1. When a star dies…

2. Introduction What are compact objects? –White dwarf, neutron stars & black holes Why study? –Because it’s fun! –Test of physics in extreme condition.

3. Why compact? It is all about balance! Degenerate pressure

4. How are they formed? End stage of stars Mass determines fate

6. Low mass stars Sun-like stars Massive stars Low mass stars Sun-like stars Massive stars Low mass stars Sun-like stars Massive stars It’s all about mass

7. Red Giants Sun-like stars

8. Planetary Nebula 1 light yr across UV from the white central dwarf Emission lines

9. M57 Blue SnowballCat’s Eye DumbbellHelix

10. White Dwarfs Snow White and the Seven Dwarfs

11. White Dwarfs =>  10 6 g/cm 3 Mass ~ M  (but <1.4) Radius ~ R 

12. White Dwarfs ~100,000K when born Blackbody peaks @ UV Yes, it’s organic! -- Crystalline carbon, oxygen like diamond, but 3,000 times harder So? Type Ia supernova

13. Example: Sirius B Discovered in 1862 m v =8.3 Surface temperature 25,000K Separation: 20AU Orbital period: 50 yrs

14. Sirius B

15. Death of Massive Stars

16. Supernova (Type II) E tot ~10 53 ergs (99% neutrinos) E kin ~ 10 51 ergs E visible ~10 49 ergs Ni-56, Co-56 Outshine the host galaxy! Core  NS/BH Not type I!

17. Example: SN 1987a movie

18. Movies x3

19. Neutron Stars Predicted by Baade & Zwicky (1934) Densest object that has surface M ~ 1.4 M  ; R~10 km Giant nucleus A=10 57 Degenerate neutron pressure Strong magnetic field ~ 10 12 gauss (H: 160eV) Strong surface gravity ~ 10 11 g Surface temperature ~ 10 6 K

20. How Compact? Or 466,000 x

21. How Compact? M ~ 1.4 M  ; R~10 km =>  10 14 g/cm 3 Similar to nucleus: 10 -24 g/(10 13 cm) 3 World Population: ~10 9

22. Mass-radius Relation

23. Structure Atmosphere: ~cm Crust: Fe Neutron drip: 4x10 11 g/cm 3 Superfluidity Nuclear density: 2.8x10 14 g/cm 3 Core: quark matter?

24. Pulsar LGM: Jocelyn Bell (1967) Period 1.6 ms to 8s Are pulsars neutron stars? –Timescale (< 500km) –Good clocks

25. Blackbody + Power-law Where’s the energy from? Rotating magnet Polar cap Outer gap Emission

26. Example: Crab Pulsar SN1054 –guest star P=33ms Jet+torus (movies)

27. Research Topics Quark matter? Cooling Atmosphere Gamma-ray emission Magnetars: 10 15 gauss AXP VHE (>100Gev) from SNR

28. URCA Process Cooling

29. Quark Stars? Stable quark matter (Witten 1984) 3C 58 ? RXJ 1856.5-3754 ?

31. GRB Energy scale: keV – MeV Total energy: 10 52 ~10 54 erg Timescale: ms – ks

32. Social Behavior Double NS/ Pulsar Millisecond (recycled) pulsars HMXBs LMXBs QPO

33. Double NS Double NS: PSR B1913+16 –Test of GR (93’ Nobel) Double pulsars: PSR J0737-3039 –GR, magnetosphere –movie

34. QPO Quasi-periodic oscillations

35. Reference Shapiro & Teukolsky --Black holes, White dwarfs and Neutron Stars – the Physics of Compact Objects