991002
2003dh 030329
1997dq
1998ey
1992ar
Hypernova CandidatesEkinetic > (5-10)×1051ergs
SN 1998bw
GRB 980425
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56Co decay
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Parameters [Mej, E, M(56Ni)]
Si
C+O
He
H-rich
MC+O
FeCollapse
56Ni
56Co
56
Fe
Mms/M MC+O/M
~ 40 13.8
~ 35 11.0
~ 22 5.0
Light Curve Spectra
~ [dyn • diffusion]1/2
~ • RV R c
Mej1/2
½Mej¾E -¼
E Mej3
E Mej
CO Star Models for SNeIc
56 Ni
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Spectral Fitting: SN1997ef
Normal SN
E51=1
MCO = 6M
Hypernova
E51=20,
MCO = 11M
Too Narrow Features
Broad Features
Iwamoto et al. 2000
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0 50 100 t (days)
98bw&CO138
94I &CO21
97ef&CO100
Radioactive Decay 56Ni 56Co 56Fe
C+O Star Models
98bw 97ef 94I
Mms
(M)
40 35 15
MC+O
(M)
13.8 10.0 2.1
EK
(1051erg)
30 20 1
M(56Ni)(M)
0.5 0.15 0.07
log L (erg/s)
43
42
41
Light curves of Hypernovae & SNeIc
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SN 2003dh SN 2003dh GRB/SN ConnectionGRB/SN Connection
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SN 2003dh : Early spectra
Hjorth et al (2003)
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Kawabata et al. (Subaru)
GRB 030329/SN 2003dh (36d)
IAU Circ. 8133
Similar to SN 1998bw at < ~ 30 days (Stanek et al.; Hjorth et al.)
to SN 1997ef at > ~ 30 days (Kawabata et al.)
Matheson et al.
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Mej=8ME=3.8×1052ergs M(56Ni)=0.35M
Bolometric Light Curves
COMDH
SN 1998bw
SN 2003dh
Mazzali et al (2003)
SN 1997efSN 2002ap
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SN 1997D:Ⅱ Faint SN 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
m-M=30.64 (NGC1536)
E~4×1050erg narrow lines
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Supernovae/HypernovaeNomoto et al. (2003)
Failed SN?
13M~15M
EK
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M(56Ni)/M Nomoto et al. (2003)
[/Fe] 0≫
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Hydrodynamics
Collimated jets (Z) + Bow shock (All direction)
M Lateral expansion
Radial Velocity/c
R/1010cm
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SNe in Binary SystemsSingle M1~M2
”Conservative”M1»M2
”Non-Conservative”
1 2 21
RSG
SNII
Spiral-in
He, C+O Star
SNIb/c
Wolf Rayet (WN, WC)
SNIb/c
Hypernovae?
?
Rapid Rotator
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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
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Low Energy vs High Energy Explosion
56Ni56Ni
28Si28Si 16O16O
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15M, E51=1
25M, E51=30(Hypernova)
Mn
Co Cr
Zn
UN2003
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First Supernovae and EMP stars
• EMPs: [Fe/H] < - 2.5– Trends in [(Zn, Co, Mn, Cr)/Fe]– C, N-rich Stars– HE0107-5240 (Christlieb et al.)
• Black-Hole Forming Supernovae
Variations in Explosion Energy Rotation
Mixing & Fallback Binarity
Jets, …
High Energy, Jets
Mixing & Fallback
(~25M - 130M)
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Type Ia/IIn SN2002ic
(Kotak et al. 2003)
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Discovery of H-lines in SN Ia 2002ic
Hamuy et al(2003)
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SN2002ic: ~222d(Subaru)
―― SN2002ic
―― SN1997cy(IIn)
―― SN1999E(IIn)
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SN2002ic: Bolometric Light Curve
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Circumstellar Interaction Model
• CSM= 0 *(R/R0) –n
H line
• Ejecta SNIa (W7)
• Contact Discontinuity R0=1e+15cm
=0 ~ 1-25e-15g/cm3
ejecta CSM
Reverseshock
Forwardshock
High T~107K
low T~109K
X-ray
Coolingshell
Reemitin Optical
(Chevalier & Fransson)
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Result(I)-Light Curve
• Density 0=2.5e-14g/cm3
• Index n=1.8
(Suzuki et al. 2003)
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Origin of H-rich CSM
Binary
Single AGB Star
→SN I1/2
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Circumstellar Medium of SN2002ic
• Mass ~2-3M
• M ~ 10-4M yr-1
• Aspherical
• Binary Scenario: Massive Companion → WD wind → SN Ia
• Single Star Scenario: AGB Star (Low Metallicity?) → Type I1/2
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First Supernovae
[Fe/H] : -5 -4 -3 -2.5 Faint SNe
Hypernovae Normal SNe
Black-Hole Forming Supernovae (20-130M)
⇒ First Black Hole > 2~6M
Faint SNe (High and Low energy) ⇒ C,O-rich ejecta ⇒ Efficient Cooling of ISM ⇒ Formation of Low Mass C,O-rich 2nd Generation Stars