晚期原中子星的磁场
Magnetic fields in late-stage proto-neutron stars
摘要：
我们探讨了晚期原中子星的热结构和磁场结构。我们发现在恒星的不同区域的熵的主要贡献，从我们建立一个简化的状态方程的热中子星。有了这个，我们数值求解恒星平衡方程，找到一系列的模型，包括磁场和旋转到开普勒速度。我们近似状态方程作为一个正压，并讨论了这一假设的有效性。对于固定的磁场强度，感应椭圆率随温度的增加，我们给出了定量的公式。对于较热的恒星，开普勒速度要低得多，这可能会为非回收的NS设定一个事实上的最大旋转速率，远低于1 kHz。强于$10^{14}$ G周围的磁场在热中子星和冷中子星中子星中具有定性相似的平衡态，具有大尺度的简单结构，极向场分量在环向场分量上占主导地位，我们认为这一结果可能是普遍的。我们表明，截断磁场的解决方案在低多极导致严重的不准确性，特别是对于快速旋转或强环形场分量的模型。
英文摘要：
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.
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