Magnetar Oscillations: Shedding Light on the Neutron Star Equation of StateState of Nuclei Below Neutron DripState of Nuclei Above Neutron DripNuclear State Within in Neutron Star Crust-ray Light Curve of Magnetar Giant Flare from SGR 1900+14Sudden Displacement Sends Pulse Into the Surrounding MagnetospherePlasma Generation in MagnetosphereAdiabatic Indices at Varying Densities Below Neutron DripAdiabatic Indices at Varying Densities Above Neutron DripShear Speed Nearly Constant Throughout CrustNS 11R9 Toroidal Mode FrequencyNS 24R115 Toroidal Mode FrequencySome ThoughtsReferencesBinding Energy of Extremely Large NucleiNuclear State Within Neutron Star CrustMagnetar Oscillations:Magnetar Oscillations:Magnetar Oscillations:Shedding Light on the Neutron Shedding Light on the Neutron Shedding Light on the Neutron Star Equation of StateStar Equation of StateStar Equation of StateStephen R. SchwartzStephen R. SchwartzStephen R. SchwartzState of Nuclei Below Neutron DripState of Nuclei Below Neutron DripState of Nuclei Below Neutron DripBPS (1971)State of Nuclei Above Neutron DripState of Nuclei Above Neutron DripState of Nuclei Above Neutron DripNegele (1974)Nuclear State Within in Neutron Nuclear State Within in Neutron Nuclear State Within in Neutron Star CrustStar CrustStar CrustLRP (1993)γγγ---ray Light Curve of Magnetar ray Light Curve of Magnetar ray Light Curve of Magnetar Giant Flare from SGR 1900+14Giant Flare from SGR 1900+14Giant Flare from SGR 1900+14Duncan (2003)W & S (2007)Sudden Displacement Sends Pulse Sudden Displacement Sends Pulse Sudden Displacement Sends Pulse Into the Surrounding MagnetosphereInto the Surrounding MagnetosphereInto the Surrounding MagnetosphereDuncan (2003)Plasma Generation in Plasma Generation in Plasma Generation in MagnetosphereMagnetosphereMagnetosphereDuncan (2003)Adiabatic Indices at Varying Adiabatic Indices at Varying Adiabatic Indices at Varying Densities Below Neutron DripDensities Below Neutron DripDensities Below Neutron DripNegele (2007)Adiabatic Indices at Varying Adiabatic Indices at Varying Adiabatic Indices at Varying Densities Above Neutron DripDensities Above Neutron DripDensities Above Neutron DripNegele (1974)Shear Speed Nearly Constant Shear Speed Nearly Constant Shear Speed Nearly Constant Throughout CrustThroughout CrustThroughout CrustPiro (2005)-0.5 0 0.5 1 950000 960000 970000 980000 990000 1e+06 1.01e+06 1.02e+06 1.03e+06 1.04e+06Dimensionless Oscillation AmplitudeRadius (cm)Oscillation Amplitudes for l=2: NS 07R952t0 -0.5 0 0.5 1 950000 960000 970000 980000 990000 1e+06 1.01e+06 1.02e+06 1.03e+06 1.04e+06Dimensionless Oscillation AmplitudeRadius (cm)Oscillation Amplitudes for l=2: NS 07R952t0 2t1 -0.5 0 0.5 1 950000 960000 970000 980000 990000 1e+06 1.01e+06 1.02e+06 1.03e+06 1.04e+06Dimensionless Oscillation AmplitudeRadius (cm)Oscillation Amplitudes for l=2: NS 07R952t0 2t1 2t3 -0.5 0 0.5 1 950000 960000 970000 980000 990000 1e+06 1.01e+06 1.02e+06 1.03e+06 1.04e+06Dimensionless Oscillation AmplitudeRadius (cm)Oscillation Amplitudes for l=2: NS 07R952t0 2t1 2t3 2t6NS 11R9 NS 11R9 NS 11R9 Toroidal Toroidal Toroidal Mode Mode Mode FrequencyFrequencyFrequency••Thickness:Thickness:8.24%8.24%••Mass Ratio:Mass Ratio:4.09%4.09%••Surface Surface RedshiftRedshift::~ ~ 0.270.27••Radius Estimate:Radius Estimate:~ ~ 9km9km•Mass EstimateMass Estimate115115W & S (2007)NS 24R115 NS 24R115 NS 24R115 Toroidal Mode Toroidal Mode Toroidal Mode FrequencyFrequencyFrequency••Redshift neglected Redshift neglected model yields NS model yields NS with unrealistically with unrealistically high densitieshigh densities••Information on crust Information on crust thickness still thickness still informativeinformative••Thickness:Thickness:8.43%8.43%••Mass Ratio:Mass Ratio:3.49%3.49%Some ThoughtsSome ThoughtsSome Thoughts••Crust turned out to be about half Crust turned out to be about half as thick as expectedas thick as expected••Would expect that this could be Would expect that this could be slightly mitigated by adding the slightly mitigated by adding the effects of the magnetic field into effects of the magnetic field into the pulsation equationthe pulsation equation••Waiting for more flares!Waiting for more flares!ReferencesReferencesReferences••Baym, G., Pethick, C., and Sutherland, P. 1971, ApJ.Baym, G., Pethick, C., and Sutherland, P. 1971, ApJ.170, 299.170, 299.••Duncan, R.C. 2003, http://solomon.as.utexas.edu/.Duncan, R.C. 2003, http://solomon.as.utexas.edu/.••Lorenz, C.P., Ravenhall, D.G., and Pethick, C.J. 1993,Lorenz, C.P., Ravenhall, D.G., and Pethick, C.J. 1993,Phys. Rev. Lett., 70, 4.Phys. Rev. Lett., 70, 4.••Negele, J.W. 1974, Negele, J.W. 1974, Physics of Dense MatterPhysics of Dense Matter, IAU, IAUSymposium 53, Dordrecht, Boston, Reidel, p.1.Symposium 53, Dordrecht, Boston, Reidel, p.1.••Piro, A. 2005, ApJ, 634, L153.Piro, A. 2005, ApJ, 634, L153.••Thompson, C. and Duncan, R.C. 1995, Mon. Not. R. Ast. Thompson, C. and Duncan, R.C. 1995, Mon. Not. R. Ast. Soc., 275,255.Soc., 275,255.••Watts, A. and Strohmayer, T.E. 2007, arXiv:astroWatts, A. and Strohmayer, T.E. 2007, arXiv:astro--ph/0608476.ph/0608476.Binding Energy of Extremely Binding Energy of Extremely Binding Energy of Extremely Large NucleiLarge NucleiLarge NucleiNegele (1974)Nuclear State Within Neutron Nuclear State Within Neutron Nuclear State Within Neutron Star CrustStar CrustStar CrustLRP