SLIDE 1
The Final Fates of The Final Fates of Massive Stars Massive Stars
- K. Nomoto (IPMU, U. Tokyo)
Evolution of Stars
SNIa SNII/Ib
The Final Fates of The Final Fates of Massive Stars Massive Stars - - PowerPoint PPT Presentation
The Final Fates of The Final Fates of Massive Stars Massive Stars - - PowerPoint PPT Presentation
The Final Fates of The Final Fates of Massive Stars Massive Stars K. Nomoto (IPMU, U. Tokyo) SNII/Ib Evolution of Stars SNIa The Final Fates of Single Stars M < 0.08 M Brown Dwarf 0.08 -- 0.46 M He White Dwarf 0.46
SLIDE 2
SLIDE 3
The Final Fates of Single Stars
- M < 0.08 M
Brown Dwarf
- 0.08 -- 0.46 M
He White Dwarf
- 0.46 -- 8 M
C+O White Dwarf
- 8 M -- Mup
O+Ne+Mg WD
- Mup -- 10 M
ONeMg–cc-SN + NS
- 10 M -- Mns
Fe-cc-Supernova + NS
- Mns -- 140 M
Fe-cc-Supernova + BH
- 140 -- 300 M
Pair Instability SN
- 300 -- 105 M
SN + BH
- 105 M < M BH(H)
SLIDE 4
SLIDE 5
Supernova Observations
Distant SNe & Nearby SNe
- Photometry Light Curve (UBVRIJHK)
- Spectra (HDS, FOCAS, IRCS, OHS)
Circumstellar Matter : ToO Early phase : ToO Nebular phase
- Polarization
- SN Properties (Mass, Energy, Abundance,
Distribution, Shape)
- Connections to:
Progenitors; GRBs; Metal-Poor Stars
SLIDE 6
GRB 030329 / SN 2003dh
Hjorth et al (2003) Stanek et al (2003) ;
SLIDE 7
Ia Ic Ib 94I 97ef 98bw
He Ca O SiII
Hyper
- novae
Early Spectra of Supernovae & Hypernovae
Hypernovae： broad features blended lines “Large mass at high velocities” I c: no H, no strong He, no strong Si
Patat et al. (1999)
SLIDE 8
- 19
- 18.5
- 18
- 17.5
- 17
- 16.5
- 16
- 15.5
- 15
5 10 15 20 25 30 35 40 Bolometric Magnitude Days since GRB/XRF explosion
SN1994I SN2006aj SN2003lw SN1997ef SN2002ap SN2003dh SN1998bw
GRB-SN
SLIDE 9
56Co-decay
SLIDE 10
Parameters [ Mej , E, M( 56Ni)]
Si C+ O He H-rich MC+ O Fe Collapse
56Ni 56Co ５６Fe
Mms / M MC+ O / M ~ 40 13.8 ~ 35 11.0 ~ 22 5.0
Light Curve Spectra
τ ~ [ τdyn • τdiffusion ] 1/ 2
~
- R
V R c κ Mej
1/ 2
∝ κ½ Mej
¾ E -¼
E ∝ Mej
3
E ∝ Mej
CO Star Models for SNe Ic
５６Ni
SLIDE 11
Spectral Fitting: SN1997ef
Normal SN (E51=1) Small Mej Hypernova (E51=20) Large Mej at High Vel. Too Narrow Features Broad Features
Iwamoto et al. (2000)
E51=E/1051 erg
SLIDE 12
GRB-Supernovae
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
SLIDE 13
Main sequence mass vs. Kinetic energy
SLIDE 14
Main sequence mass vs. 56Ni mass
SLIDE 15
Hypernova in Prague
SLIDE 16
Hypernova in Prague
SLIDE 17
Nebular Spectra of SNe Ibc
15 SNe Ibc. Previously, only 3!
Subaru, 8 m FOCAS Maeda et al. (2008: Science)
SLIDE 18
Late-Time Spectroscopic Data
- Asphericity is COMMON to core-collapse SNe!
Double-Peaks！ [OI] emission line
SLIDE 19
Fe (56Ni) O
“Single-peak” “Double-peak” “Single-peak” “Single-peak”
[OI] 6300
SN = Point source
Geometry
Doppler shift
@ ~ 1 year
λ
O
10/20
Bipolar vs. Spherical: How distinguished?
SLIDE 20
SN-GRB Connection
GRB-HN Magnetar Non-SN GRB
SLIDE 21
SUBARU/OHS observations of SNe Ia 05W, 03du, 03hv
Motohara et al. (2006)
Fe: Flat top! Blue shift!
Fe Fe
SLIDE 22
Main sequence mass vs. 56Ni mass
SLIDE 23
Faint Supernovae - EMP Stars
Fallback: small M(Ni) large [CNO/Fe] CEMP (1) Jet-like Energetic Explosion Zn, Co enhanced (2) Weak Explosion Mixing & Fallback
SLIDE 24
Faint SN 2008ha: Spectra(narrow)
Foley et al. (2009) Filippenko (1997) SN Ia SN I 2008ha (v ~ 700 km/s)
SLIDE 25
- 1
1 2 3 4 5 B N F Na Al P Cl K Sc V Mn Co Cu Ga C O Ne Mg Si S Ar Ca Ti Cr Fe Ni Zn
HE1327-2326 [Fe/H]=-5.5
- 1
1 2 3 4 5 5 10 15 20 25 30 B N F Na Al P Cl K Sc V Mn Co Cu Ga C O Ne Mg Si S Ar Ca Ti Cr Fe Ni Zn
Z [X/Fe] HE0107-5240 [Fe/H]=-5.3
Tominaga et al. 2007
Jet-induced SN models
HMP Stars
High E High Co/Fe
- Fallback
Small Fe
(Frebel et al. 2004) (Christlieb et al. 2002)
Dark Hypernova
SLIDE 26
Jet-induced Nucleosynthesis
Jet BH/NS BH
Edep : 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
40M 1.5x1052erg
SLIDE 27
Ca-rich EMP Star
(Lai et al. 2009)
SLIDE 28
EPM stars in dSph Sextans
- Low [Mg/Fe]
at [Fe/H] =-2.8 SN Ia ? SN II ? ~10 M ? ~25 M ?
(Aoki et al. 2009)
SLIDE 29
SN – GRB – EMP star Connections
- GRB-SNe = Hypernovae
- Faint SNe – EMP stars (CEMP, Zn, Co)
Weak SNe “Dark” Hypernovae Non-SN GRB
- Faint SNe -- Ca-rich SN
- - Ca-rich EMP
- dSph low Mg/Fe
Diversity in SN properties:
- ONeMg (AGB)-SN --- SN 2008S (faint IIn)
- Most Luminous SN 2006gy (Kawabata’s poster)
SLIDE 30
8 – 10 M Stars
Super AGB Stars (1.07 M < Mcore < MCh) degenerate ONeMg core
- 8 M < M < Mup
ONeMg White Dwarfs Mup ~ 9 M ( Z )
- Mup < M < 10 M (Mcore ~ MCh)
ONeMg Core Collapse SN II due to Electron Capture
SLIDE 31
Electron Capture in ONeMg Core
- 24Mg(e-,ν)24Na
(e-,ν)24Ne
ρ>4.0×109gcm-3
- →collapse
SLIDE 32
Most Luminous Supernova 2006gy
32 Probing Stellar Populations out to the Distant Universe
SN 1998bw M(56Ni)=0.4M M(56Ni)=20M!? SN 2006gy (R) 2 arcsec Subaru R band (394day) Mirror image subtracted Kawabata, Tanaka, et al. (ApJ 2009; also Poster )
Also Agnoletto et al. (08)
SLIDE 33
SN2006gy vs PISN
PISN
SLIDE 34
Diversity & Peculiarities of Supernovae
- vs. Progenitors, Mechanisms