A Model for GW Emission from CCSN Explosions

1. A Model for GW Emission from CCSN Explosions by Jeremiah W. Murphy NSF AAP Fellow (University of Washington) Collaborators: Christian Ott (Caltech), Adam Burrows (Princeton U.)

2. What is the mechanism of explosion?

3. Multi-Messenger Astrophysics: Exhibit A

4. Learnfrom GW?

5. Indirect Direct

7. Neutrino Mechanism: • Neutrino-heated convection • Standing Accretion Shock Instability (SASI) • Explosions? Maybe • Acoustic Mechanism: • Explosions but caveats. • Magnetic Jets: • Only for very rapid rotations • Collapsar?

8. Mechanism is inherently multi-dimensional

9. Mechanism is inherently multi-dimensional GW Emission

10. Explosion Dynamics

11. Theory: to appreciate what we can learn from GWs

12. Fundamental Question of Core-Collapse Theory Steady-State Accretion Explosion ?

13. Neutrino Mechanism: • Neutrino-heated convection • Standing Accretion Shock Instability (SASI) • Explosions? Maybe • Acoustic Mechanism: • Explosions but caveats. • Magnetic Jets: • Only for very rapid rotations • Collapsar?

14. Burrows & Goshy ‘93 Steady-state solution (ODE) Explosions! (No Solution) Le Critical Curve Steady-state accretion (Solution) . M

15. Is a critical luminosity relevant in hydrodynamic simulations?

16. How do the critical luminosities differ between 1D and 2D?

17. Murphy & Burrows ‘08

18. Murphy & Burrows ‘08

19. Nordhaus et al. ‘10

20. Why is critical luminosity of 2D simulations ~70% of 1D?

21. Turbulence

22. A Theoretical Framework • Solutions for successful explosions • Develop Turbulence model for CCSN • Use 3D simulations to calibrate • Derive critical curve with turbulence • Use turbulence model in 1D rad-hydro simulations • Quick self consistent explosions • Systematic investigations of explosions, NS masses, etc.

24. Murphy, Ott, and Burrows, ‘09

27. Initial LIGO Enhanced LIGO Advanced LIGO

29. Source Region for GWs?

31. Characteristic GW frequencies and amplitudes?

32. N2 < 0 Convectively unstable N2 > 0 N2 > 0 Stably stratified (gravity waves)

33. N2 < 0 Convectively unstable The Model: Buoyant Impulse vp N2 > 0 Dp Over shoot N2 > 0 Stably stratified (gravity waves) b(r) = ∫ N2dr = buoyant accel.

34. b Dp Rb = vp2 The Model: Buoyant Impulse b(r) = ∫ N2dr Dp ~ vp / N fp ~ N/(2) h+ fp vp Similar analysis for 3D convection in stellar interiors (Meakin& Arnett 2007, Arnett & Meakin 2009)

35. b Dp Rb = vp2 The Model: Buoyant Impulse b(r) = ∫ N2dr Dp ~ vp / N fp ~ N/(2) h+fpvp Similar analysis for 3D convection in stellar interiors (Meakin& Arnett 2007, Arnett & Meakin 2009)

36. fp ~ N/(2)

37. Progenitor Mass and  Luminosity Dependence

38. h+ fp vp

39. ) ( - dlnρ dlnP 1 GMr N2 = dlnr dlnr Γ1 r3

40. Local Thermodynamics and Neutrino transport Dense matter EOS ) ( - dlnρ dlnP 1 GMr N2 = dlnr dlnr Γ1 r3

41. Summary • GW Emission • Explosion Mechanism • Protoneutron Star Structure • Dense Matter EOS • Explosion Dynamics