Mass and Radius Constraints Using Magnetar Giant Flare

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Mass and Radius Constraints Using Magnetar Giant Flare Oscillations Alex T. Deibel With: Edward

Mass and Radius Constraints Using Magnetar Giant Flare Oscillations Alex T. Deibel With: Edward F. Brown (Michigan State University) Andrew W. Steiner (INT, University of Washington) HEAD Meeting 2013 Apr-8 -2013

Magnetar Giant Flares - QPOs • Giant flares triggered by crust reconfiguration • Modeled

Magnetar Giant Flares - QPOs • Giant flares triggered by crust reconfiguration • Modeled crust oscillations can be compared to QPOs Strohmayer & Watts 2006 Figure: Robert Duncan Deibel Apr-8 -2013

Crust composition • Nuclei crystal lattice • Neutron-rich nuclei • Degenerate electron and neutron

Crust composition • Nuclei crystal lattice • Neutron-rich nuclei • Degenerate electron and neutron gases • Magnetic field melts the crust and changes crust thickness Deibel, Steiner, and Brown 2013 (submitted) Deibel Apr-8 -2013

Perturbing the crust Bz ’ = 0 Surface Bz Outer Crust (Z, N), e

Perturbing the crust Bz ’ = 0 Surface Bz Outer Crust (Z, N), e Neutron Drip Inner Crust (Z, N), e, n Core ’ = 0 Deibel Apr-8 -2013

Assigning crust modes to QPO frequencies Equilibrium Nuclei Solve for Schumaker & Thorne 1983

Assigning crust modes to QPO frequencies Equilibrium Nuclei Solve for Schumaker & Thorne 1983 Piro 2005 Samuelsson & Andersson 2007 Steiner & Watts 2009 = Deibel Apr-8 -2013

Constraining masses and radii EOS: Steiner et al. 2010 Deibel, Steiner, and Brown 2013

Constraining masses and radii EOS: Steiner et al. 2010 Deibel, Steiner, and Brown 2013 (submitted) Deibel Apr-8 -2013

Summary Choose a mass and radius from Steiner et al. EOS Find crust composition

Summary Choose a mass and radius from Steiner et al. EOS Find crust composition and shear modulus Integrate perturbation through the crust Compare eigenmodes to QPOs Magnetar masses and radii agree to within 1 with PREs and LMXBs from Steiner et al. 2010 Deibel Apr-8 -2013

Extras

Extras

Discovery of Magnetars • Class of pulsars with recurring gamma ray emission (SGRs) Getting

Discovery of Magnetars • Class of pulsars with recurring gamma ray emission (SGRs) Getting the magnetic field: • Observe a pulsar’s period and spin-down rate • Assume a moment of inertia to get a dipole magnetic field Deibel Apr-8 -2013

Crust Modes • QPOs are torsional modes • Oscillations confined to the crust e

Crust Modes • QPOs are torsional modes • Oscillations confined to the crust e t d ui rfl pe su us Cr er ph os m at • Crust modes will depend on crust composition Core 10 km 1 km Deibel Apr-8 -2013

Shell effects - Magic Numbers Dieperink 2009 Magnetic Field - Landau Quantization Deibel Apr-8

Shell effects - Magic Numbers Dieperink 2009 Magnetic Field - Landau Quantization Deibel Apr-8 -2013

Model addition (1): Shell Effects No shell effects With shell effects Deibel Apr-8 -2013

Model addition (1): Shell Effects No shell effects With shell effects Deibel Apr-8 -2013

Model addition (2): Magnetic Field B = 0. 0 G B = 2. 0·

Model addition (2): Magnetic Field B = 0. 0 G B = 2. 0· 1015 G Deibel Apr-8 -2013

Core equation of state 1. 5 M 1. 0 M Steiner, Lattimer, Brown 2010

Core equation of state 1. 5 M 1. 0 M Steiner, Lattimer, Brown 2010 Deibel Apr-8 -2013

A giant flare from the magnetar SGR 1806A giant flare from the magnetar SGR 1806
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