Diversity of Supernova-Hypernova Properties K. Nomoto (IPMU, U. Tokyo)
Diversity & Peculiarities of Supernovae • Ultra-Luminous SNe (IIn, II-L, Ic) Pair Instability ? Core-Collapse ? GRB ? CSM Interaction ? • Ultra-Faint SNe (IIn, Ic): SN Impostor ? (peculiar) SN Ia ? Super AGB ? Fallback SN ? non-SN GRB ? • GRB-SN : • Magnetar ?
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 -- M up O+Ne+Mg WD • M up -- 10 M ONeMg–cc-SN + NS • 10 M -- M ns Fe-cc-Supernova + NS • M ns -- 140 M Fe-cc-Supernova + BH • 140 -- 300 M Pair Instability SN • 300 -- 10 5 M SN + BH • 10 5 M < M BH(H)
(I) 8 – 10 M Stars Super AGB Stars (1.07 M < M core < M Ch ) degenerate ONeMg core • 8 M < M < M up ONeMg White Dwarfs M up ~ 9 M ( Z ) • M up < M < 10 M (M core ~ M Ch ) ONeMg Core Collapse SNe II due to Electron Capture Nomoto 1984
Electron Capture in 8-10 M Stars • 24 Mg(e - , ν ) 24 Na (e - , ν ) 24 Ne ρ >4.0 × 10 9 gcm -3 • → collapse Accretion-Induced Collapse of a WD ?
Presupernova Density Structure Density Nomoto- Umeda et al.- Steep Density Gradient
9M Star Neutrino Heating Weak Explosion Steep Density Gradient E exp =1 10 50 erg M ej =0.014 M Nucleosynthesis M （ 56 Ni)=0.002-0.003M Kitaura, Janka, & Hillebrandt (2006)
56 Co-decay
Faint SNe IIn: SN 2008S, NGC300-OT (Della Valle et al. 08; Pastorelle 08; Botticella et al. 09) -14 Progenitor = Super AGB star ? (Prieto et al. 08,09 Thompson et al. 08) SN Impostor ? (Smith et al. 09 Bond et al. 09 Berger et al. 09) Botticellar et al. 2009
(II) M > 10 M : Fe Core Collapse (20 M ; z=0.02 ) Ohkubo et al.
SNe II-P Plateau (Smartt 08) M( 56 Ni) Radioactive tail
M ( 56 Ni) – Main Sequence Mass (Smartt 2008)
Faint Supernovae SN 2008ha (I ?) 2005cz (Ib) (Kawabata+) 2005E (Ib) (Peretz+) 2008S (IIn) （ Kawabata et al. 2010 Nature in press)
Faint SN 2008ha: Spectra(narrow) SN I 2008ha SN Ia Filippenko (1997) Foley et al. (2009)
Fallback model for SN 2008ha - CO star core-collapse model (13 M 2.7 M ) Moriya et al.
Fallback in Jet-induced Explosion Jet Jet BH/NS BH (Tominaga et al. 2007) Maeda et al. cf. “Collapsar” (e.g., MacFadyen et al. 01) Mazzali et al. Modjaz et al. Magnetorotational Supernovae (e.g., Moiseenko et al. 06) . [OI] 6300A (SUBARU E dep : Energy deposition rate (Rotation, B etc.) Same mass and explosion energy 1.5x10 52 erg 40 M
Dark Hypernova non-SN GRB GRB 060614 Della Valle et al. 2006 Fynbo et al. 2006 Gal-Yam et al. 2006
GRB 030329 / GRB 030329 / SN SN 2003dh 2003dh Stanek et al (2003) ; Hjorth et al (2003)
Spectra of Supernovae & Hypernovae I c : no H, no strong He, SiII Ia no strong Si O Ca He Ib Hypernovae ： broad features Ic 94I blended lines 97ef Hyper “ Large mass at -novae 98bw high velocities” Patat et al. (1999)
GRB-SN SN2003dh SN2003lw SN1998bw SN2006aj SN1997ef SN2002ap SN1994I
GRB-Supernovae Three GRB － SNe = all Type Ic Hypernovae E > 10 52 erg ( ～ 10 × normal SN) Large M ms →Black Hole Forming SNe Aspherical E/10 51 erg M( 56 Ni)/M GRB SN M CO /M M ms /M 980425 1998bw 14 40 30 0.4 030329 2003dh 11 35 40 0.35 031203 2003lw 16 45 60 0.55
M( 56 Ni) - M(main Seq) 23
Hypernova in Prague
Hypernova in Prague
Non-GRB, peculiar SN Ib 2005bf SN2005bf MAGNUM (U. Tokyo)
Anupama et al. (2005) SN Ib 2005bf Tominaga et al. (2005) Folatelli et al. (2006) Double Peaks M( 56 Ni) =0.07 M : 1 st =0.3 M : 2 nd
SN 2005bf: Light Curve @ Late Phases SUBARU obs M( 56 Ni) < 0.07 M Maeda et al. (astro-ph/0705.2713) (ApJ 2007 Sep)
1 st peak: 56 Ni decay 2 nd peak: Magnetized Pulsar ? L=L 0 (t/t 0 ) β L 0 =8x10 43 erg/s(*) T 0 =60day β = -4 (n = 2) (*) If dipole, e.g., B 0 ~10 15 G, P 0 ~10 ms Maeda et al. (astro-ph/0705.2713) (ApJ 2007 Sep)
SN 2005bf: Unipolar Explosion ? (NS kick ?) Maeda, et al. ApJ 2007
Spectropolarimetry with Subaru VLT Subaru 31 Tanaka et al. 2009
SN 2005bf Polarization Large asymmetry Nebular spectra Unipolar? 2 nd Peak Magnetic power? 32 Tanaka et al. 2009
Brightest Hypernova: 1999as @z=0.127 ( Knop et al.) E ~ 3 × 10 52 erg mag M ms ~ 60M M CO ~ 20M M( 56 Ni) ~ 5.4M (Deng et al. ) SN 1999as
Extremely Luminous SNe SN Ic 2007bi (Pair-Instability?) M( 56 Ni) ~ 5 M (SN 1987A x 70) Gal-Yam et al. 2009
Massive Star Origin ? Pop III : Mass Accretion ? (e.g. Ohkubo+ 2009) M ~ 40 - 140 M M ~ 140 – 300 M M > 300 M (dM/dt ??) Stellar Mergers in Dense Star Clusters? (e.g., Ebisuzaki+)
Pop III Stars: Mass Accretion Pair-Instability (140-300 M ) or Core-Collapse Accretion Final Mass 1 M Ohkubo et al. (2009)
Pop III Stars: Mass Accretion Core Collapse (40-140 M ) LSN & GRB ? Accretion Final Mass 1 M Ohkubo et al. (2009)
Core-Collapse E 51 = 30 E 51 = 100 SN Models 56 Ni 56 Ni M = Log (Mass 50M Fraction) Mr E 51 = 30 E 51 = 100 Log (Mass M = Fraction) 56 Ni 56 Ni 100M Mr Umeda & Nomoto Mr
Models for Luminous SNe Core-Collapse PISN • M (ms) = 100 M 270 M • M (C+O core) = 43 M 121 M • M (ejecta) = 39 M 121 M • E (kin) = 3.3 E52 erg 7E52 erg • M (56Ni) = 6.1 M 9.8 M • LC: rise time = 52 - 85 days 150 days • Jet-induced Explosion Aspherical Hypernova GRB?
PISN vs. Core-Collapse : SN Ic 2007bi, SN IIn 2006gy Moriya et al.
SN Ibc 2007bi (core-collapse Hypernova) Moriya et al.
Photospheric Velocity (SN 2007bi) Moriya et al.
Extremely Luminous Supernovae Pair Instability SN ? Core-Collapse Hypernovae (Pop III GRB?) Circumstellar Interaction ? Mass loss ? Mass Accretion ? Stellar Mergers ? Extremely Faint Supernovae Fallback SN ? Low Mass SN? non-SN GRB & Metal Poor Stars
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