Dark matter signatures of black holes with Yukawa potential

This study uses a nonsingular Yukawa–modified potential to obtain a static and spherically symmetric black hole solution with a cosmological constant. Such Yukawa–like corrections are encoded in two parameters, α and λ, that modify Newton’s law of gravity in large distances, and a deformation parameter ℓ0, which plays an essential role in short distances. The most significant effect is encoded in α, which modifies the total black hole mass with an extra mass proportional to αM, mimicking the dark matter effects at large distances from the black hole. On the other hand, the effect due to λ is small for astrophysical values. We scrutinize the quasinormal frequencies and shadows associated with a spherically symmetric black hole and the thermodynamical behavior influenced by the Yukawa potential. In particular, the thermodynamics of this black hole displays a rich behavior, including possible phase transitions. We use the WKB method to probe the quasinormal modes of massless scalar, electromagnetic, and gravitational field perturbations. In order to check the influence of the parameters on the shadow radius, we consider astrophysical data to determine their values, incorporating information on an optically thin radiating and infalling gas surrounding a black hole to model the black hole shadow image. In particular, we consider Sgr A* black hole as an example and we find that its shadow radius changes by order of 10−9, meaning that the shadow radius of a black hole with Yukawa potential practically gives rise to the same result encountered in the Schwarzschild black hole. Also, in the eikonal regime, using astrophysical data for Yukawa parameters, we show that the value of the real part of the QNMs frequencies changes by 10−18. Such Yukawa–like corrections are, therefore, difficult to measure by observations of gravitational waves using the current technology.