论文标题
后期原始中子星中的磁场
Magnetic fields in late-stage proto-neutron stars
论文作者
论文摘要
我们探索后期原始中子星的热和磁场结构。我们发现恒星不同区域的熵的主要贡献，我们从中为热中子恒星构建了一个简化的状态方程。因此，我们通过数值求解恒星平衡方程，以找到一系列模型，包括磁场和旋转到开普勒速度。我们将状态方程近似为双向，并讨论该假设的有效性。对于固定的磁场强度，诱导的椭圆时随温度而增加。我们为此提供定量公式。对于较热的恒星，开普勒速度的速度大大降低，这可能会为非循环NSS的最大旋转速率设定为远低于1 kHz的最大旋转速率。在热中子和冷中子星中，磁场强于$ 10^{14} $ g在质量上具有相似的平衡状态，具有大规模的简单结构，并且在环形膜上占主导地位的poloidal场成分；我们认为这个结果可能是普遍的。我们表明，在低多物体处截短的磁场溶液会导致严重的不准确性，特别是对于具有快速旋转或强烈的环形场分量的模型而言。
We explore the thermal and magnetic-field structure of a late-stage proto-neutron star. We find the dominant contribution to the entropy in different regions of the star, from which we build a simplified equation of state for the hot neutron star. With this, we numerically solve the stellar equilibrium equations to find a range of models, including magnetic fields and rotation up to Keplerian velocity. We approximate the equation of state as a barotrope, and discuss the validity of this assumption. For fixed magnetic-field strength, the induced ellipticity increases with temperature; we give quantitative formulae for this. The Keplerian velocity is considerably lower for hotter stars, which may set a de-facto maximum rotation rate for non-recycled NSs well below 1 kHz. Magnetic fields stronger than around $10^{14}$ G have qualitatively similar equilibrium states in both hot and cold neutron stars, with large-scale simple structure and the poloidal field component dominating over the toroidal one; we argue this result may be universal. We show that truncating magnetic-field solutions at low multipoles leads to serious inaccuracies, especially for models with rapid rotation or a strong toroidal-field component.
