We show that the expected inhomogeneous temperature distribution induced at the surface of a neutron star by the anisotropy of heat transport in the magnetized envelope allows us to understand quite well the observed pulse profiles of the four nearby pulsars for which surface thermal emission has ...
In principle, a neutron star can live "forever," as they're one of the final states of a massive star, a star corpse, if you will. However, if they have a binary companion, like another neutron star or black hole, they may merge eventually and create a black hole or a more massive...
[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 ...
To determine the detectability of thermal radiation from the surface of a neutron star, the surface temperature as a function of time is needed. To find this, the surface temperature as a function of core temperature is found; t...
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....
afewmilliseconds.MagneticfieldsareamplifieduptoB~109–1015G.(upto1012timestheaveragemagneticfieldofthesun)=>Rapidlypulsed(opticalandradio)emissionfromsomeobjectsinterpretedasspinperiodofneutronstars Pulsars/NeutronStars Neutronstarsurfacehasatemperatureof~1millionK.CasAinX-rays ...
We consider Joule heating caused by dissipation of the magnetic field in the neutron star crust. This mechanism may be efficient in maintaining a relatively high surface temperature in very old neutron stars. Calculations of the thermal evolution show that, at the late evolutionary stage (t >= ...
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 ...
We fit 9 years of archival Chandra ACIS spectra of the likely neutron star in the ~330 years old Cassiopeia A supernova remnant with our non-magnetic carbon atmosphere model. Our fits show a relative decline in the surface temperature by 4% (5.4 sigma, from 2.12+-0.01*10^6 K in 2000 ...
Abstract: We calculate the isospin chemical potential that is required for Beta equilibrium in nuclear matter under neutron star merger conditions, in the temperature range 1 MeV < T < 5 MeV. We improve on previous work by using a consistent description of nuclear matter based on the IUF and...