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Modeling Type Ia Supernovae from ignition, to explosion, to emission

Modeling Type Ia Supernovae from ignition, to explosion, to emission. Daniel Kasen UC Santa Cruz. Supernova Discovery History Asiago Catalog (all supernova types). Supernova Factory Lick observatory SN search CfA SN group Carnegie SN project ESSENCE Supernova Legacy Survey.

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Modeling Type Ia Supernovae from ignition, to explosion, to emission

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  1. Modeling Type Ia Supernovaefrom ignition, to explosion, to emission Daniel Kasen UC Santa Cruz

  2. Supernova Discovery HistoryAsiago Catalog (all supernova types)

  3. Supernova Factory Lick observatory SN search CfA SN group Carnegie SN project ESSENCE Supernova Legacy Survey Supernova Discovery FutureRough predictions and promises… Can we use Type Ia SNe as reliable standard candles at the few % level? Systematic error, not statistical error, is the issue (e.g., luminosity evolution) PanStarrs Dark Energy Survey JDEM Large Synoptic Survey Telescope (LSST)

  4. SN Ia ProgenitorsAccreting white dwarf near the Chandrasekhar limit Issues with the single degenerate scenario Where is the hydrogen? How do you make them in old (~10 Gyr) systems? What about observed “Super-Chandra” events? Could double white dwarf systems be the answer? Accretion rate: 10-7 Msun / year

  5. C/O Si/S/Ca 56Ni Fe C/O boom

  6. Type Ia Supernova Light Curvespowered by the beta decay: 56Ni 56Co 56Fe

  7. Type Ia Width-Luminosity Relationbrighter supernovae have broader light curves

  8. Type Ia Supernova Spectrum 20 days after explosion

  9. C/O Si/S/Ca 56Ni Fe Toy Type Ia Supernova Models w/ Stan Woosley Sergei Blinikov Elena Sorokina Spherical Chandrasekhar mass models with varied composition Parameters MFe MNi MSi “mixing” MFe +MNi +MSi + Mco = MCH

  10. 3-dimensional Time-Dependent Monte Carlo Radiative Transfer SEDONA Code Expanding atmosphere Realistic opacities Three-dimensional Time-dependent Multi-wavelength Includes spectropolarization Treats radioactive decay and gamma-ray transfer Iterative solution for thermal equilibrium Non-LTE capability Kasen et al 2006 ApJ

  11. Broadband Synthetic Light CurvesModel Compared to observations of SN 2001el Parameters MFe = 0.1 Msun MNi = 0.6 Msun MSi = 0.4 Msun Kasen, ApJ 2006 Kasen (2006) ApJ

  12. Day 15 after explosion Time Evolution of SpectrumRecession of photosphere reveals deeper layers Day 35 after explosion C/O Si/S/Ca Model SN1994D 56Ni Fe

  13. Spectroscopic Time Series Optical Day 1 to Day 100

  14. Width-Luminosity RelationshipKasen and Woosley, ApJ, 2007

  15. FeII bound-bound Supernova Ejecta Opacityblending of millions of line transitions FeIII bound-bound

  16. All iron is FeII T ~ 7000 K FeIII starts becoming FeII Infrared Secondary Maximum marks the transition from FeIII to FeII I-Band Kasen (2006) ApJ

  17. Origin of the Width-Luminosity Relationdimmer SN are cooler, and recombine to FeII faster B-band I-band

  18. Model Width-Luminosity RelationWoosley, Kasen, Blinnikov, Sorokina, ApJ (2007) SN 99by B-band SN 91T

  19. Presupernova Evolution (~1000-109 years) accreting, convective white dwarf Type Ia supernova modeling challenge ignition Explosion (~1-100 secs) turbulent nuclear combustion / hydrodynamics free expansion Light Curves / Spectra (~1-100 days) radioactive decay / radiative transfer Observations

  20. White Dwarf Convection and IgnitionKuhlen, Woosley, and Glaitzmeier (2006)

  21. White Dwarf Convection (No rotation)3-D calculation, Ma and Woosley

  22. White Dwarf Convection (With Rotation)3-D calculation, Ma and Woosley

  23. t = 0.0 sec t = 0.5 sec t = 1.0 sec t = 1.5 sec 3D Deflagration ModelSubsonic turbulent combustion Roepke et al. (2005)

  24. 2D Deflagration Model Roepke, Kasen, Woosley MNi = 0.2 Msun EK = 0.3 x 1051 ergs

  25. DeflagrationToDetonationKhokhlov (1991)Hoeflich (1994)Gamezo et al (2005) Gamezo et al. But how to detonate?

  26. 2D Delayed Detonation Roepke, Kasen, Woosley The stronger the deflagration phase  the more pre-expansion  the lower the densities at detonation  the less 56Ni produced MNi = 0.5 Msun EK = 1.2 x 1051 ergs

  27. Off-Center Ignition University of Chicago FLASH Center

  28. Off-center Detonation Roepke, Kasen, Woosley An alternative to super-chandra SNe? Howell et al, 2006 Hillebrandt, Sim, Roepke 2007 MNi = 1.0 Msun EK = 1.3 x 1051 ergs

  29. Spectrum of Off-center Detonationexpansion velocities depend on orientation I-Band Kasen (2006) ApJ

  30. Spectroscopic Homogeneity and Diversitymonitoring silicon expansion velocities from Leonard et al, ApJ 2006

  31. Asymmetry and PolarizationObserved SNeIa are polarized at ~0.4 % level

  32. Asymmetry and PolarizationModel polarization spectrum at maximum lightas seen from different viewing angles

  33. The Theoretical Understanding of Type Ia Supernovae Pressing Questions What are the progenitors? How and where does ignition happen? How might the deflagration transition into a detonation? How do the light curves depend upon the progenitor and its environment?

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