The Evolution and Explosion of Mass-Accreting Pop III Stars Ken Nomoto (IPMU / U.Tokyo)
Pop III Stars Pop III GRBs Pop III SNe? M > 10 5 M :SMS (Super Massive Stars) GR instability Collapse M ~ 300-10 5 M : Collapse (& Explosion ) IMBH SMBH? Pop III GRBs? M ~ 140-300M : Pair Instability SNe Complete Disruption M ~ 8-140M : Core Collapse Pop III GRBs, Hypernovae SNe II
Unusual SNe --Pop III SNe? Luminous SNe (IIn, II-L, Ic) (-23 mag) Pair Instability? Core-Collapse? GRB? CSM Interaction? Faint SNe (IIn, Ic) (-14 mag) SN Impostor? Super AGB? Fallback SN? non-sn GRB?
Formation of Pop III.1 Stars Dark Matter Halo (~10 6 M, z ~ 20) Primordial Cloud (~10 4 M ) H 2 formation and cooling Collapsing Core (~10 3 M ) Static Proto-Star (~0.01 M ) Mass-Accretion Stellar Evolution, Explosion
M J ~1000 M ~0.01 M Yoshida et al. Bromm et al. Abel et al. O Shea & Norman
Accretion onto Protostar First Star 4 K
(McKee et al.) Pop III.1 & Pop III.2 Pop III.1 Gas of primordial composition Initial conditions: purely cosmological Pop III.2 Gas of primordial composition Initial conditions modified by radiative and kinetic feedback from a Pop III.1 star, but not chemical feedback
Formation of Pop III.2 Stars Dark Matter Halo Primordial, reionized cloud H 2 & HD formation and line cooling Collapsing Core (~40 M ) Static Proto-Star Mass-Accretion Stellar Evolution, Explosion
Accretion Rates (Yoshida+ 08) (Poo III.2) (Pop III.1) Ohkubo, Nomoto et al. (09)
Accretion rates with stellar feedback
Accretion rates with stellar feedback McKee & Tan Ohkubo, Nomoto et al. (09)
Mass Accreting Pop III Stars Expansion Ohkubo, Nomoto, et al. (09)
Pop III Stars: Mass Accretion Pair-Instability (140-300 M ) or Core-Collapse Accretion Final Mass pp 3 α CNO 1 M Ohkubo et al. (2009)
Pop III Stars: Mass Accretion Core Collapse (40-140 M ) LSN & GRB? Accretion Final Mass pp 3 α CNO 1 M Ohkubo et al. (2009)
Final Fates of Accreting Pop III Stars Hypothetical Scenario: (dm/dt : uncertain) (stellar feedback) Pop III.1 M > 300 M Core Collapse M = 140-300 M PISN? M = 40 140 M?? Pop III.2 M < 50 M Core Collapse
Pop III GRBs? 915 M 40 M He Star (Suwa 2010)
Extremely Luminous SNe SN Ic 2007bi (Pair-Instability?) M( 56 Ni) ~ 5 M (SN 1987A x 70) Gal-Yam et al. 2009
SNe 2007bi, 2006gy Core-Collapse vs. PISN Core Collapse PISN PISN Core Collapse Rise time Moriya et al.
56 Co-decay
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 ( 56 Ni) = 6.1 M 9.8 M LC: Rise time = 52-85 days 150 days Jet-induced Explosion Aspherical Hypernova GRB?
Evolution of the 90M Star Oscillation Fe core collapse E 51 =30 M( 56 Ni)=5M (Umeda & Nomoto)
100-130 M : Nuclear Instability Woosley, Blinnikov, Heger (2007)
More Luminous SN 2005ap Quimby + (2009)
Interaction with Optically Thick Circumstellar Matter dm/dt=0.1 Ms/y Accreting matter In Pop III star? Moriya et al. (2010)
Pair Instability SN vs EMP stars Umeda & Nomoto 2002
Pop III.2: Core Collapse SN (20M, Z=0, E 51 =1 ) Tominaga, Umeda, Nomoto 07 (E51=1, M(Ni)=0.07) Heger & Woosley 08 (E51=1.2 mix S=4 piston) Limongi, Straniero, Chieffi 00 (E51=1, M(Ni)=0.1)
Poor Fit to Extremely Metal-Poor (EMP) Stars High Explosion Energy (Cayrel et al. 2004 )
SN II Yields ~ Metal Poor (MP Stars EPM Stars? Kobayashi, Umeda, Nomoto et al. 2006
[Co/Fe] [Cr/Fe] 0 0 Co Cr [Mn/Fe] -4 [Fe/H] -4 [Fe/H] 0 [Zn/Fe] 0 Mn Zn -4 [Fe/H] -4 [Fe/H] Cayrel et al. (2004)
Hypernova Nucleosynthesis (1) M(Complete Si-burning) (Zn, Co)/Fe (Mn, Cr)/Fe Fe/(O, Si) (2) More α rich entropy Zn/Fe 64 Ge Low energy High energy Ti/Fe (3) More O burns (Si, S, Ca)/O
Normal supernova vs. Hypernova 25M model Normal SN (E 51 =1) Hypernova (E 51 =10)
EMP stars vs. Hypernova (E 51 =10) Tominaga, Umeda, Nomoto (2006)
Hypernova in Prague
Hypernova in Prague
Hyper Metal-Poor (HMP) Stars [Fe/H] < -5 [C, N, O/ Fe] > 3 Christlieb, Frebel, Aoki, et al.
M=25M, E=7 10 50 erg (Weak Explosion) [Fe/H]=-5.3 Log X 0-1 58 Ni 56 Fe O He C H Ne C -2-3 Ti Mg O -4 M BH ~6M 2 4 6 8 Mr (M ) Fallback Ejecta (little Fe) Mixing Umeda & Nomoto (2003) N
Fallback model for SN 2008ha - CO star core-collapse model (13 M 2.7 M ) Moriya et al.
Jet-induced Nucleosynthesis Jet BH/NS Jet BH Special relativistic hydrodynamics (Tominaga et al. ApJL 2007) cf. Collapsar (e.g., MacFadyen et al. 01) Magnetorotational Supernovae (e.g., Moiseenko et al. 06). E dep : Energy deposition rate (Rotation, B etc.) Same mass and explosion energy 40M 1.5x10 52 erg
Mixing-fallback vs. Jet SN model High entropy due to the energy concentration. Mixing-fallback model Jet SN model
(Frebel et al. 2004) HMP Stars Jet-induced SN models (Christlieb et al. 2002) High E High Co/Fe Fallback Small Fe Dark Hypernova Tominaga et al. 2007
M( 56 Ni) Bright HN Smaller E dep. smaller M( 56 Ni) and larger [C/Fe] [C/Fe] Dark HN HMP stars UMP stars High E Fallback. CEMP stars EMP stars Tominaga et al. (2007) E dep
Dark Hypernova non-sn GRB GRB 060614 Della Valle et al. 2006 Fynbo et al. 2006 Gal-Yam et al. 2006
First stars --Metal-poor stars -- GRB connection Hypernovae with relativistic jets M ms ~ 20 130 M sun Larger. E dep Smaller GRBs GRB-HNe No-SN GRBs Metal-Poor stars EMP stars UMP stars HMP stars
Carbon-enhanced metal-poor DLA z = 2.34, [Fe/H] = -3.04, [C/Fe] = +1.53 (Cooke et al. 2010)
Carbon-enhanced metal-poor DLA z = 2.34, [Fe/H] = -3.04, [C/Fe] = +1.53 (Cooke et al. 2010) SN model : M = 25 M, E 51 = 1 (Kobayashi et al. 2011)
Faint Supernovae EMP (extremely metal-poor) Stars Fallback Supernovae: small M(Ni) large [CNO/Fe] CEMP (1) Jet-induced Hypernovae large [Zn/Fe], [Co/Fe], [Ti/Fe] (2) Weak Explosion Mixing & Fallback
Final Fates of Accreting Pop III Stars Hypothetical Scenario: (dm/dt : uncertain) (stellar feedback) Pop III.1 M > 300 M Core Collapse PISN? M = 40 140 M?? Pop III.2 M < 50 M Core Collapse *Extremely Luminous Supernovae: PISNe vs. Core-Collapse Hypernovae(GRB?) Circumstellar Interaction?