The complete set of five Earth Orientation Parameters (EOP) can only be estimated accurately using geodetic Very Long Baseline Interferometry (VLBI). Their precision and accuracy depends on network geometry and station-dependent properties. Atmospheric turbulence poses one of the largest error sources for geodetic VLBI, impacting the precision of EOP. Thus, it becomes imperative to consider this factor while choosing the optimal locations for geodetic VLBI. The magnitude of tropospheric turbulence is approximated through the refractive index structure constant, \(C_\textrm{n}^\textrm{2}\). In this study, we simulate the optimal locations for geodetic VLBI in India, considering individual tropospheric turbulence parameters per telescope location. The study identifies 14 potential VLBI stations, co-located with GPS stations and homogeneously distributed all over India, and computes the \(C_\textrm{n}\) values from zenith wet delay variances over 24 h obtained from GPS data. These locations are simulated in addition to three different reference networks, which show the current and future VLBI Global Observing System (VGOS) networks. Multiple schedules have been generated and simulated for each configuration using VieSched++, and the precision of EOP is compared when constant and station-specific tropospheric turbulence parameters are used. The study shows that, for the investigated networks, southern stations are optimal for polar motion and celestial pole offsets estimation, whereas an eastern station is optimal for UT1−UTC estimation. Furthermore, the study highlights that for reference networks with fewer stations, utilizing station-specific \(C_\textrm{n}\) values significantly influences the determination of optimal locations. It further demonstrates how station-specific \(C_\textrm{n}\) values impact the positioning of VGOS telescopes in each network for each EOP differently. The findings show that higher \(C_\textrm{n}\) values generally lead to a degradation in EOP precision. Geometrically, a station might be at a good location, but if the \(C_\textrm{n}\) value is too high, that location is not favorable.

完整的五个地球方向参数 （EOP） 只能使用大地测量甚长基线干涉测量法 （VLBI） 进行准确估计。它们的精度和准确度取决于网络几何和与测站相关的属性。大气湍流是大地测量 VLBI 的最大误差源之一，影响了 EOP 的精度。因此，在为大地测量 VLBI 选择最佳位置时，必须考虑这一因素。对流层湍流的大小通过折射率结构常数 \（C_\textrm{n}^\textrm{2}\） 来近似计算。在这项研究中，我们模拟了印度大地测量 VLBI 的最佳位置，考虑了每个望远镜位置的单个对流层湍流参数。该研究确定了 14 个潜在的 VLBI 站，与 GPS 站位于同一位置，均匀分布在印度各地，并根据从 GPS 数据获得的 24 小时内的天顶湿延迟方差计算 \（C_\textrm{n}\） 值。除了三个不同的参考网络之外，还模拟了这些位置，这些参考网络显示了当前和未来的 VLBI 全球观测系统 （VGOS） 网络。使用 VieSched++ 为每个配置生成和模拟了多个计划，并在使用常数和特定站点的对流层湍流参数时比较了 EOP 的精度。研究表明，对于所研究的网络，南部站最适合极地运动和天极偏移估计，而东部站最适合 UT1−UTC 估计。此外，该研究强调，对于站点较少的参考网络，使用特定于站点的 \（C_\textrm{n}\） 值会显著影响最佳位置的确定。 它进一步演示了特定于站点的 \（C_\textrm{n}\） 值如何以不同的方式影响每个 EOP 中每个网络中 VGOS 望远镜的定位。研究结果表明，较高的 \（C_\textrm{n}\） 值通常会导致 EOP 精度的下降。从几何学上讲，一个车站可能位于一个不错的位置，但如果 \（C_\textrm{n}\） 值太高，则该位置就不利。