1 / 14

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. Delayed Explosions. Neutrino Trapping. Neutrinos Arrive from SN1987A. Hirata et al Phys. Rev. Lettt 58, 1490 (1987). PTF, LSSN, CRTS (~700 / yr ).

keiran
Download Presentation

Ay 123 Lecture 11 - Supernovae & Neutron Stars

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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. Delayed Explosions

  4. Neutrino Trapping

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

  6. PTF, LSSN, CRTS (~700/yr) SNf and SDSS & SNLS High-Z Searches KAIT Calán-Tololo Search Zwicky + Amateurs Supernova Discovery Statistics - I

  7. Supernova Discovery Statistics - II

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

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

  10. 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)

  11. Routes to a SNeIain degenerate C-O WD systems 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

  12. 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

  13. 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!

  14. 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)

More Related