Diversity of Supernova-Hypernova Properties K. Nomoto (IPMU, U. - PowerPoint PPT Presentation

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