A New Type of Thermonuclear Supernova, and How the Pulsar Got his Spin

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Presentation transcript:

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 NCSU Physics Colloquium

Remnants of Core-Collapse Supernovae Relic Blastwave Spinning Neutron Star NCSU Physics Colloquium

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 NCSU Physics Colloquium

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! NCSU Physics Colloquium

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 NCSU Physics Colloquium

To investigate the dynamics of the stalled supernova shock, we consider an idealized problem: NCSU Physics Colloquium

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. NCSU Physics Colloquium

Spherical Accretion Shock Instability Blondin, Mezzacappa, DeMarino 2003, ApJ, 584, 971 NCSU Physics Colloquium

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. NCSU Physics Colloquium

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 NCSU Physics Colloquium

NCSU Physics Colloquium

NCSU Physics Colloquium

NCSU Physics Colloquium

NCSU Physics Colloquium

NCSU Physics Colloquium

NCSU Physics Colloquium

NCSU Physics Colloquium

NCSU Physics Colloquium

NCSU Physics Colloquium

NCSU Physics Colloquium 50 rotational period (ms) 100 200 NCSU Physics Colloquium

NCSU Physics Colloquium

SASI A non-rotating, spherically symmetric progenitor star can leave behind a neutron star spinning with a period of tens of milliseconds. NCSU Physics Colloquium