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Sub-Nuclear Matter in Neutron Stars and Supernovae Nuclear Pasta and Complex Fluids

Sub-Nuclear Matter in Neutron Stars and Supernovae Nuclear Pasta and Complex Fluids. W.G.Newton 1 , J.R.Stone 1,2 1 University of Oxford, UK 2 Physics Division, ORNL, Oak Ridge, TN, USA. Outline. Overview of NS, SN Matter Anatomy of Supernovae (SNe) and Neutron Stars (NSs)

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Sub-Nuclear Matter in Neutron Stars and Supernovae Nuclear Pasta and Complex Fluids

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  1. Sub-Nuclear Matter in Neutron Stars and SupernovaeNuclear Pasta and Complex Fluids W.G.Newton1, J.R.Stone1,2 1University of Oxford, UK 2Physics Division, ORNL, Oak Ridge, TN, USA

  2. Outline • Overview of NS, SN Matter • Anatomy of Supernovae (SNe) and Neutron Stars (NSs) • Superfluidity in NSs • The Transition to Uniform Matter • Astrophysical consequences • Frustration and Complex Fluids • Nuclear Pasta • Self-consistent models • QMD • Hartree-Fock • A new Hartree-Fock study of nuclear pasta • Computational Method • Preliminary Results • Conclusions

  3. Anatomy of Core Collapse SN • Collapse proceeds until core reaches few times nuclear saturation density (≈2.4×1014g cm-3 or 0.16 baryons fm-3) • Neutrinos initially trapped above densities of (≈1012g cm-3), temperatures reach up to ≈100MeV and the proton fraction is roughly constant at ≈0.3

  4. Anatomy of a Neutron Star • <1011 g cm-3 Nuclear physics relatively well known (heavy nuclei) • >4×1011 g cm-3 (neutron drip): nuclear models begin to diverge • >5×1014 g cm-3 physics is extremely uncertain (Hyperons? Meson condensates? Quarks? When does description in terms of nucleonic degrees of freedom become unphysical?

  5. Superfluids in Neutron Stars • At temperatures below a critical temperature of ≈ 109K - 1010K, neutrons in the inner crust and core are expected to become superfluid (and, in the core, protons superconducting). • Superfluids have zero viscosity, and so cannot support bulk rotation. • If a fluid, rotating with period P(s), is cooled below the critical temperature, it arranges itself into quantized vortices of spin, density 104 /P cm-2

  6. Quantized vortices in a sodium gas cooled into a Bose-Einstein condensate and set into rotation (Onofrio et al, Phys Rev Lett 85, 2228, 2001) Superfluid Vortices

  7. Transition to Uniform Matter • The density regime 1013 < ρ < 2×1014 g/cm3 is important • It marks the transition from the outer crystalline crust of a NS, or the gas of nuclei, neutrons and leptons in a core collapse, to the liquid, homogeneous phase above nuclear saturation density

  8. The Transition to Uniform Matter: Astrophysical Consequences • Neutrino opacities and emission mechanisms • during core collapse • neutron star cooling • Pulsar Glitches • star-quakes • superfluid vortex dynamics • Pinned vortices? • Change in crustal composition and reheating during accretion • NS Oscillation • GWs

  9. If a system contains energetically favourable (attractive) and unfavourable (repulsive) interactions operating over the same range, matter will be frustrated. Prototypical frustrated system: Ising anti-ferromagnet on triangular lattice. Impossible to minimize energy with respect to all interactions simultaneously Large number of low energy configurations result Frustration and Complexity • At densities just below nuclear saturation (1013 – 1014 g cm-3) the • distances between Coulomb repelling nuclei becomes comparable • with the range of the attractive nuclear interaction that binds nuclei. • Complex structures thus develop – nuclear pasta.

  10. Nuclear Pasta • Competition between surface tension and Coulomb repulsion of closely spaced heavy nuclei results in a series of shape transitions from the inner crust to the core (Ravenhall et al Phys. Rev. Lett. 50, 2066, 1983 and Hashimoto et al, Progress of Th. Physics, 71, 2, 320, 1984). • The basic sequence is • (a) spherical (meatball/gnocchi) → (b) rod (spaghetti) → (c) slab (lasagna) → (d) tube (penne) → (e) bubble (swiss cheese?) → uniform matter

  11. Nuclear Pasta vs Complex Fluids • A wide range of mechanical properties are exhibited (liquid crystal, • sponge, rubber…) • Pethick, C.J. and Potekhin, A.Y. – Liquid Crystals in the Mantles of • Neutron Stars – Phys. Lett. B, 427, 7, 1998

  12. Self-consistent Modeling: QMD • Quantum Molecular Dynamics (QMD): semi-classical dynamical simulations with nucleonic degrees of freedom (Watanabe and Sonoda, nucl-th/0512020). • Pasta shapes emerge without pre-conditioning. • Pasta formation from compression and cooling demonstrated. 0.1ρ0 0.175ρ0 0.35ρ0 0.5ρ0 0.55ρ0

  13. Self-consistent Modeling: Mean field • Magierski and Heenen PRC65 045804 (2001): 3D HF calculation of nuclear shapes at bottom of neutron star crust at zero T • When examined self-consistently in three dimensions, many more configurations emerge - has effect of smoothing EoS • An important new phenomenon emerges: the fermionic Casimir effect. Scattering of unbound nucleons off nuclear structures leads to an effective interaction between those structures of order the energy difference between configurations

  14. Computational Method: Skyrme HF • Choose phenomenological nuclear interaction (Skyrme) • Assume one can identify (local) unit rectangular cells of matter at a given density and temperature, calculate one unit cell containing A nucleons (A up to 5000) • Hartree-Fock approximation: system can be represented by a single Slater determinant. • Minimize energy w.r.t. single particle wavefunctions: Schrödinger equation for A nucleons → A Schrödinger equations (A up to 5000) • Periodic boundary conditions φ(x,y,z) = φ(x+L,y+L,z+L) (More generally Bloch boundary conditions φ(x,y,z) = eikrφ(x+L,y+L,z+L)) • Impose parity conservation in the three dimensions: tri-axial shapes allowed, but not asymmetric ones. • Solution only in one octant of cell • Additional free parameters: A, (proton fraction yp), proton and neutron quadrupole moments Qp,20, Qp,22

  15. Unconstrained calculation at 8 densities between 0.01fm-3 and 0.12fm-3, T=0MeV, yp=0.03: Self-consistent dissolution of nuclear structure

  16. Integrated Densities at nb = 0.0195fm-3

  17. Integrated Densities at nb = 0.0312fm-3

  18. Integrated Densities at nb = 0.0390fm-3

  19. Integrated Densities at nb = 0.0507fm-3

  20. Integrated Densities at nb = 0.0585fm-3

  21. Integrated Densities at nb = 0.0702fm-3

  22. Integrated Densities at nb = 0.0780fm-3

  23. Integrated Densities at nb = 0.0976fm-3

  24. Minimization with respect to A T = 2.5MeV, nb=0.04fm-3 • Minimization with respect to quadrupole moments is obtained in a similar way

  25. T=5MeVnb=0.12fm-3Boundary Conditions and Shell Effects

  26. Pasta phase superimposes • artificial and real oscillations, • and real minima, on the curve

  27. Conclusions and Future • The properties of matter in the density region 1013 < ρ < 2×1014 g/cm3 are an important ingredient in NS and SN models • Thorough microphysical description of transition to uniform matter – the nuclear pasta phases – is underway • Generalize boundary conditions to the Bloch form: φ(x,y,z) = eikrφ(x+L,y+L,z+L) • Calculate entrainment coefficient • Examine response of matter to perturbation • neutrino interactions • mechanical properties • Investigate effects of BCS pairing • The Future(?) • Hydrodynamical modeling of pasta phases • Mesoscopic structures

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