论文标题
磁化密集富含中子物质的热力学
Thermodynamics of magnetized dense neutron-rich matter
论文作者
论文摘要
中子恒星是巨大恒星的可能终端状态之一。它被重力压缩，并通过核退化压力稳定。尽管有其名称，但这些对象的组成并不完全是清楚的。但是，从推断的密度来看，中子很可能会占恒星内部的很大一部分。虽然所有中子星有磁场，但某些中子星（“'Magnetar''）比具有推断的磁表面磁场的其他磁场要高得多，在$ 10^{14} $之间，至$ 10^{15} $高斯。尽管中子星是宏观物体，但由于恒星的能量，压力和磁场的极端值，微观尺度上的热力学可以印在恒星的大尺度行为上。这种贡献的重点是描述磁化密度中子物质的热力学，其状态方程并探索可能的铁磁状态的条件，磁化真空的贡献以及可能的观察意义。
A neutron star is one of the possible end states of a massive star. It is compressed by gravity and stabilized by the nuclear degeneracy pressure. Despite its name, the composition of these objects is not exactly known. However, from the inferred densities, neutrons will most likely compose a significant fraction of the star's interior. While all neutron stars are expected to have a magnetic field, some neutron stars (''magnetars'') are much more highly magnetized than others with inferred magnetar surface magnetic field is between $10^{14}$ to $10^{15}$ gauss. While neutron stars are macroscopic objects, due to the extreme value of the stars' energy, pressure, and magnetic field the thermodynamics on the microscopic scale can be imprinted on the star's large scale behaviour. This contribution focusses on describing the thermodynamics of magnetized dense neutron matter, its equation of state and to explore conditions of a possible ferromagnetic state, contributions from the magnetized vacuum, as well as possible observational implications.
