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Ay 123 Lecture 11 - Supernovae & Neutron Stars

Ay 123 Lecture 11 - Supernovae & Neutron Stars. Timescales for HS Burning. faster and faster. Structure of Massive Star at End of HS Burning. Neutrinos Arrive from SN1987A. Hirata et al Phys. Rev. Lettt 58, 1490 (1987). Neutrino Trapping. Supernova Discoveries. Supernovae Light Curves.

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Ay 123 Lecture 11 - Supernovae & Neutron Stars

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  1. Ay 123 Lecture 11 - Supernovae & Neutron Stars Timescales for HS Burning faster and faster..

  2. Structure of Massive Star at End of HS Burning

  3. Neutrinos Arrive from SN1987A Hirata et al Phys. Rev. Lettt 58, 1490 (1987)

  4. Neutrino Trapping

  5. Supernova Discoveries

  6. Supernovae Light Curves II Plateau Ia II Linear Doggett & Branch AJ 90, 2303 (1985)

  7. Supernovae Spectra Thermonuclear: Type Ia: Si, no H Core Collapse: Type II: H emission Type Ib: He, weak H Type Ic: no H, no He Review: Filippenko, ARAA 35, 309 (1997)

  8. Origin of `P Cygni’ Profile P Cygni: luminous blue variable with blue-shifted (absorbing) outflow against core emission

  9. Delayed Explosions

  10. Decay of Nuclei and SN II light curves Ni56 t=6.1d Co56 t=77d SN1987A: McCray ARAA 31, 175 (1993)

  11. The Ring Around SN1987A Original FOC image (1990) Post-repair image 1.66” IUE observes a brightening in UV emission lines 413d after SN explosion - pre-SN ejecta is being illuminated by the explosion. Resolving the diameter of the ring gives its size and an absolute distance to the LMC Panagia et al Ap J 380, L29 (1991)

  12. Cosmological Distances from SN II P Flux, temperature & expansion velocity during `plateau phase’

  13. Hubble Diagram for SNe IIP scatter = 0.26 mag (for Ia scatter~0.20) Could detect acceleration with present technology (~15 SNIIP) More effectively probe to high z with JWST/TMT (Nugent et al 2006)

  14. SN Ia Light Curve Shape - Luminosity Correlation Reduces scatter on `Hubble diagram’ No correction Correction Phillips 1993 Ap J 413, L105; Riess et al 1995 Ap J 438, 17

  15. Host Galaxy Dependence of SNe Ia Properties Ia rate SFR/mass Width of light curve SN Ia rate correlates with specific SFR of host galaxy Light curve `stretch’ likewise correlates SN properties depend on mix of stellar population Sullivan et al Ap J 648, 868 (2006)

  16. Routes to a SNeIa in single degenerate C-O WD systems (Nomoto et al astro-ph/9907386) AGB with C+O core RG+He core WD + MS in common envelope WD + red giant Wind reduces rate Short time delay Significant time delay

  17. Cosmic Acceleration From SNe Ia Perlmutter et al 1999 • Light curve corrected peak luminosities give luminosity distance • Redshifts give cosmic expansion velocities • SNe Ia are too faint for a given redshift c.f. decelerating models!

  18. Implications of Cosmic Acceleration • Why not ? two puzzles: • expect = 8GmP4 • (10120 larger) • Why acceleration now? • M  R-3 (matter) • vac = const (vacuum) Perlmutter et al 1999 Alternative: new physics - “dark energy”: quintessence: equation of state p = w ;  R-3(1+w) dynamical scalar field w = w(t)

  19. Deep HST Survey Riess et al Ap J 659, 98 (2007)

  20. First Year Results from CFHT SNLS Astier et al A&A 447, 31 (2006) 71 homogenously studied SNe Ia w = -1.023 ± 0.090 i.e. equivalent to Cosmological Constant

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