The First Stars and Hypernovae The First Stars and Hypernovae

K. Nomoto (Univ. of Tokyo)

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

• 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

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

Mn

Co Cr

Zn

trend

McWilliam, Ryan, Spite,

[Fe/H] [Fe/H]

C-rich EMP Stars

Aoki et al. (2002)-4 -3 -2 -1 0

[Fe/H]

[C/F

e]

2

1

0

-1

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?

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

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

56Co decay

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

Spectral Fitting: SN1997ef

Normal SN

E51=1

MCO = 6M

Hypernova

E51=20,

MCO = 11M

Too Narrow Features

Broad Features

Iwamoto et al. 2000

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

SN 2003dh SN 2003dh GRB/SN ConnectionGRB/SN Connection

SN 2003dh : Early spectra

Hjorth et al (2003)

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.

Mej=8ME=3.8×1052ergs M(56Ni)=0.35M

Bolometric Light Curves

COMDH

SN 1998bw

SN 2003dh

Mazzali et al (2003)

SN 1997efSN 2002ap

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

Supernovae/HypernovaeNomoto et al. (2003)

Failed SN?

13M~15M

EK

M(56Ni)/M Nomoto et al. (2003)

[/Fe] 0≫

Hydrodynamics

Collimated jets (Z) + Bow shock (All direction)

M Lateral expansion

Radial Velocity/c

R/1010cm

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

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

Low 　 Energy ｖｓ High Energy Explosion

56Ni56Ni

28Si28Si 16O16O

15M, E51=1

25M, E51=30(Hypernova)

Mn

Co Cr

Zn

UN2003

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)

Type Ia/IIn SN2002ic

(Kotak et al. 2003)

Discovery of H-lines in SN Ia 2002ic

Hamuy et al(2003)

SN2002ic: ~222d(Subaru)

―― SN2002ic

―― SN1997cy(IIn)

―― SN1999E(IIn)

SN2002ic: Bolometric Light Curve

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)

Result(I)-Light Curve

• Density 0=2.5e-14g/cm3

• Index n=1.8

(Suzuki et al. 2003)

Origin of H-rich CSM

Binary

Single AGB Star

→SN I1/2

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

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