THE QUARK NOVA PROJECT I

THE QUARK NOVA PROJECT I

Distinct Photometric and Chemical Evidence of the Quark Nova

in SN2006gy

Friday, December 10th 2010Mathew Kostka – PhD StudentRachid Ouyed – SupervisorNico Koning, Denis Leahy, Wolfgang Steffen – Collaborators

Canadian Workshop on the Nuclear and Astrophysics of Stars.

SN 2006gy

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 2006gyPulsational 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

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)

Collision with Envelope

Geometric Model

• RSNE– Temperature: T a t -2

– Velocity: v a r

• HP– Temperature: T a t -4/3

– Velocity: v = const

Methodology

• Using SHAPE1. Build time evolving geometric model2. Run radiative transfer code

Simultaneously creates light curve and spectra

Developed by: Wolfgang Steffen & Nico Koning

Model Light Curve

Model Comparison

Pulsational Pair Instability Circum-stellar Material Quark 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?

References1. Woosley et al., 2007, Nature, 450, 3902. Ofek et al., 2007, ApJ, 659, L133. Smith et al., 2007, ApJ, 666, 11164. Smith et al., 2008, ApJ, 686, 4855. Van Marle et al., 2010, MNRAS, 407, 2305 6. Witten, 1984, Phys. Rev. D, 30, 2727. Margetis et al., 2000, Annu. Rev. Nucl. Part. Sci., 50, 299 8. Ouyed et al., 2002, A&A, 390, L39 9. Niebergal et al., 2010, (in press) arXiv:1008.480610. Keranen et al., 2005, ApJ, 618, 48511. Kawabata et al., 2009, ApJ, 697, 747 12. Brown & Mallik, 2008, A&A, 481, 50713. Leahy & Ouyed, 2008, MNRAS, 387, 1193

Best Fit ParametersPhysical Parameter Value

Stellar Mass (RSNE + HP) 80 (60 + 20) Msun

Shock Temperature 1.2 x 10 9 K

QN Delay Time 10 days

Shock Speed 6000 km s -1

HP Speed 95 km s -1

HP Thickness 5 x 10 8 m

RSNE Temp. Pwr. Law index 0.4

RSNE Density Pwr. Law index 0.2

Radiative Parameters Value

A 655

B 6 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)