J/ApJ/416/276 J/ApJ/416/276 Eq. of State in Magnetic Neutron Stars O E Rognvaldsson I Fushiki E H Gudmundsson C J Pethick J Yngvason Astrophys. J. 416 276 1993 1993ApJ...416..276R Atomic physics Models, evolutionary Stars, variable Landau levels stars: neutron Thomas-Fermi approximation This catalog is based on the calculated equation of state in cold dense matter. Each table in the catalog lists bulk properties of Fe-56 in a magnetic field ranging from one million to 1000 million Tesla.

We calculate the equation of state for cold dense matter in high magnetic fields in the Thomas-Fermi approximation, taking all Landau levels into account. Total energies and chemical potentials for atoms and matter are also calculated, and we present detailed profiles of the electron density as a function of the distance from the atomic nucleus for various values of the magnetic field strength and total matter density. The profiles show a Landau shell structure, which for iron atoms at low pressure is particularly pronounced for magnetic fields of order 10^11^ G. In compressed matter this structure is reflected in a high compressibility when the density is such that electrons at the boundary of a unit shell start to occupy a new Landau band. This leads to an oscillatory behavior of the density gradient as a function of depth in the surface layers of magnetic neutron stars.

density density of matter kg/m3 radius radius of cell m pressure pressure Pa eatom total energy of atom (in 1.602E-16J) keV chempot chemical potential (in 1.602E-16J) keV zg12 depth.(surface gravity)/(10^12 m/s^2) m N. Paul Kuin ADC 1996Jul09 J_ApJ_416_276.xml