Neutron starsDiffusionCoolingNear the surface of any neutron star there is a thin heat blanketing envelope that produces substantial thermal insulation of warm neutron star interiors and that relates the internal temperature of the star to its effective surface temperature. Physical processes in the ...
surface temperature and luminosity are related to their “actual” values byTse−ϕandLse2ϕ, respectively. Because the structure of the star is virtually independent of temperature, however, the redshift can be determined from the interior model and then included in the calculation of the ...
[17] If the surface temperature exceeds 106 kelvin (as in the case of a young pulsar), the surface should be fluid instead of the solid phase observed in cooler neutron stars (temperature <106 kelvins).[17] The "atmosphere" of the star is roughly one meter thick, and its dynamic is ...
In the case of radio pulsars, neutrons at the surface of the star decay into protons and electrons. As these charged particles are released from the surface, they enter the intense magnetic field that surrounds the star and rotates along with it. Accelerated to speeds approaching that of light...
Neutron stars can exist in isolation, only detectable by their surface temperature, or they can dwell in partnerships with "ordinary" stars, often siphoning off their material, or in some cases, they can exist in binary systems with another neutron star. ...
cooling scenarios involving fast neutrino emission, from a kaon or pion condensate, quark matter, or the direct Urca process, require the presence of baryon pairing in the central core of the star to control the strong neutrino emission and produce surface temperatures compatible with observations. ...
Particularly, the surface temperatures deduced from X-ray observations within the hydrogen atmosphere model are more consistent with the thermal history of neutron stars containing hyperons, if the critical temperature for the onset of lambda and nucleon pairing is not too small....
Others 3–5 have considered the possibility of accelerating particles by the electric field near the surface of the neutron star arising from nonzero E·B . High energy photons are also likely to be produced in association with these particles and these have been observed from the Crab pulsar....
THE ENERGY DEPENDENCE OF NEUTRON STAR SURFACE MODES AND X-RAY BURST OSCILLATIONSstars: neutronstars: oscillationsX-rays: burstsX-rays: starsWe calculate the photon energy dependence of the pulsed amplitude of neutron star (NS) surface modes. Simple approximations demonstrate that it depends most ...
(for example, on the location and properties of hotspots on the neutron-star surface, the rotation rate of the star, and its compactness, which determines the light bending around the pulsar). This information enables constraints on the pulsar’s mass and radius. In addition to NICER, the ...