Using relativistic mean-field models, the formation of clusterized matter, as the one expected to exist in the inner crust of neutron stars, is determined under the effect of strong magnetic fields. As already predicted from a calculation of the unstable modes resulting from density fluctuations at subsaturation densities, we confirm in the present work that for magnetic field intensities of the order of \(\approx 5\times 10^{16}\) G to \(5\times 10^{17}\) G, pasta phases may occur for densities well above the zero-field crust-core transition density. This confirms that the extension of the crust may be larger than expected. It is also verified that the equilibrium structure of the clusterized matter is very sensitive to the intensity of the magnetic fields. As a result, the decay of the magnetic field may give rise to internal stresses which may result on the yield and fracture of the inner crust lattice.

使用相对论平均场模型，在强磁场的作用下确定了中子星内壳中预期存在的团簇物质的形成。正如已经从不饱和密度下的密度波动导致的不稳定模式的计算中预测的那样，我们在目前的工作中确认，对于\(\approx 5\times 10^{16}\) G 到\ (5\乘以 10^{17}\)G，对于远高于零场地壳核转变密度的密度，可能会出现面食阶段。这证实了地壳的延伸可能比预期的要大。也证实了团簇物质的平衡结构对磁场强度非常敏感。因此，磁场的衰减可能会产生内应力，从而导致内地壳晶格的屈服和断裂。