- 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 on the moment of inertia
- 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
- I4Observations versus theory
- 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
Bedford Astronomy Club
» Strange Stars
-
Bedford Club Nederland
-
Reviews
-
Popular Articles
- Density Upper Atmosphere Earth
- Preface to 2004 Edition Quantum
- The Ash Dome Ascension Hours
- Morphogenesis mystery pattern
- Extended Solid Rocket Nozzles
- The Butterfly Bullet Space Shuttle
- Slurry Infiltration Consolidation
- Ahmad Cohen method Time Steps
- Kelvin Helmholtz Instability at
- Our Solar System Outer Space
- Riemanns Theory Gravity
- Equatorial Constellations
- Reflective Telescopes Active Optics
- The Ferraro Law Isorotation Mass
- The Ideal Gas Rigid Rotor Harmonic
-
Categories