The equilibrium structure of the crust of a neutron star results from the balance of pressure, electromagnetic and elastic stresses, and gravitational pull exerted by the whole star. The global structure of the crust can be calculated by solving Einstein’s equations

where is the gravitational constant and the speed of light. The Ricci scalar and the scalar curvature are determined from the spacetime metric , which represents gravity. Pressure, electromagnetic and elastic stresses are taken into account in the energy-momentum tensor .As a first approximation, treating the star as an ideal fluid, the energy-momentum tensor is given by (see, e.g., Landau & Lifshitz [248])

where is the mass-energy density and is the 4-velocity of the fluid. Equation (84) can be written in an equivalent but more general form [70] where is the total 4-current, is the total particle number density in the fluid rest frame and is the momentum per particle of the fluid given by The quantity is a dynamic effective mass defined by the relation where is the speed of light. As shown by Carter & Langlois [80], Equation (85) can be easily transposed to fluid mixtures (in order to account for superfluidity inside the star) as follows where X labels matter constituents and is a generalized pressure, which is not simply given by the sum of the partial pressures of the various constituents (see Section 10).The electromagnetic field can be taken into account by including the following contribution to the stress-energy tensor

where is the electromagnetic 2-form. Likewise elastic strains in the solid crust contribute through an additional term . While the components of are small compared to (remember that the shear modulus is of , Section 7), it can produce nonaxial deformations in rotating neutron stars, and nonsphericity in nonrotating stars, as discussed in Section 12.5. For the time being, we will use the ideal-fluid approximation, , and consider the effect of on neutron star structure in Section 12.5. We will, therefore, consider purely-hydrostatic equilibrium of the crust, instead of a more general hydro-elastic equilibrium.

6.1 Spherical nonrotating neutron stars

6.2 Approximate formulae

6.3 Crust in rotating neutron stars

6.4 Effects of magnetic fields on the crust structure

6.2 Approximate formulae

6.3 Crust in rotating neutron stars

6.4 Effects of magnetic fields on the crust structure

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