Thermal Emission from Neutron Stars with no Atmosphere

Details Thermal Emission from Neutron Stars with no Atmosphere Thermal Emission from Neutron Stars with no Atmosphere

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004head....8.3901z&link_type=abstract

American Astronomical Society, HEAD meeting #8, #39.01; Bulletin of the American Astronomical Society, Vol. 36, p.1204

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Scientific paper

In a cool neutron star (T < 106 K) endowed with a rather high magnetic field (B > 1013 G), a phase transition may occur in the outermost layers. As a consequence the neutron star becomes ``bare'', i.e. no gaseous atmosphere sits on the top of the crust. The surface of cooling, bare neutron stars not necessary gives off blackbody radiation because of the strong suppression in the emissivity at energies below the electron plasma frequency. Here we present a detailed analysis of the emission properties of a bare neutron star. We derive the surface emissivity for a Fe composition and we find that the emitted spectrum is strongly dependent on the electron conductivity in the solid surface layers. In the cold electron gas approximation (no electron-lattice interactions), the spectrum turns out to be a featureless depressed blackbody in the 0.1--2 keV band with a steeper low-energy distribution. When damping effects due to collisions between electrons and the ion lattice (mainly due to electron-phonons interactions) are accounted for, the spectrum is more depressed at low energies and spectral features may be present, depending on the magnetic field strength. The implications for RX J1856 and other isolated neutron stars are discussed.

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