1. A New Type of Thermonuclear Supernova, and How the Pulsar Got his Spin
Novel Explosions:
A New Type of Thermonuclear Supernova, and
How the Pulsar Got his Spin
John M. Blondin
NC State University
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2. Remnants of Core-Collapse Supernovae
Relic Blastwave
Spinning Neutron Star
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3. The Supernova story has a long history of computational physics…
1966 Colgate and White
Neutrino-Driven prompt explosion
1985 Bethe and Wilson
Shock reheating via neutrino energy deposition
1992 Herant, Benz, and Colgate
Convective instability above neutrino-sphere
1957 Burbidge^2 Fowler Hoyle
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4. Anatomy of a Core-Collapse Supernova
The last decade has seen a great deal of interest in multidimensional effects:
Convection with the proto-neutron star
Neutrino-driven convection below the stalled shock
Instability of the stalled shock
All of these may operate together!
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5. First generation of 2D SN models hinted at
a low-order asymmetry in the shock wave
at late times (100’s of msec after bounce).
Burrows, Hayes & Fryxell 1995
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6. To investigate the dynamics of the stalled supernova shock,
we consider an idealized problem:
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7. SN Code Verification
Houck and Chevalier 1992
Blondin and Mezzacappa 2005
This post-bounce model provides an opportunity to verify supernova codes against the results of a linear perturbation analysis.
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8. Spherical Accretion Shock Instability
Blondin, Mezzacappa, DeMarino 2003, ApJ, 584, 971
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9. The SASI is a global acoustic mode:
The spherical accretion shock acts as an acoustic cavity,
with a trapped standing wave growing exponentially with time.
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10. Must move to 3D!
This initial SASI discovery with axisymmetric 2D simulations pointed to the obvious need for models in full 3D.
Add picture of bi-polar SASI
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rotational period (ms)
100
200
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22. SASI A non-rotating, spherically symmetric progenitor star can leave
behind a neutron star spinning with a period of tens of milliseconds.
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