2010 October 30'
title: Axisymmetric and stationary structures of magnetized barotropic stars with extremely strong magnetic fields deep inside
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stars: magnetic field – stars: neutron – stars: white dwarf

Introduction
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The magnetic field inside a star is scarcely detectable by direct observations but has been considered to affect stellar evolutions and activities in many aspects. For instance, if strong magnetic fields are hidden inside degenerate stars such as white dwarfs or neutron stars, they may significantly affect the cooling process of the stars by providing an energy reservoir or by modifying heat conduction. Highly localized, anisotropic and relatively strong magnetic field configurations, on the other hand, may affect accretion modes onto degenerate stars in close binary systems by providing a well-focused channel of accretion to their magnetic poles. In order to know the possible distributions and strengths of the magnetic fields inside the stars, we have to rely on theoretical studies. Until very recently, however, theoretical investigations could give us few hints about the interior magnetic fields. The reason for that may be twofold: one is related to the difficulty of the evolutionary computations of stellar magnetic fields and the other is related to the lack of methods 