Do we still need to search for supernovae ? Enrico Cappellaro Osservatorio Astronomico di Padova Istituto Nazionale di Astrofisica 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 Talk Outline • SN Ia are the best luminosity distance indicators on cosmological scale o for precision cosmology we need to understand SN Ia diversity • Stars with mass >8 M end their life as core collapse supernovae o stripped-envelope SNe and GRBs o progenitor mass and explosion outcome o mass loss history in massive stars 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 Basic SN classification max. +10 months Ia Ib II 52° Congresso SAIt Scenario 3 - 8 M Thermonuclear explosion of WD in binary system 30 - 60 M core-collapse of massive star after strong mass loss 8 - 40 M core-collapse of massive star after low/moderate mass loss Teramo, 4 - 8 Maggio 2008 Precision cosmology with SN Ia SNAP collaboration 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SN Ia, are they standard candles ? Δm15 1.5 mag 52° Congresso SAIt < 1.0 1.0 - 1.3 1.0 - 1.7 > 1.7 Teramo, 4 - 8 Maggio 2008 absolute magnitude SN Ia, are they standard candles ? -20 max Δm15 -18 15d -16 0 40 days from maximum 52° Congresso SAIt Altavilla et al. 2004 MNRAS 349, 1344 Teramo, 4 - 8 Maggio 2008 SN Ia, are they standard candles ? Prieto et al. 2006 ApJ 647, 501 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SN Ia explosion models: carbon deflagration in a C-O white dwarf (W7) Branch etal.1985 AGB Nomoto etal. 1984 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 Modeling SN Ia ejecta tomography Mazzali et al. 2008 MNRAS in press 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 Modeling SN Ia ejecta tomography 2004eo W7 Mazzali et al. 2008 MNRAS in press 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 stratification SN Ia diversity Benetti et al 2005 ApJ 623, 1001 Ni mass 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SN Ia diversity The orro mark vs m15(B) σ~0.13M + 54Fe & 58Ni σ~0.09M 56Ni outer vel NSE ≈ inner vel IME IME shell encloses ≥ 1.05±0.09 M irrespective of m15(B) ~0.09Msun ~0.13Msun less 56Ni corresponds to more IME for a similar total mass Mazzali et al. 2007 Science 315, 825 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SN Ia explosion models Ropke et al. 2007 Deflagration spots 5 20 800 M(NSE) 1.14 0.83 0.64 M(IME) 0.22 0.44 0.55 Weak deflagration leaves fuel at high density which is burned to NSE by detonation 52° Congresso SAIt Strong deflagration exhausts fuel and expands the star. Detonation at lower density makes IME Teramo, 4 - 8 Maggio 2008 Not the end of the story …. The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar mass white dwarf star (2 M) Howell et al 2006 Nature 433, 308 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SN Ia precursor scenarios single or double degenerate ? The collapse of a stripped-envelope massive star in a dense environment ? Benetti et al. 2006 ApJ 653, L129 SN2002ic: evidence for an asymptotic giant branch star in the progenitor system of a type Ia SN (Hamuy et al 2003 Nature 424, 651) 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SN Ia precursor scenarios single or double degenerate ? Patat et al. 2007, Science 317, 924 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SN Ia precursor scenarios single or double degenerate ? X-ray (Chandra) Roelofs etal 2008 astro-ph/0802-2097 2003 optical (HST) 2004 optical (SWIFT) X-ray X-ray luminosity consistent with typical super-soft source single degenerate, accreting progenitor model is favored optical offset: 1.18±0.27” SN2007on Voss & Nelemans 2008 Nature 451, 802 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SN Ia progenitor population Adopting SFR as in Hopkins & Beacon 2006 Botticella et al. 2008 A&A 479, 49 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SN Ia progenitor population Adopting SFR as in Hopkins & Beacon 2006 Botticella et al. 2008 A&A 479, 49 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SNe and GRBs Long GRBs are linked to highly energetic SN Ic SN 1998bw / GRB98042 SN 2003dh / GRB030329 SN 2003lw / GRB031203 1998bw 1994I 1998bw Galama et al 1998 Nature 395, 762 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SNe and GRBs There are high energy SN Ic without GRB SN1997ef SN 2002ap SN 2003jd SN 2004aw Mazzali et al 2005 Science 308, 1284 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SNe and GRBs Some long GRB do not show a SN GRB010921 GRB060614 No SN brighter than magV = -12.6 Gal-Yam et al 2006 Nature 44,1053 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SNe and GRBs GRB/XRF can be associated to normal SN Ib/c SN 2006jc / XRF060218 SN 2008D / XRF080109 20 dec 2001 16 oct 2004 A WR which had a LBV-like outburst 2 yr before core collapse Mazzali etal 21 sep 2006 52° Congresso SAIt submitted 20 oct 2006 Pastorello et al 2007 Nature 447, 829 Teramo, 4 - 8 Maggio 2008 SNII: H rich, core collapse progenitor M > 8MO kinetic energy ~1051 erg total energy ~1053 erg remnant neutron star After 1987A ejecta 1 - 30 MO composition O, Mg, Si, Ne, Ca age < 50 Myr Progenitor radius early light curve realization 100% Explosion energy 56Ni mass Mass loss history ejecta mass, CSM Asymmetries explosion mechanism 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 From core collapse to explosion …….. the mechanism for core collapse supernova explosions remains unknown. Nonetheless, one-, two-, and three-dimensional simulations performed thus far have shown that (1) neutrino transport, (2) fluid instabilities, (3)rotation, and (4) magnetic fields, together with proper treatments of (5) the sub- and super- nuclear density stellar core equation of state, (6) the neutrino interactions, and (7) gravity will be important. Mezzacappa, A. (2005) ASP Conference Series, Vol. 342, p.175 One of the outstanding problems in astrophysics is the mechanism of core-collapse supernova explosions. …..………………………. The potential roles as factors in explosion of neutrinos, the nuclear equation of state(EOS), exotic physics, general relativity, dimensionality, instabilities, magnetic fields, and rotation all continue to be topical. Burrows et. al. 2006 ApJ 640, 678 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SNII: H rich, core collapse 1 order of mag in envelope mass 5 mag 5 mag range at maximum Small spread in nebular phases MNI=0.07 M 1 order of mag in progenitor radius Turatto et al 1990 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 Faint core collapse SNe .. fallback of material onto the collapsed remnant of the explosion of a 25-40 M 0.3 > MNi > 0.002M Pastorello et al 2004 MNRAS 347 ,74 Turatto et al. 1998 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 Faint core collapse SNe The progenitor of SN 2005cs M = 9 ± 3 MSUN Maund et al. 2005 MNRAS 364, L33 M = 10 ± 3 MSUN Li et al. 2006 ApJ 641, 1060 M = 6-8 Msun Eldridge et al 2007 MNRAS 376, 52 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 SN II modelling 92am 98bw 69L 99em 04A 03gd 87A 05ay 97D 99br 05cs 01dc 03Z Iwamoto etal 2000 Zampieri 2007 AIPC 924, 358 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008 Very massive stars 1. Pair-instability SN, producing 15-20 Msun of Ni56 (Smith 2007 astro-ph/0710.3431) 2. Massive shell ejection due to pulsational pair instalibiliy (Woosley et al 2007 Nature 450,390 ApJL 671, 17) 3. High energy SN Ia in a dense shell (2002ic–like) (Oefk 2007 ApJ 659, 13) 4. Collision of two massive stars in a dense young cluster (Portegies & van den Heuvel 2007 Nature 450, 388) 5. Core collapse of a massive star within a 10 Msun shell ( η Carinae – like) (Smith & McCray 2007 ApJL 671, 17) Smith et al. 2008 astro-ph/0804.0042 52° Congresso SAIt 6. Quark nova astro-ph/0708.1787) (Leahy and Ouyed 2008 Teramo, 4 - 8 Maggio 2008 What next o Understanding the physics of SNIa to support future SNAP-JDEM mission: detailed observation and modeling of nearby SN Ia o What dictates the final fate of massive stars: observing and modeling the UV - optical – nearIR SN SED o Link SN progenitor to their parent population: measure the SN rates at high redshift (z>1) 52° Congresso SAIt Teramo, 4 - 8 Maggio 2008