标题： 引力辐射在霍拉瓦引力中 显示英文标题

标题： Gravitational Radiation in Horava Gravity

摘要： 我们研究了自引力双星系统在Horava引力低能极限下的引力波辐射。 我们发现，对于牛顿源，广义相对论的能量损失公式预测已被修改：四极矩贡献发生了变化，部分原因是张量模式的传播速度不同；此外，由于额外的标量自由度，存在一个单极矩贡献。 偶极矩贡献仅在更高阶的后牛顿级数中出现。 我们利用这些发现，通过与双脉冲星观测到的辐射阻尼进行比较，来约束Horava引力的低能作用量。 即使这种比较并不完全合适——因为致密天体无法在后牛顿近似中描述——它仍提供了一个数量级的估计。 在后牛顿度规与广义相对论度规一致的极限下，我们的能量损失公式为低能Horava引力提供了最强的约束。 显示英文摘要

摘要： We study the radiation of gravitational waves by self-gravitating binary systems in the low-energy limit of Horava gravity. We find that the predictions for the energy-loss formula of General Relativity are modified already for Newtonian sources: the quadrupole contribution is altered, in part due to the different speed of propagation of the tensor modes; furthermore, there is a monopole contribution stemming from an extra scalar degree of freedom. A dipole contribution only appears at higher post-Newtonian order. We use these findings to constrain the low-energy action of Horava gravity by comparing them with the radiation damping observed for binary pulsars. Even if this comparison is not completely appropriate - since compact objects cannot be described within the post-Newtonian approximation - it represents an order of magnitude estimate. In the limit where the post-Newtonian metric coincides with that of General Relativity, our energy-loss formula provides the strongest constraints for Horava gravity at low-energies.