FOE, Raleigh, May 13. SN Progenitors:
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1 FOE, Raleigh, May 13 SN Progenitors: Evolution and Uncertainties Raphael HIRSCHI in collaboration with: SHYNE Keele: C. Georgy, N. Nishimura, S. Jones, M. Bennett (Keele, UK) GVA code: G. Meynet, A. Maeder, S. Ekström (Geneva, CH) and C. Chiappini (IAP, D) VMS: P. Crowther (Sheffield), O. Schnurr (IAP), N. Yusof, H. Kassim (UM, KL, Malaysia) MESA: B. Paxton (KITP), F. X. Timmes, Arizona (US) SNe: K. Nomoto (IPMU, J), T. Fischer (TUD, D) Nucleo: F.-K. Thielemann, U. Frischknecht, M. Pignatari (Basel, CH), T. Rauscher (Herts, UK) NUGRID: F. Herwig (Victoria, Canada), C. Fryer (LANL), UChicago, UFrankfurt,...
2 Recent Papers/Reviews - West, Heger, Austin, The Impact of Helium-burning Reaction Rates on Massive Star Evolution and Nucleosynthesis, 2013ApJ W (see also Tur et al 2010ApJ T, Tur etal 2009ApJ T) - Chieffi, Limongi, Pre-supernova Evolution of Rotating Solar Metallicity Stars in the Mass Range M and their Explosive Yields, 2012ApJS L - Takahashi, Umeda, Yoshida, Evolution of progenitors for electron capture supernovae, ApJ subm., 2013arXiv T Reviews: - Umeda, Yoshida and Takahashi, Massive Star Evolution and Nucleosynthesis -Lower End of Fe-Core Collapse Supernova Progenitors and Remnant Neutron Star Mass Distribution, 2012arXiv U, Accepted for publication in Progress of Theoretical and Experimental Physics - Langer, Pre-Supernova Evolution of Massive Single and Binary Stars, ARAA, 2012, astroph Maeder and Meynet, Rotating massive stars: From first stars to gamma ray bursts, 2012RvMP M - Woosley, Heger and Weaver, The evolution and explosion of massive stars, 2002RvMP W
3 Plan - Introduction - Stellar evolution model ingredients Code comp. - Most massive stars PCSN (PISN) - Least-massive massive stars ECSN - Super-desktops - Conclusions & Outlook
4 Massive Stars Massive stars: M > 8.8 M Main sequence: hydrogen burning WR After Main Sequence: LBV BSG RSG MS Helium burning Supergiant stage (red or blue) Wolf-Rayet (WR): M > 20 M WR without RSG: M > 40 M Advanced stages: carbon, neon, oxygen, silicon burning iron core Core collapse bounce supernova explosion 4 Raphael Hirschi Keele University (UK)
5 Supernova Explosion Types Massive stars: SN II (H envelope), Ib (no H), Ic (no H & He) WR White dwarfs (WD): in binary systems Accretion Chandrasekhar mass SN Ia (Turatto 03)
6 Supernova Explosion Types Massive stars: SN II (H envelope), Ib (no H), Ic (no H & He) WR ECSN? White dwarfs (WD): in binary systems Accretion Chandrasekhar mass SN Ia GRB PCSN? (=PISN) (Turatto 03)
7 Geneva Stellar Evolution Code 1.5D hydrostatic code (Eggenberger et al 2008) Rotation: (Maeder & Meynet 2008) Ω Centrifugal force: KEY FOR GRB prog. Mass loss: enhanced and anisotropic Mixing: meridional circ. & shear Mass loss dep. on Z & Ω Convection: Schwarzschild HP Large nuclear reaction network: rates from NACRE/reaclib s process ( isotopes)! B-fields (Spruit 02, Maeder 05) Frischknecht et al 2010, 2011 Models ZAMS until Silicon burning Ekstroem et al 11, Georgy et al 12, 13, Groh et al 13, Yusof et al 13 Meynet & Maeder 2000
8 Mass loss Mass loss prescriptions: O-type & LBV stars (bi-stab.): Vink et al 2000, 2001 and RSG de Jager et al 1988 WR stars (clumping effect): Nugis & Lamers 2000 M Z = M Z o Z/Z o - α = (Kudritzki & Puls 00, Ku02) (Nugis & Lamers, Evans et al 05) - α = (Vink et al 00,01,05) Z(LMC)~Z /2.3 => Mdot/1.5 Mdot/2 Z(SMC)~Z /7 => Mdot/2.6 - Mdot/5 Mass loss at low Z still possible? RSG (and LBV?): no Z-dep.; CNO? (Van Loon 05, Owocky et al) Mechanical mass loss critical rotation (e.g. Hirschi 2007, Ekstroem et al 2008, Yoon et al 2012)
9 Final stages & SN type Ratio SNIbc/SNII: tests final type Georgy et al 09 - THEORY: Georgy et al 09 (solid line) binaries: Eldridge etal 08 (dotted) - OBS: Prantzos & Boissier 03 (triangles) Prieto etal 08 (pentagons)
10 Code Comparison: GENEC MESA KEPLER Goal: determine code-related uncertainties (no ROT) PRELIMINARY results!! Jones et al (in prep)
11 Code Comparison: GENEC MESA KEPLER GENEC Conv. envelope He H C C He Ne O PRELIMINARY results!! Jones et al (in prep) Si
12 Code Comparison: GENEC MESA KEPLER MESA Conv. envelope He H He C Ne C O Si PRELIMINARY results!! Jones et al (in prep)
13 Code Comparison: GENEC MESA KEPLER KEPLER Conv. envelope He H He C Ne C O Si Differences in Si/Fe-cores due to complex series of convective shells PRELIMINARY results!! Jones et al (in prep)
14 Late Shell Mergers or Not? Tur et al 07/09/10 Results affected by C/Ne/O shell mergers need for 3D simulations
15 Code Comparison: GENEC MESA KEPLER (Enclosed mass within radius, r) Solid lines: end core Si-b. Dashed line: collapse (vc~-1000km/s) PRELIMINARY results!! Jones et al (in prep)
![(Crowther et al 10, MNRAS) 300 M Mr H H He He Age [Myr]](/docs-images/94/118224085/images/16-2.jpg "Log10(Time left until collapse) (Yusof et al 13 MNRAS,")
16 The Evolution of VMS VMS = Very Massive Stars: M > 100 M 20 M Minimax=320M!(Crowther et al 10, MNRAS) 300 M Mr H H He He Age [Myr] Log10(Time left until collapse) (Yusof et al 13 MNRAS, aph ) VMS: much larger convective core & mass loss!
17 Proximity to the Eddington Limit Solar Z: Time evolution: (Yusof et al 13 MNRAS, aph ) Stars never reach Edd = 1 strong Mdot Edd 1 just before collapse Possible LBV-type Mdot in WR stars?
18 The fate of VMS: PCSN/BH/CCSN? (Yusof et al 13 MNRAS, aph ) Zsolar: no PCSN (Rotating) models with Z<Z(LMC) lose less mass, and enter the PCSN instability region! BUT mass loss uncertain! PCSN range from Heger & Woosley (2002) MCO Mini Consistent with Langer et al (2007): PCSN for Z<Z /3 18 Raphael Hirschi Keele University (UK)
19 The fate of VMS: SNII/SNIb c? SN type: - SNIc at solar Z, - SNIb/c at Z(SMC) ~ ok for SN2007bi (Gal-Yam 2009 BUT see Dessart et al 12,13) - NO SNIIn predicted! ~ NOT ok for SN2006gy (e.g. Woosley et al 2007) (Yusof et al 13 MNRAS, aph )
20 The fate of Z=0 Yoon et al 2012 (see also Chatzopoulos, & Wheeler 2012 and Heger & Woosley 2012 Z= 0: Models including Mdot, rotation & B-fields Rotation lowers mass range for PISN Mechanical Mdot important Yoon et al 2012
21 ECSN progenitors & Super AGB Early evolution like AGBs; TP-phase core growth Dep. on Mdot mixing off-centre C-ignition Jones et al (in prep) ONeMg core Jones et al (in prep) Critical ONeMg core mass = Mcrit = ~1.375 (Miyaji et al. 1980; Nomoto 1984) See also: Miyaji (1980); Nomoto(1984, 1987); Miyaji & Nomoto (1987); Garcia-Berro, Ritossa and Iben (1990s); Eldridge & Tout (2004); L. Siess (2006, 2007, 2009, 2010), Poelarends (2008); Doherty et al. (2010)... See also Takahashi's talk
22 Can Massive Stars produce ECSN? 7-15 M models MESA stellar evolution code: Paxton et al M is a typical massive star: All burning stages ignited centrally. Fate: Fe-CCSN Jones et al, 13, ApJ subm; see also Mueller et al 12, Umeda et al 12
23 Can Massive Stars produce ECSN? 9.5 M still a massive star: Jones et al (in prep) Ne-Si burning stages ignited off-centre. Fate: still Fe-CCSN
24 Can Massive Stars produce ECSN? 8.8 M failed massive star: Jones et al (in prep) See also Nomoto 84: case 2.6 Timmes et al 92,94 Eldridge & Tout 04 Ne-b. starts off-centre but does not reach the centre. MESA Oxygen deflagration Agile-Bolztran for collapse + explosion Fischer et al (in prep) Fate: ECSN
25 Fate of Least Massive MS: ECSN/Fe CCSN? Fe-CCSN ECSN Both SAGB and failed massive stars may produce ECSN See also Takahashi's talk
26 Pre SN Luminosities Lowest-mass massive stars LESS luminous than SAGB/ failed massive stars no dredge-up/out Jones et al (in prep) & Eldridge & Tout 04
27 Weak interaction rates Current rate tables (Oda et al 1994) are far too sparse!! NEED: well sampled, Coulomb corrected EC+beta-decay rates For sd-shell nuclei 27 Raphael Hirschi Keele University (UK)
28 Mass Loss Uncertainties Fate of 8.7 Mo model High/low 3rd dredge-up efficiency, respectively Jones et al (in prog.) Hard to produce ECSN with Bloecker Mdot!
29 Super Desktops Norwegian HPC company FROM: distributed memory clusters TO: scalable shared memory clusters For the same cost! Super-desktop: single OS, 288 CPUs, RAM 576 GB Large scale: better balance between shared/distributed memory
30 Conclusions - Very massive stars found in NGC3603 & R136: M up to 320 Mo!! PCSN~Zo would be SNIb/c, not SNII! SN2007bi ok; SN2006gy X - Rotation Strong mixing between He & H-burning zones * Lowers minimum mass for PCSN, key for GRBs/magnetars * Large s process, primary 14N,13C prod. over entire Z range - ECSN: progenitor mass range study underway and promising Failed massive star = additional channel to ECSN - Major uncertainties: mass loss (LBV, RSG, AGB), magnetic fields, weak rates and convective boundary mixing 30 Raphael Hirschi Keele University (UK)
31 Keele is Not Kiel (Germany) But Where is it? West Midlands: Keele Keele area is famous for pottery: Wedgwood,... and football: Stoke city fc in premier league
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