地面Sagnac延迟约束修正重力模型
Terrestrial Sagnac delay constraining modified gravity models
摘要：
修正的引力理论包括$f(\mathbf{R})-$引力模型，这些模型通常受到宇宙演化情景的约束。然而，最近的研究表明，它们也可以被常Ricci曲率Kerr- $f(\mathbf{R}_{0})$恒星大小的黑洞周围吸积盘的签名所约束。我们在这里的目的是使用另一个实验事实，即，地面Sagnac延迟以约束特定$f(\mathbf{R})-$重力规定的参数。我们假定Kerr- $f(\mathbf{R}_{0})$解渐近地描述了地球表面附近的弱引力。在这个时空中，我们将研究来自源/观察者的反向光束在非测地线和测地线圆形轨道上运动，并计算光束重新结合时的时间间隔。我们在这两种情况下得到了称为Sagnac延迟的\textit{exact }时间间隙，并将其扩展以显示如何通过Ricci曲率、引力源的质量和自旋来校正平坦空间值。在假设修正量的量级为延迟测量中剩余不确定性的量级的条件下，我们导出了Ricci曲率的允许区间。我们的结论是，地面Sagnac延迟可以用来限制特定的$f(\mathbf{R})$处方的参数。结果表明，尽管采用了近地表的弱场引力，模型的参数范围仍然与强场吸积盘现象的参数范围相同。
英文摘要：
Modified gravity theories include $f(\mathbf{R})-$gravity models that are usually constrained by the cosmological evolutionary scenario. However, it has been recently shown that they can also be constrained by the signatures of accretion disk around constant Ricci curvature Kerr-$f(\mathbf{R}_{0})$ stellar sized black holes. Our aim here is to use another experimental fact, viz., the terrestrial Sagnac delay to constrain the parameters of specific $f(\mathbf{R})-$gravity prescriptions. We shall assume that a Kerr-$f(\mathbf{R}_{0})$ solution asymptotically describes Earth's weak gravity near its surface. In this spacetime, we shall study oppositely directed light beams from source/observer moving on non-geodesic and geodesic circular trajectories and calculate the time gap, when the beams re-unite. We obtain the \textit{exact }time gap called Sagnac delay in both cases and expand it to show how the flat space value is corrected by the Ricci curvature, the mass and the spin of the gravitating source. Under the assumption that the magnitude of corrections are of the order of residual uncertainties in the delay measurement, we derive the allowed intervals for Ricci curvature. We conclude that the terrestrial Sagnac delay can be used to constrain the parameters of specific $f(\mathbf{R})$ prescriptions. Despite using the weak field gravity near Earth's surface, it turns out that the model parameter ranges still remain the same as those obtained from the strong field accretion disk phenomenon.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
