Photoabsorption in magnetic neutron star atmospheres

Details Photoabsorption in magnetic neutron star atmospheres Photoabsorption in magnetic neutron star atmospheres

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...261..235v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 261, no. 1, p. 235-244.

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20

Absorption Spectra, Magnetic Stars, Neutron Stars, Photoabsorption, Stellar Atmospheres, Absorption Cross Sections, Atomic Energy Levels, Computational Astrophysics, Local Thermodynamic Equilibrium, Plasma Temperature

Scientific paper

The photoabsorption opacity is computed for magnetized atomic hydrogen in LTE, for conditions of interest in calculations of the emitted spectra from the surface of magnetic neutron stars. The resultant photoabsorption cross sections are found to strongly differ from those obtained in the nonmagnetic case in three principal ways: (1) photoabsorption edges appear in the soft X-ray range, at photon energies greater than 0.1 keV; (2) photoabsorption is the dominant opacity mechanism at high plasma temperatures reaching up to 1 keV; and (3) the cross section is strongly dependent on the angle and polarization of the incident photon. The first of these deviations is clearly due to the increased atomic binding in the neutron star's magnetic field, while the second is due to the presence of bound atoms at these temperatures, and is linked to the free electron's 1D phase space. The third distinguishing property is reminiscent of a similar behavior of the free-free and Thomson cross sections in the presence of a strong magnetic field.

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