The timing of millisecond pulsars has long been used as an exquisitely precise tool for testing the building blocks of general relativity, including the strong equivalence principle and Lorentz symmetry. Observations of binary systems involving at least 1ms pulsar have been used to place bounds on the parameters of Einstein-ther theory, a gravitational theory that violates Lorentz symmetry at low energies via a preferred and dynamical time threading of the spacetime manifold. However, these studies did not cover the region of parameter space that is still viable after the recent bounds on the speed of gravitational waves from GW170817/GRB170817A. The restricted coverage was due to limitations in the methods used to compute the pulsar ‘sensitivities’, which parameterize violations of the strong-equivalence principle in these systems. We extend here the calculation of pulsar sensitivities to the parameter space of Einstein-ther theory that remains viable after GW170817/GRB170817A. We show that observations of the damping of the period of quasi-circular binary pulsars and of the triple system PSR J0337+1715 further constrain the viable parameter space by about an order of magnitude over previous constraints.

长期以来，毫秒脉冲星的计时一直被用作测试广义相对论构建模块的精密工具，包括强等效原理和洛伦兹对称性。对包含至少 1ms 脉冲星的双星系统的观测已被用于确定爱因斯坦理论参数的界限，这是一种引力理论，通过时空流形的首选和动态时间线程在低能量下违反洛伦兹对称性。然而，这些研究并没有涵盖在最近来自 GW170817/GRB170817A 的引力波速度的界限之后仍然可行的参数空间区域。有限的覆盖范围是由于用于计算脉冲星“灵敏度”的方法的限制，这些方法对这些系统中强等效原理的违反进行了参数化。我们在这里将脉冲星灵敏度的计算扩展到爱因斯坦理论的参数空间，该理论在 GW170817/GRB170817A 之后仍然有效。我们表明，对准圆形双星脉冲星和三重系统 PSR J0337+1715 的周期阻尼的观察进一步将可行参数空间限制在大约一个数量级以上。