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 Nico Koning, Denis Leahy, Wolfgang Steffen – Collaborators Canadian Workshop on the Nuclear and Astrophysics of Stars.

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)

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

SN 2006gy

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

Two step process: Hadronic  U,D  U,D,S Detonative combustion Outer layers accelerated to ultra-relativistic velocities 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)

Collision with Envelope

Geometric Model RSNE – Temperature: T  t -2 – Velocity: v  r HP – Temperature: T  t -4/3 – Velocity: v = const

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

Model Light Curve

Model Comparison Pulsational Pair InstabilityCircum-stellar MaterialQuark Nova

Model Spectrum

Spectral fit

Consistencies

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

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

References 1.Woosley et al., 2007, Nature, 450, Ofek et al., 2007, ApJ, 659, L13 3.Smith et al., 2007, ApJ, 666, Smith et al., 2008, ApJ, 686, Van Marle et al., 2010, MNRAS, 407, Witten, 1984, Phys. Rev. D, 30, Margetis et al., 2000, Annu. Rev. Nucl. Part. Sci., 50, Ouyed et al., 2002, A&A, 390, L39 9.Niebergal et al., 2010, (in press) arXiv: Keranen et al., 2005, ApJ, 618, Kawabata et al., 2009, ApJ, 697, Brown & Mallik, 2008, A&A, 481, Leahy & Ouyed, 2008, MNRAS, 387, 1193

Best Fit Parameters Physical ParameterValue Stellar Mass (RSNE + HP)80 ( ) Msun Shock Temperature 1.2 x 10 9 K QN Delay Time10 days Shock Speed6000 km s -1 HP Speed95 km s -1 HP Thickness5 x 10 8 m RSNE Temp. Pwr. Law index0.4 RSNE Density Pwr. Law index0.2 Radiative Parameters Value A655 B6 x 10 -4

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)

Quark Nova (Jaikumar et al. 2007)