ИСТИНА

We present a promising detailed strategy for the wormhole (WH) search by astronomical observations. By determining the cumulative effect of an additional acceleration on a component of an astrophysical system, one can hypothesize about the hidden nature of a black hole (BH) as a candidate for a WH. We estimated an upper limit on this effect for several stars in known systems containing BH, such as S2 and S62, which orbit Sgr A*; additionally, we model a synthetic system consisting of a traversable WH, a star on our side, and a perturber located on the opposite side of the WH throat. We also examine recently discovered objects from the Gaia catalog: Gaia BH1, BH2, and BH3. For all types of systems, it is demonstrated that in a simple model of a traversable Schwarzschild WH, a perturbing object (star) located on the opposite side of the WH throat is capable of causing a significant anomalous acceleration on the object (star) observed on our side. Furthermore, we show that for stars located in the center of our Galaxy, this effect predominates over major competing effects, such as perturbations from surrounding stars and dark matter halo. The magnitude of the anomalous acceleration estimated for real objects ranges from 10^{-4} to 10^{-2} cm/s^2 (for typical distances of the order of 500 pc), which -- given future enhancements in observational precision -- will allow the detection of the desired effect. We present the precision of determining the acceleration of a star at the pericenter of a binary system within the astrometric project Gaia, calculated as a function of observational errors related to the parameters of the binary system (masses of each component, eccentricity of the orbit, period) as of 2024. The achieved precision estimate is already comparable to the predicted values of the sought effect. In the considered synthetic systems, with optimal parameter selection, the anomalous acceleration can reach 1.5 cm/s^2, making this effect significantly relevant for the search for WH in our Galaxy.