标量-张量引力下的半解析恒星结构
Semi-Analytic Stellar Structure in Scalar-Tensor Gravity
摘要：
重力的精确测试可以用来约束假设的非常轻的标量场的性质，但是这些测试关键取决于宏观天体物理对象如何耦合到新的标量场。我们开发的准解析方法求解恒星结构方程使用标量张量引力，看到恒星的性质如何依赖于在微观水平上的标量耦合的假设的目标。我们通过将这些方法应用于Brans-Dicke标量来说明这些方法，以及它们的推广，其中标量-物质耦合是标量场的弱函数。表征球对称恒星外部场的四个可观测参数（恒星半径R、质量M、标量“电荷”Q和标量的渐近值phi_infty）由于与内部解匹配而服从两个关系，推广了广义相对论中通常的质量-半径关系M（R）。我们确定这些关系如何依赖于微观标量耦合，同意早期的工人时，比较是可能的。显式的解析解得到的启发性玩具模型的恒定密度的恒星，其属性，我们比较更现实的状态方程的中子星模型。
英文摘要：
Precision tests of gravity can be used to constrain the properties of hypothetical very light scalar fields, but these tests depend crucially on how macroscopic astrophysical objects couple to the new scalar field. We develop quasi-analytic methods for solving the equations of stellar structure using scalar-tensor gravity, with the goal of seeing how stellar properties depend on assumptions made about the scalar coupling at a microscopic level. We illustrate these methods by applying them to Brans-Dicke scalars, and their generalization in which the scalar-matter coupling is a weak function of the scalar field. The four observable parameters that characterize the fields external to a spherically symmetric star (the stellar radius, R, mass, M, scalar `charge', Q, and the scalar's asymptotic value, phi_infty) are subject to two relations because of the matching to the interior solution, generalizing the usual mass-radius, M(R), relation of General Relativity. We identify how these relations depend on the microscopic scalar couplings, agreeing with earlier workers when comparisons are possible. Explicit analytical solutions are obtained for the instructive toy model of constant-density stars, whose properties we compare to more realistic equations of state for neutron star models.
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