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We present numerical calculations of the equation of state for dense matterin high magnetic fields, using a temperature dependent Thomas-Fermi theory witha magnetic field that takes all Landau levels into account. Free energies foratoms and matter are also calculated as well as profiles of the electrondensity as a function of distance from the atomic nucleus for representativevalues of the magnetic field strength, total matter density, and temperature.The Landau shell structure, which is so prominent in cold dense matter in highmagnetic fields, is still clearly present at finite temperature as long as itis less than approximately one tenth of the cyclotron energy. This structure isreflected in an oscillatory behaviour of the equation of state and otherthermodynamic properties of dense matter and hence also in profiles of thedensity and pressure as functions of depth in the surface layers of magneticneutron stars. These oscillations are completely smoothed out by thermaleffects at temperatures of the order of the cyclotron energy or higher.Comment: 37 pages, 17 figures included, submitted to Ap

Thomas‐Fermi Calculations of Atoms and Matter in Magnetic Neutron Stars. II. Finite Temperature Effects