Bedford Astronomy Club

» Strange Stars

  • A - 2
  • Ccx
  • Lom
  • A3
  • Accreted crust
  • Af
  • After the discovery of pulsars 19682005
  • An example Partially ionized hydrogen plasma
  • Analytical Models Of Nuclear Density Profiles
  • Analytical Representations Of Unified Eoss
  • B - 2
  • Eek
  • B1 Steplike profile model
  • B2 Smooth Composition Model
  • B21 Spherical nuclei in the inner crust
  • B22 Spherical nuclei in the outer crust
  • B23 Exotic nuclei
  • Before the discovery of pulsars 19321967
  • Bgn2
  • Birth in supernova explosions Supernova connection
  • Bound species in strong magnetic fields
  • C - 2
  • Nk4
  • C1 Representation convenient for nonrotating stars
  • C2 Representation convenient for rotating stars
  • C3 Adiabatic index
  • Changes in stellar parameters due to a corequake
  • Compressible liquid drop model CLDM
  • Con Macroglitches of radio pulsars
  • Con Strangelets in galaxies
  • Consequences
  • Cooling of neutron stars
  • Crystallization
  • D85
  • Deviations from an idealized ground state model
  • Effects of motion
  • Elastic properties of neutron star crust
  • Elastic shear moduli
  • Envelopes With Strong Magnetic Fields
  • Equilibrium Plasma Properties Outer Envelopes
  • Estimates of AR AI and AE in corequakes
  • Evolutionary scenarios Three driving forces
  • Exotic nuclei
  • Exotic selfbound states of superdense matter
  • Extended Thomas Fermi ETF calculations
  • F F F Fdeu Frad Fx Ffu457
  • Free electron in a magnetic field
  • From bcc lattice to isotropic solid
  • From November 2005 to August 2006 and beyond
  • G io ii i2
  • Gravitational surface redshift
  • Ground state of the bottom layers of the crust
  • Ground state of the inner crust at p 1014 g cm3
  • Ground state of the outer crust
  • History from prediction to discovery
  • Id
  • Ijk
  • Info - 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 36 37 38 39 40 41 42 43 44 45 46 47 48 49 50 51 52 53 54 55 56 57 58 59 60 61 62 63 64 65 66 67 68 69 70 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85
  • Introduction - 2 3
  • Ionization equilibria in the chemical picture
  • Jf2
  • Jo
  • K
  • Kaon condensation - 2
  • Kk99
  • Largeamplitude corequake and collapse
  • Linear response to a phase transition in the neutron star center
  • List Of Figures
  • List Of Tables
  • Lmc X4
  • M 17 072
  • M01
  • Magnetic condensation
  • Magnetic fields
  • Magnetic oscillations
  • MC0 MCo [FA FunstAj dA 774
  • Mesonexchange nucleonnucleon interaction
  • Mi Uks tnhzks2 ph
  • Millisecond and submillisecond pulsars
  • Mixedphase core and neutron star corequakes
  • Mixedphase state - 2
  • Mm0
  • Mmaxmmax ReqMm axRMmaX pspS12 838
  • MMq
  • Models of strongly magnetized outer envelopes of neutron stars
  • Moderate softening with density jump
  • Moderate softening without any density jump
  • Molecules and chains
  • N - 2 3
  • Nam2h n0
  • Neutrino processes
  • Neutrinos from Supernova 1987A and binding energy of neutron stars
  • Neutron star models
  • Neutron star radii
  • Neutron Star Structure
  • Neutron stars
  • Neutron Stars With Exotic Cores
  • Nj nee ZintjE3ion
  • Nnp
  • Nucleation of exotic highdensity phase
  • Nucleons
  • Nucleons and hyperons
  • Observational evaluations of the Crab Nebula parameters
  • Opal
  • Other models of strange quark matter
  • P - 2
  • P f a2h i2 T 3
  • P [g cm3
  • P14
  • Phase transitions and neutron star structure
  • Phenomenological nucleonnucleon interaction
  • Pion condensation - 2
  • Pm
  • Pmin max32 1 0808 x MM ms 6109
  • Pro Submillisecond pulsars
  • Pulsar glitches and crustal moment of inertia
  • Pulsar white dwarf binaries
  • Pulsars
  • Pulsars in binaries with nondegenerate stars
  • Quantum corrections to the CLDM energy
  • Quark deconfinement
  • Quark matter
  • Reaching the crustcore interface from the core side
  • Relativistic corrections and threebody interaction
  • Rp
  • Seismology
  • Semianalytical Eoss In Neutron Star Cores
  • Solid cores of neutron stars 771 Physical origins and models
  • Springer
  • Strange matter history
  • Strong softening with density jump The third family of compact stars
  • Strong softening without any density jump The third family of compact stars
  • Strongly coupled Coulomb plasma
  • Strongly magnetized hydrogen atmosphere
  • Strongly magnetized iron envelopes
  • Structure
  • Structure And Equation Of State Of Neutron Star Crusts
  • Summary of neutron star mass measurements
  • Superfluidity
  • T - 2
  • T0
  • Tables Of Eoss In Neutron Star Crust
  • Telescopes
  • The Bag Model with massive strange quarks and QCD interactions
  • The bulk approximation
  • The effects of the magnetic field on plasma ions
  • The energy balance of the Crab pulsar and its nebula
  • The formation of the crust in a newly born neutron star
  • The Hamiltonian
  • The nucleation of a mixed normalexotic phase
  • The proof of the inequality M A M A
  • The properties of nuclear matter
  • The simplest toy MIT Bag Model
  • The strange matter hypothesis
  • Theory Versus Observations
  • Thermodynamic functions of the ideal electron gas
  • Thermodynamics and kinetics
  • Threebody interaction
  • U
  • U 170037
  • Units
  • Unusual nuclear shapes
  • V
  • Vijk Vjk
  • Vl yS vIl2 21 Vss 3y4 ln yss
  • Volume 326
  • W
  • W fd w
  • Xray emission from accreting neutron stars in binaries
  • Y RMlx EOS A
  • Z32 1 Z32
  • Zmv T I
  • [ k4 1 ft[he 3 B X dk mB gaEg2
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