论文标题
大规模标量重力中的中子星的结构
Structure of neutron stars in massive scalar-tensor gravity
论文作者
论文摘要
我们在具有庞大的标量场的两衍生标量调整理论中计算了球形对称中子星模型的家族。我们提出的数值方法使我们能够使用压缩网格上的弛豫算法计算出所得的空间到无限半径。我们讨论了因此获得的中子星模型的虚弱和强烈标量的分支的结构，并依赖于该理论的标量和张量领域之间的线性和二次耦合参数$α_0$，$β_0$，以及标量质量$ $ $ $ $ $。对于$β_0$的高度负值，我们会遇到类似于“引力原子”的配置，该配置由一个高度紧凑的Baryon星星组成，该恒星被标量云包围。基于结合 - 内er计算的稳定性分析表明，这些配置是不稳定的，我们希望它们能够迁移到径向降低的baryon密度{\ it和}标量场强度的模型。
We compute families of spherically symmetric neutron-star models in two-derivative scalar-tensor theories of gravity with a massive scalar field. The numerical approach we present allows us to compute the resulting spacetimes out to infinite radius using a relaxation algorithm on a compactified grid. We discuss the structure of the weakly and strongly scalarized branches of neutron-star models thus obtained and their dependence on the linear and quadratic coupling parameters $α_0$, $β_0$ between the scalar and tensor sectors of the theory, as well as the scalar mass $μ$. For highly negative values of $β_0$, we encounter configurations resembling a "gravitational atom", consisting of a highly compact baryon star surrounded by a scalar cloud. A stability analysis based on binding-energ calculations suggests that these configurations are unstable and we expect them to migrate to models with radially decreasing baryon density {\it and} scalar field strength.
