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(Informal) workshop - Ferrara April 2004

(Informal) workshop - Ferrara April 2004. SNe. He-detonation. C - deflagration. C-delayed detonation. Induced Core collapse (nuclear runaway fails ). Pair instability, core collapse & O explosion (core collapse fails). Astrophysical (natural) Explosive Devices. Thermonuclear SNe.

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(Informal) workshop - Ferrara April 2004

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  1. (Informal) workshop - Ferrara April 2004 SNe

  2. He-detonation C-deflagration C-delayed detonation Induced Core collapse (nuclear runaway fails) Pair instability, core collapse & O explosion (core collapse fails) Astrophysical (natural) Explosive Devices Thermonuclear SNe Gravitational collapse

  3. II p Type II H Core collapse of massive stars II L SNe I b (strong He) I c (weak He) No H Type I Thermonuclear explosion I a (strong Si) based on spectra and light curves morphologies SNe Classification

  4. Riess et al. , 1997 Brighter Slower Decline Dimmer Faster Decline Type Ia light curve standard candles visible up to z ~ 1

  5. High-z Team (Brian Schmidt & co) DL • Supernova Cosmology Project (Saul Perlmutter & co.) 0.25 mag fainter than for an EMPTY Universe Fainter  Further z The Universe is Accelerating

  6. Type IIp light curve: potentialstandard candles up to z ~ 5 (with NGST)

  7. Non-degenerate log P r4/3 relativistic M2 M1 r5/3 Non-relativistic log r The virial theorem: stellar core evolution Collapse or ignition

  8. M<0.8 M¤ 0.8<M/M¤<8 8<M/M¤<11 11<M/M¤<100 M>100 M¤ t>1/HO 15 Gyr<t<30 Myr 0.5<Mf /M¤<1.1 CO WD t.10-30 Myr Mf =1.2-1.3 M¤ ONeMg WD t.1-10 Myr Mf =1.2-2.5 M¤ Fe (Ye.0.45) collapse NS or BH t#1Myr O (pair jnstability) (Ye=0.5) may or may not explode Stellar evolution

  9. He-burning: the competition between 3a->12C and 12C+a->16O+g 5 M Z=0.02 Y=0.28 4He 12C 16O

  10. Jp Ex (keV) ECM (keV) 10957 0- 10367 4+ 3195 2685 2+ 9847 9580 1- 2418 8872 2- Q = 7.162 MeV Gamow peack energies 7117 1- 12C+4He 6917 2+ -45 -245 6130 3- 0+ 6049 0 0+ Not an error bar 16O level scheme Na<s,v> (10-15 cm3mol-1s-1) for T9=0.2

  11. Carbon left in the core 0.8M < M < 25M (from Imbriani et al. 2001). Core Collapse CO WD ONeMgWD High rate – empty circle Low rate - Black circle 1 Hp overshoot – triangle Breathing pulses - square

  12. Supernovae Ia • Bright • Homogeneous • No evolutionary effects Thermonuclear Explosion of a CO WD M~MChandrasekhar Light Curve L 56Ni 56Co 56 Fe ~ 1.4 M time L  MNi

  13. RG MS H accreting WDsSingle Degenerate system: WD+RG Roche lobe overflow a) GWR: ang. momentum loss Merging scenario:Double Degenerate system: CO+CO b) secondary tidal disruption c) accretion 10-5 Myr-1

  14. High rate 12C(a,g)16O Low rate White Dwarf interior: C and O profiles

  15. 12C(a,n)16O and the final mass of 56Ni DM(56Ni)=10%

  16. Rate HIGH LOW MV -19.21 -19.30 Rise time 18.0 d 15.3 d from Dominguez, Hoflich, Straniero 2002 HIGH RateC/O  Observed: 18± 0.4 d

  17. g e-,e+ n,n n,n g e- Massive stars from Limongi, Chieffi & Straniero 2001

  18. Degenerate electrons Thermal contribution Pressure contributions

  19. At the onset of the core collapse • e-+p à n+ne (10 MeV) • 56Fe+g à 13a+4n (124 MeV)

  20. 1051 erg lost each 0.1 Mo hard core (1014 g/cm3) +0.2 ms +2.0 ms -0.5 ms 1012 g/cm3 3x1014 g/cm3 COLLAPSE, BOUNCE & STALL subsonic | supersonic

  21. Ye and 12C(a,g)16O Low rate (solid) High rate (dotted) from Imbriani et al. 2001

  22. M-R relation:high rate = shorter C burning = more compact progenitor

  23. Observable consequences: SN yields

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