Einstein Observatory Limits on Neutron Star Surface Temperatures
نویسندگان
چکیده
منابع مشابه
Forecasting neutron star temperatures: predictability and variability.
It is now possible to model thermal relaxation of neutron stars after bouts of accretion during which the star is heated out of equilibrium by nuclear reactions in its crust. Major uncertainties in these models can be encapsulated in modest variations of a handful of control parameters that change the fiducial crustal thermal conductivity, specific heat, and heating rates. Observations of therm...
متن کاملElectrical Conductivity of the Neutron Star Crust at Low Temperatures
The electrical conductivity of the neutron star crust at low temperatures is calculated by taking into account the mixing of the electron wave functions due to the interaction with the crystal lattice of atomic nuclei. We show that the previously existed model of exponential reduction of the electron–ion scattering rate can lead to an overestimation of the electrical conductivity by several ord...
متن کاملBoundary layer on the surface of a neutron star
In an attempt to model the accretion on to a neutron star in low-mass X-ray binaries, we present 2D hydrodynamical models of the gas flow in close vicinity of the stellar surface. First, we consider a gas pressure-dominated case, assuming that the star is non-rotating. For the stellar mass we take Mstar = 1.4 × 10−2 M and for the gas temperature T = 5 × 106 K. Our results are qualitatively diff...
متن کاملNeutron Star Envelopes and Thermal Radiation from the Magnetic Surface
The thermal structure of neutron star envelopes is discussed with emphasis on analytic results. Recent progress on the effect of chemical constitution and high magnetic fields on the opacities and the thermal structure is further reviewed in view of the application to pulsar cooling and magnetars.
متن کاملSpot–like Structures of Neutron Star Surface Magnetic Fields
There is growing evidence, based on both X–ray and radio observations of isolated neutron stars, that besides the large–scale (dipolar) magnetic field, which determines the pulsar spin–down behaviour, small–scale poloidal field components are present, which have surface strengths one to two orders of magnitude larger than the dipolar component. We argue in this paper that the Hall–effect can be...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Symposium - International Astronomical Union
سال: 1987
ISSN: 0074-1809
DOI: 10.1017/s0074180900161194