2012/08/31 by A. Y. Potekhin, V. F. Suleimanov, M. van Adelsberg +1 · 1 citation
Physics and Astronomy · #Astrophysical Phenomena and Observations #Neutron star #Pulsars and Gravitational Waves Research #Radiation #Radiative transfer #Solar and Space Plasma Dynamics #Spectral line #Stars #Stellar atmosphere #Thermal #Thermal radiation #astro-ph.HE
paper · pdf · doi:10.1051/0004-6361/201219747
published as Astron. Astrophys. 546, A121 (2012) · 14 pages, 13 figures. In v.2, an error in Eq.(B12) and several typos are fixed
openalex publication_date 2012/09/17 · arxiv created 2016/02/15 · arxiv updated 2016/02/16 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Context. Simple models fail to describe the observed spectra of X-ray-dim isolated neutron stars (XDINSs). Interpretating these spectra requires detailed studies of radiative properties in the outermost layers of neutron stars with strong magnetic fields. Previous studies have shown that the strongly magnetized plasma in the outer envelopes of a neutron star may exhibit a phase transition to a condensed form. In this case thermal radiation can emerge directly from the metallic surface without going through a gaseous atmosphere, or alternatively, it may pass through a “thin” atmosphere above the surface. The multitude of theoretical possibilities complicates modeling the spectra and makes it desirable to have analytic formulae for constructing samples of models without going through computationally expensive, detailed calculations.