论文标题
经过修订的形式主义，用于在一般相对论中缓慢旋转超级流体中子星
A revised formalism for slowly-rotating superfluid neutron stars in general relativity
论文作者
论文摘要
我们讨论了Hartle-Thorne公式中缓慢旋转，一般相对论的，超流体的中子星。恒星的组成是通过简单的两流体模型来描述的，该模型解释了超流体中子和所有其他成分。 We apply a perturbed matching framework to derive a new formalism for slowly-rotating superfluid neutron stars, valid up to second-order perturbation theory, building on the original formulation reported by Andersson and Comer in 2001. The present study constitutes an extension of previous work in the single-fluid case where it was shown that the Hartle-Thorne formalism needs to be amended since it does not provide the correct results when the energy density does not vanish在恒星的表面。我们详细讨论了需要应用于原始两流体形式主义的校正，以说明边界处的非消失能量密度。在此过程中，我们还发现在所有情况下，在原始两流体模型中恒星表面变形时需要进行校正（不论表面能量密度的值如何）。两种形式主义之间发现的差异是通过构建数值恒星模型来说明的，重点是在计算恒星质量的计算，恒星的变形以及旋转的开普勒极限中进行比较。特别是，使用一个玩具模式的状态方程，能量密度不会在恒星的边界上消失，我们证明了对形式主义的校正会影响缓慢旋转的超流体中子恒星的结构。
We discuss slowly-rotating, general relativistic, superfluid neutron stars in the Hartle-Thorne formulation. The composition of the stars is described by a simple two-fluid model which accounts for superfluid neutrons and all other constituents. We apply a perturbed matching framework to derive a new formalism for slowly-rotating superfluid neutron stars, valid up to second-order perturbation theory, building on the original formulation reported by Andersson and Comer in 2001. The present study constitutes an extension of previous work in the single-fluid case where it was shown that the Hartle-Thorne formalism needs to be amended since it does not provide the correct results when the energy density does not vanish at the surface of the star. We discuss in detail the corrections that need to be applied to the original two-fluid formalism in order to account for non vanishing energy densities at the boundary. In the process, we also find a correction needed in the computation of the deformation of the stellar surface in the original two-fluid model in all cases (irrespective of the value of the energy density at the surface). The discrepancies found between the two formalisms are illustrated by building numerical stellar models, focusing on the comparison in the calculation of the stellar mass, the deformation of the star, and in the Kepler limit of rotation. In particular, using a toy-model equation of state for which the energy density does not vanish at the boundary of the star we demonstrate that the corrections to the formalism we find impact the structure of slowly-rotating superfluid neutron stars in a significant way.
