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Modeling Neutron Star Atmospheres
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Models of thermal emission of neutron stars, presumably formed in their atmospheres, are needed to infer the surface temperatures, magnetic fields, chemical composition, and neutron star masses and radii from the observational data. This information, supplemented with model equations of state and neutron star cooling models, is expected to move us further in understanding the fundamental properties of the superdense matter in the neutron star interiors. The neutron star atmospheres are very different from those of usual stars due to the immense gravity and huge magnetic fields. In this presentation we review the current status of the neutron star atmosphere modeling and present most important results.
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Cited by 2 Pith papers
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Evaluating the Evidence of Multipolar Surface Magnetic Field in PSR J0108$-$1431
The thermal X-ray peak of PSR J0108-1431 is offset from its radio peak by more than 0.1 in rotational phase, which the authors interpret as evidence for a multipolar surface magnetic field.
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Neutron Star Mass-Radius Constraints for EXO 0748$-$676 from 2008-2025 Quiescent X-ray Spectra
Joint MCMC analysis of Chandra and XMM-Newton quiescent spectra yields M = 1.77^{+0.17}_{-0.22} M_⊙ and R = 12.62^{+0.56}_{-0.74} km at 7.1 kpc, with conservative ranges 1.41-2.11 M_⊙ and 10.15-15.13 km when distance ...
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