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In a cool neutron star (T < 1.e6 K) endowed with a rather high magnetic field(B > 1.e13 G), a phase transition may occur in the outermost layers. As aconsequence the neutron star becomes `bare', i.e. no gaseous atmosphere sits onthe top of the crust. The surface of a cooling, bare neutron star does notnecessarily emit a blackbody spectrum because the emissivity is stronglysuppressed at energies below the electron plasma frequency, omega_p. Sinceomega_p ~ 1 keV under the conditions typical of the denseelectron gas in thecondensate, the emission from a T ~ 100 eV bare neutron star will besubstantially depressed with respect to that of a perfect Planckian radiator atmost energies. Here we present a detailed analysis of the emission propertiesof a bare neutron star. In particular, we derive the surface emissivity for aFe composition in a range of magnetic fields and temperatures representative ofcooling isolated neutron stars, like RX J1856.5-3754. We find that the emittedspectrum is strongly dependent on the electron conductivity in the solidsurface layers. In the cold electron gas approximation (no electron-latticeinteractions), the spectrum turns out to be a featureless depressed blackbodyin the 0.1-2 keV band with a steeper low-energy distribution. When dampingeffects due to collisions between electrons and the ion lattice (mainly due toelectron-phonon interactions) are accounted for, the spectrum is more depresseddepending on the magnetic field strength. Details of the emitted spectrum arefound, however, to be strongly dependent of the assumed treatment of thetransition from the external vacuum to the metallic surface. The implicationsof out results to RX J1856.5-3754 and other isolated neutron stars arediscussed.Comment: 20 pages including 10 figures, Latex; corrected expressions for the  conductivities; accepted for publication in the Ap

Bare Quark Stars or Naked Neutron Stars? The Case of RX J1856.5−3754