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Part II: Jan Staff Part III: Brian Niebergal

Quark-Nova: Astrophysical Implications A primer on Compact Stars and Type II Super-novae A primer on Quark Stars and Quark-Novae Application to brightest Supernovae (SN 2006gy case) Application to Epoch of Reionization R. Ouyed (U. Calgary). Part II: Jan Staff

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Part II: Jan Staff Part III: Brian Niebergal

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  1. Quark-Nova:Astrophysical ImplicationsA primer on Compact Stars and Type II Super-novae A primer on Quark Stars and Quark-NovaeApplication to brightest Supernovae (SN 2006gy case)Application to Epoch of ReionizationR. Ouyed (U. Calgary) Part II: Jan Staff Part III: Brian Niebergal

  2. 0 Type II Supernovae(Core-collapse Supernovae) Mass > 8 Msun

  3. Core-Collapse Supernovae Hydrogen present when they explode!

  4. Mass-shedding Stars Black Holes Neutron Stars White Dwarfs May or may not have hydrogen when they explode!

  5. GRAVITY→ RADIATION !!! Energy release NS Grav. Energy (1053 erg) Kinetic Energy (1051 ergs) Radiation (1049 ergs) 1% 1%

  6. The Quark-Nova

  7. Compact Stars in the QCD Phase Diagram Hybrid stars Think of a Quark Star as a nucleon with ~1057 quarks. The quarks are still confined!

  8. u and d convert to s in order to reduce Pauli repulsion by increasing flavor degeneracy ? TG

  9. Upon reaching a critical density (~5 times nuclear density), the core of the neutron star converts rapidly into (u,d,s) quark matter

  10. Hybrid Stars (HS) Neutron Stars with Quark Cores Lead to Black Holes Heavy NSs (HS candidates) Lead to Neutron Stars

  11. Neutron star to Quark star Transition The QUARK-NOVA ! The quark matter core becomes unstable and shrinks faster than the envelope response time!

  12. Core collapse Neutrino & photon emission

  13. The KEY message to “explosive astrophysics” community: Quark Matter Photon Fireball !

  14. The KEY message to “explosive astrophysics” community: Quark Matter Photon Fireball ! CFL

  15. QN key ingredients Energy Reservoir (more than 1053 erg) Photon Fireball (up to 1052 ergs in K) Ultra-relativistic iron-rich ejectum Heavy-element-rich (A>130) ejecta + Massive Progenitor

  16. Quark Nova and Super-luminous Supernovae "This was a truly monstrous explosion, a hundred times more energetic than a typical supernova,"

  17. 1051 ergs in Radiation ! 100 times a normal Supernova !

  18. 3 Possible Mechanisms • (1) interaction of the supernova blast wave with circumstellar material (CSM) • (2) energy from radioactive decay of 56Ni • (3) Oscillating PISN Need too much surrounding Ejecta ! Need too much Nicke ! Very massive progenitor ! Artificial energy input!

  19. Standard picture stretched to the extreme ! Ekinetic = 6.4x1052 erg; Mejecta = 53Msun; M(Ni+CO) = 15Msun

  20. Neutron Star What does the Quark-Nova has to offer in this context? Dual Explosion! Quark Star Quark-Nova Ejecta

  21. Application SN2006gy Mejec = 40Msun Rstar = 10 Rsun 2000 < VSN (km/s) < 4800 tdelay = 15 days

  22. Find the first bump (the SN) before the second bump (the QN) A double-hump! Light-Curves of SN2005gj and SN2005ap Keep same parameters as for SN2006gy except SN2005gj tdelay = 10 days SN2005ap tdelay = 40 days

  23. Kawabata et al. 2009, ApJ The Nature of the Beast

  24. As the photosphere receeds deeper, one would start seeing heavy elements processed during the QN. These lines should look narrow since the QN ejecta is slowed down by interaction with the preceeding SN ejecta … The Photosphere

  25. OCCURRENCE RATE Lead to Black Holes Heavy NSs (QS candidates) Lead to Neutron Stars • Superluminous supernova are rare events: about 1 out of 1000 supernovae • Dual Shock quark novae are also estimated to occur for about 1 out of 1000 supernovae Follow-up talk by Jan Staff: implications to GRBs ……

  26. Quark-Novae and Reionization Era ? HII (Hydrogen “fully” ionized) ? HI z 9 8 7 6 5 4 3 2 1 0

  27. reionization The Source(s) of reionizatio? Fan et al. 2006 2 Key Constraints: WMAP: zstart= 20 (tau_e~0.11) WMAP: zend ~ 6 From Avi Loeb

  28. One is left with first stars!

  29. Loeb, Ostriker, Chiu, Fan, Venkatessan, Tegmark, Gnedini, Becker, Carilli, Ferrara, Gallerani, Jiang, Richards, Choudhury, Strauss, Xu, Walter, White ect… Pop III stars unlikely !

  30. 6 < z < 8 If GRBs are indeed quark-novae (see Staff’s talk) then high-z GRBs should cluster around z~6-8

  31. FIN … or is it may be just … the beginning

  32. or is it may be just … the beginning FIN …

  33. Takeaway message: Photon-driven (instead of traditional neutrino-driven) explosions Dual-explosions Dual-explosion

  34. Target or seed nuclei (neutron star crust) Neutrons v Collapsing core r-process nucleo-synthesis

  35. R-process Elements from the Quark Nova Light element (Ge, Ti) production by alpha-burning 195Pt 132Xe U island 79Se 44Ti 152Eu 73Ge Observations of Gamma-rays from 44Ti (half-life=90 years) could in principle confirm the Quark-Nova Scenario

  36. The Nature of the Beast Spectrum 2006gy Ia

  37. Hot SN ejecta cools slowly by adiabatic expansion QN inside a SN QN shock/chunks wave moves through entire Supernova ejecta SN ejecta becomes fully shocked by QN chunks Shocks/chunks breakout

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