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.
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 - PowerPoint PPT Presentation
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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