Equation of state and opacities for hydrogen atmospheres of neutron stars with strong magnetic fields

We present an equation of state and radiative opacities for a strongly magnetized hydrogen plasma at magnetic fields B, temperatures T, and densities rho typical for atmospheres of isolated neutron stars. The first- and second-order thermodynamic functions, monochromatic radiative opacities, and Rosseland mean opacities are calculated and tabulated, taking account of partial ionization, for 8 x 10(11) G less than or equal to B less than or equal to 3 x 10(13) G, 2 x 10(5) K less than or equal to T less than or equal to 10(7) K, and a wide range of rho. We show that bound-bound and bound-free transitions give an important contribution to the opacities at T less than or similar to (1-5) x 10(6) K in the considered range of B in the outer neutron star atmosphere layers, which may substantially modify the X-ray spectrum of a typical magnetized neutron star. In addition, we reevaluate opacities due to free-free transitions, taking into account the motion of both interacting particles, electron and proton, in a strong magnetic field. Compared to the previous neutron star atmosphere models, the free-free absorption is strongly suppressed at photon frequencies below the proton cyclotron frequency. The latter result holds for any field strength, which prompts a revision of existing theoretical models of X-ray spectra of magnetar atmospheres.