论文标题
中子恒星中的fermions状态方程
Equation of state of fermions in neutron stars
论文作者
论文摘要
使用数量密度和能量密度，在存在各种统计效应的情况下得出了中子星的每个显微区域的费米状态方程。它根据中子星的统计特性和相应的阶段计算为温度（t），化学电位（μ）和磁场（b）的功能。据表明，描述中子星的动态行为的可测量特性取决于异常的统计条件。证明，在强磁场（B大于μ）中，压力（P）显示了对数对B（P与（μ/B）的对数成比例的对数（P）。发现具有较小（较长的）磁场的区域与较小的磁场之间的磁场相比，磁场较小，而磁场的较大磁场则是磁场的较大的磁场。在相同温度下的密度。
Employing both the number density and energy density, the equation of state of fermions for each microscopic region of a neutron star is derived in the presence of various statistical effects. It is computed as functions of temperature (T), chemical potential (μ) and magnetic field (B) based on the statistical properties and corresponding phases of neutron stars. It is revealed that the measurable properties describing the dynamic behavior of a neutron star are determined by the unusual statistical conditions. It is demonstrated that, in a strong magnetic field (B larger thanμ), the pressure (P) shows a logarithmic dependence on B (P is proportional to logarithm of(μ/B). It is found that the regions with a higher (lower) magnetic field (density) have a shorter (longer) life time. Moreover, the relationship between the magnetic field and chemical potential confirms that the large magnetic field and high density are short lived as compared to low magnetic field and low density at the same temperature.
