A peer-reviewed theoretical study calculated how intense magnetic fields and chemical composition change the structure of dense white dwarfs. Some modeled stars became smaller while maximum masses shifted less substantially. The work treats pressure along and across the field differently within an approximately spherical model, rather than reporting a newly observed compact star.
Calculations of dense white dwarfs produced smaller radii in some sequences when magnetic pressure was allowed to vary with direction. Maximum masses changed less substantially. The European Physical Journal C published the peer-reviewed theoretical analysis on 6 November. White dwarfs are compact stellar remnants, and the new work examines their internal balance through equations for matter and gravity rather than through new telescope observations.[1]
A strong magnetic field restricts electron energies to discrete Landau levels. In some density ranges, pressure across the field can then differ from pressure along it. The researchers incorporated the electrical contribution of the crystal lattice and the constraints that electron capture places on composition at increasing density. They compared carbon, oxygen, neon and magnesium, as well as selected fixed mixtures, to track how composition affected the calculated stellar sequences.[1]
The effective model keeps spherical symmetry while incorporating directional pressure. It therefore approximates the geometry of a magnetized star. Fixed mixtures were not evolved through a complete reaction network. The mass–radius curves occupy the broad region of some published stellar estimates, but were not statistically fitted to those observations. A check of mass against central density also screens the modeled sequences without supplying a full calculation of dynamical stability.[1]
