Supernova-Hypernova

K. Nomoto (IPMU, U. Tokyo)

Diversity of

Properties

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 -- 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)

(I) 8 – 10 M StarsSuper AGB Stars (1.07 M < Mcore < MCh)

degenerate ONeMg core • 8 M < M < Mup

ONeMg White DwarfsMup ~ 9 M ( Z )

• Mup < M < 10 M (Mcore ~ MCh)ONeMg Core Collapse SNe II due to Electron Capture

Nomoto 1984

Electron Capture in 8-10 M Stars

• 24Mg(e-,ν)24Na(e-,ν)24Ne

� ρ>4.0×109gcm-3

• →collapse

Accretion-Induced Collapse of a WD ?

Presupernova Density StructureNomoto-Umeda et al.-

Density

Steep Density Gradient

9M StarNeutrino Heating Weak Explosion

Steep Density GradientEexp =11050 erg

Mej=0.014M

Nucleosynthesis

Kitaura, Janka, & Hillebrandt (2006)

M（56Ni)=0.002-0.003M

56Co-decay

Faint SNe IIn: SN 2008S, NGC300-OT(Della Valle et al. 08;Pastorelle 08;Botticella et al. 09)

Progenitor =Super AGB star ?

(Prieto et al. 08,09Thompson et al. 08)

SN Impostor ?(Smith et al. 09Bond et al. 09Berger et al. 09)

Botticellar et al. 2009

-14

(II) M > 10 M : Fe Core Collapse

(20 M; z=0.02)

Ohkubo et al.

SNe II-P (Smartt 08)

M(56Ni) Radioactive tail

Plateau

(Smartt 2008)

M (56Ni) – Main Sequence Mass

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)

Foley et al. (2009) Filippenko (1997)

SN Ia

SN I 2008ha

Fallback model for SN 2008ha- CO star core-collapse model

Moriya et al.

(13 M 2.7 M)

Fallback in Jet-induced ExplosionJet

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

(Tominaga et al. 2007)

Same mass and explosion energy40M 1.5x1052erg

Maeda et al.Mazzali et al.Modjaz et al.

[OI] 6300A (SUBARU

Della Valle et al. 2006

non-SN GRBGRB 060614

Fynbo et al. 2006Gal-Yam et al. 2006

Dark Hypernova

GRB 030329 / SN 2003dh

Hjorth et al (2003)Stanek et al (2003) ;

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

Patat et al. (1999)

SN1994I

SN2006aj

SN2003lw

SN1997efSN2002ap

SN2003dh

SN1998bw

GRB-SN

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

M(56Ni) - M(main Seq)

23

Hypernova in Prague

Hypernova in Prague

Non-GRB, peculiar SN Ib 2005bf

MAGNUM (U. Tokyo)SN2005bf

SN Ib 2005bfAnupama et al. (2005)Tominaga et al. (2005)Folatelli et al. (2006)

Double PeaksM(56Ni) =0.07 M : 1st

=0.3 M : 2nd

SN 2005bf: Light Curve @ Late Phases

Maeda et al. (astro-ph/0705.2713)(ApJ 2007 Sep)

SUBARU obs

M(56Ni) < 0.07 M

1st peak: 56Ni decay 2nd peak: Magnetized Pulsar ?

L=L0(t/t0)β

L0=8x1043erg/s(*)

T0=60day

β = -4 (n = 2)

(*) If dipole, e.g.,

B0~1015 G, P0~10 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

31Tanaka et al. 2009

SubaruVLT

SN 2005bf

32Tanaka et al. 2009

PolarizationLarge asymmetry

Nebular spectraUnipolar?

2nd PeakMagnetic power?

Brightest Hypernova: 1999as @z=0.127

E ~ 3×1052erg Mms ~ 60M

MCO ~ 20M

M(56Ni) ~ 5.4M

SN 1999as

mag

(Deng et al. )

(Knop et al.)

Extremely Luminous SNeSN Ic 2007bi (Pair-Instability?)

M(56Ni) ~ 5 M

Gal-Yam et al. 2009

(SN 1987A x 70)

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

Ohkubo et al. (2009)

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

M = 50M

M =100M

E51 = 30

E51 = 30

E51 = 100

E51 = 100

Umeda & Nomoto

56Ni 56Ni

56Ni56Ni

Log (Mass Fraction)

Log (Mass Fraction)

Mr

Mr Mr

Core-CollapseSN Models

• 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?

Models for Luminous SNeCore-Collapse PISN

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 SupernovaePair Instability SN ?Core-Collapse Hypernovae (Pop III GRB?)Circumstellar Interaction ?

Mass loss ?Mass Accretion ?Stellar Mergers ?

Fallback SN ? Low Mass SN?non-SN GRB & Metal Poor Stars

Extremely Faint Supernovae