In this work, we study magnetic field effects on neutron star matter containing the baryon octet and additional heavier spin 3/2 baryons (the \(\varDelta \)’s). We make use of two different relativistic hadronic models that contain an additional vector-isovector self interaction for the mesons: one version of a relativistic mean field (RMF) model and the chiral mean field (CMF) model. We find that both the additional interaction and a strong magnetic field enhance the \(\varDelta \) baryon population in dense matter, while decreasing the relative density of hyperons. At the same time that the vector-isovector meson interaction modifies neutron-star masses very little (\(<0.1~\mathrm M_{\mathrm{Sun}}\)), it decreases their radii considerably, allowing both models to be in better agreement with observations. Together, these features indicate that magnetic neutron stars are likely to contain \(\varDelta \) baryons in their interior.

在这项工作中，我们研究了磁场对包含重子八位组和额外的较重自旋 3/2 重子（\(\varDelta \) 's）的中子星物质的影响。我们使用两种不同的相对论强子模型，其中包含介子的额外矢量-等矢量自相互作用：相对论平均场 (RMF) 模型和手征平均场 (CMF) 模型的一个版本。我们发现额外的相互作用和强磁场都增强了致密物质中的\(\varDelta \)重子种群，同时降低了超子的相对密度。同时矢量-等矢量介子相互作用对中子星质量的影响很小（\(<0.1~\mathrm M_{\mathrm{Sun}}\))，它大大减少了它们的半径，使两个模型与观察结果更加一致。总之，这些特征表明磁性中子星的内部很可能包含\(\varDelta \)重子。