强磁场下原中子星的内部组成
The internal composition of proto-neutron stars under strong magnetic fields
摘要：
本文研究了磁场和自转对原中子星结构和组成的影响。本文将强子手征SU（3）模型应用于冷中子星（NS）和具有捕获中微子的原中子星，并在每个重子的熵固定的情况下进行了讨论。通过自洽求解Einstein-Maxwell场方程，得到了具有极向磁场的中子星和原中子星的广义相对论解。随着中微子化学势随时间的推移而减小，这会改变恒星内部的化学平衡和成分，导致这些物体的结构和粒子数量发生变化。我们发现，磁场变形的恒星和显着改变的数量被困在恒星内部的中微子，以及奇怪的内容和温度在每个演化阶段。
英文摘要：
In this work, we study the effects of magnetic fields and rotation on the structure and composition of proto-neutron stars (PNS's). A hadronic chiral SU(3) model is applied to cold neutron stars (NS) and proto-neutron stars with trapped neutrinos and at fixed entropy per baryon. We obtain general relativistic solutions for neutron and proto-neutron stars endowed with a poloidal magnetic field by solving Einstein-Maxwell field equations in a self-consistent way. As the neutrino chemical potential decreases in value over time, this alters the chemical equilibrium and the composition inside the star, leading to a change in the structure and in the particle population of these objects. We find that the magnetic field deforms the star and significantly alters the number of trapped neutrinos in the stellar interior, together with strangeness content and temperature in each evolution stage.
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