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THE QUARK NOVA PROJECT I

Canadian Workshop on the Nuclear and Astrophysics of Stars . THE QUARK NOVA PROJECT I. Distinct Photometric and Chemical Evidence of the Quark Nova in SN2006gy. Friday, December 10 th 2010 Mathew Kostka – PhD Student Rachid Ouyed – Supervisor

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THE QUARK NOVA PROJECT I

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  1. Canadian Workshop on the Nuclear and Astrophysics of Stars. THE QUARK NOVA PROJECT I Distinct Photometric and Chemical Evidence of the Quark Nova in SN2006gy Friday, December 10th 2010 Mathew Kostka – PhD Student RachidOuyed – Supervisor NicoKoning, Denis Leahy, Wolfgang Steffen – Collaborators

  2. SN 2006gy

  3. SN 2006gy • Pulsational pair instability supernova • Extremely massive star (110 solar masses) • Two ejection events • Circum-stellar material interaction • 0.1 solar masses lost per year for 10 years • All kinetic energy transformed to radiation (Woosley et al. 2007) (Ofek et al. 2007; Smith et al. 2007)

  4. SN 2006gy Pulsational pair instability Circum-stellar material (Woosley et al. 2007) (Van Marle et al. 2010)

  5. SN 2006gy

  6. Quark Star • Witten (1984) conjecture: • UDS ground state for strongly interacting matter • RHIC experiment • Existence of the Quark-Gluon Plasma • Ouyed et al. (2002) considered explosive transition from neutron star to quark star (Magertis et al. 2000) Quark Nova

  7. Quark Nova • Two step process: Hadronic U,D  U,D,S • Detonative combustion • Outer layers accelerated to ultra-relativistic velocities • 1052 erg of kinetic energy • Favourable r-process site • Predominantly form heavy elements, A>130 (Niebergal et al. 2010) (Keranen et al. 2005) (Jaikumar et al. 2007)

  8. Collision with Envelope

  9. Geometric Model • RSNE • Temperature: T a t -2 • Velocity: v a r • HP • Temperature: T a t -4/3 • Velocity: v = const

  10. Methodology • Using SHAPE 1. Build time evolving geometric model 2. Run radiative transfer code Simultaneously creates light curve and spectra Developed by: Wolfgang Steffen & NicoKoning

  11. Model Light Curve

  12. Model Comparison Pulsational Pair Instability Circum-stellar Material Quark Nova

  13. Model Spectrum

  14. Spectral fit

  15. Consistencies

  16. Further Study on SN 2006gy (Kawabata et al. 2009)

  17. Where to from here... Quark nova as universal model for super-luminous supernova?

  18. References • Woosleyet al., 2007, Nature, 450, 390 • Ofek et al., 2007, ApJ, 659, L13 • Smith et al., 2007, ApJ, 666, 1116 • Smith et al., 2008, ApJ, 686, 485 • Van Marle et al., 2010, MNRAS, 407, 2305 • Witten, 1984, Phys. Rev. D, 30, 272 • Margetis et al., 2000, Annu. Rev. Nucl. Part. Sci., 50, 299 • Ouyed et al., 2002, A&A, 390, L39 • Niebergal et al., 2010, (in press) arXiv:1008.4806 • Keranen et al., 2005, ApJ, 618, 485 • Kawabata et al., 2009, ApJ, 697, 747 • Brown & Mallik, 2008, A&A, 481, 507 • Leahy & Ouyed, 2008, MNRAS, 387, 1193

  19. Best Fit Parameters

  20. Radiative Transfer • Ray-tracing algorithm • Cont. emission & absorption coefficients • RSNE: Recombination • HP: Diffusion luminosity • Thompson Scattering • Only included scattering out of beam (Brown & Mallik 2008) (Leahy & Ouyed 2008)

  21. Quark Nova (Jaikumar et al. 2007)

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