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

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Presentation transcript:

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.)

What is the mechanism of explosion?

Multi-Messenger Astrophysics: Exhibit A

Learn from GW?

Indirect Direct

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?

Mechanism is inherently multi-dimensional

Mechanism is inherently multi-dimensional GW Emission

Explosion Dynamics

Theory: to appreciate what we can learn from GWs

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

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?

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

Is a critical luminosity relevant in hydrodynamic simulations?

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

Murphy & Burrows ‘08

Nordhaus et al. ‘10

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

Turbulence

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 o Quick self consistent explosions o Systematic investigations of explosions, NS masses, etc. A Theoretical Framework

Murphy, Ott, and Burrows, ‘09

Initial LIGO Enhanced LIGO Advanced LIGO

Source Region for GWs?

Characteristic GW frequencies and amplitudes?

N 2 < 0 Convectively unstable N 2 > 0 Stably stratified (gravity waves)

b(r) = ∫ N 2 dr = buoyant accel. N 2 < 0 Convectively unstable N 2 > 0 Stably stratified (gravity waves) DpDp Over shoot The Model: Buoyant Impulse vpvp

D p ~ v p / N f p ~ N/(2  ) h +  f p v p Similar analysis for 3D convection in stellar interiors (Meakin & Arnett 2007, Arnett & Meakin 2009) The Model: Buoyant Impulse R b =  b D p vp2vp2 b(r) = ∫ N 2 dr

D p ~ v p / N f p ~ N/(2  ) h +  f p v p Similar analysis for 3D convection in stellar interiors (Meakin & Arnett 2007, Arnett & Meakin 2009) R b =  b D p vp2vp2 b(r) = ∫ N 2 dr The Model: Buoyant Impulse

f p ~ N/(2  )

Progenitor Mass and Luminosity Dependence

h +  f p v p

N 2 = GM r r3r3 Γ1Γ1 dlnP dlnr dlnρ ( ) 1 -

N 2 = GM r r3r3 Γ1Γ1 dlnP dlnr dlnρ ( ) 1 - Dense matter EOS Local Thermodynamics and Neutrino transport

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