Neutron stars accreting matter from low-mass binary companions are observed to undergo bursts of X-rays due to the thermonuclear explosion of material on the neutron star surface. We use recent results on superfluid and superconducting properties to show that the core temperature in these neutron ...
the core of any star is incredibly hot and dense. The temperature in the core of the Sun is 15 million °C (27 million °F). The pressure and temperature are so great that hydrogen atoms are crushed together to form helium atoms. This process of combining small atoms to create larger ...
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...
We study the effects of temperature on the magnetic field of neutron star under relativistic mean field theory. The field is produced under the assumption that the photon has gained its mass in dense nuclear matters. We have computed the field at several temperatures and get a right order of ...
hyperons and mesons system at finite temperature(T=20 MeV).It's found that the different effective interactions give us different descriptions of neutron star.The results of DDME1 and TW99 have little odds,they both give the stronger meson field potential,the smaller hyperon transition density,...
To eventually become a neutron star, this white dwarf would have to exceed what is known as theChandrasekhar limit, which is generally considered to be 1.4solar masses , according toThe SAO Encyclopedia of Astronomy. That means that the core of the sun alone would have to have 1.4 times ...
We analyse the effect of neutron superfluidity on the cooling time of inner crust matter in neutron stars, in the case of a rapid cooling of the core. The specific heat of the inner crust, which determines the thermal response of the crust, is calculated in the framework of HFB approach ...
Discovery of a correlation between the frequency of the mHz quasi-periodic oscillations and the neutron-star temperature in the low-mass X-ray binary 4U 16... Discovery of a correlation between the frequency of the mHz quasi-periodic oscillations and the neutron-star temperature in the low-mass...
We found that the neutron star equation of state (EOS) with hyperons can be consistent with both mass and temperature observations. We also found that the neutron star EOS with kaon condensation can be consistent with observations, even though the cooling behavior is seldom useful to identify ...
Neutrino trapping inhibits the appearance of a mixed phase which leads to possible proto-neutron star metastability. We also demonstrate that the temperature along adiabats in the quark-hadron mixed phase is much smaller than what is found for the kaon condensate-hadron mixed phase. This could ...