Atomic calculation for the atmospheres of strongly-magnetized neutron stars

摘要: Complete modeling of radiative transfer in neutron star atmospheres is progress, taking into account the anisotropy induced by magnetic fields, nonideal effects, and general relativity. As part our modeling, we present a novel atomic calculation method producing an extensive data set including energy values oscillator strengths so-called Landau regime (B > 4.7 × 109Z2 G). Conventional atmosphere models for B = 0 are not applicable to typical field cooling stars ~ 1012-1013 G), since atom no longer keeps its spherical shape. The elemental composition configuration presently unknown, so that must be produced ground excited states several ions as function field. To accomplish this efficiently, minimized iterations Hartree equation treated exchange terms higher perturbation methods. This has effect reducing computation time significantly. Inclusion gives us much more accurate inner orbitals unlike other methods based on adiabatic approximation. While existing available only low-Z atoms, can used elements up Fe with sufficient accuracy use spectroscopic missions such Chandra, XMM-Newton, next-generation X-ray telescopes.