https://doi.org/10.1140/epjc/s10052-025-14266-y
Regular Article - Theoretical Physics
AdS black strings in a cosmic web: geodesics, shadows, and thermodynamics
1
Department of Physics, The Assam Royal Global University, 781035, Guwahati, Assam, India
2
Department of Physics, Al-Hussein Bin Talal University, 71111, Ma’an, Jordan
3
Physics Department, Eastern Mediterranean University, North Cyprus via Mersin 10, 99628, Famagusta, Turkey
Received:
16
March
2025
Accepted:
2
May
2025
Published online:
19
May
2025
In a recent article (Deglmann et al. in Ann Phys (NY) 475:169948, 2025), the authors obtained a static, cylindrically symmetric Anti-de Sitter (AdS) black string (BS) solutions, which are cylindrical generalizations of black holes (BHs), surrounded by a cloud of strings (CS) and the quintessence field (QF), and discussed its properties. In the present study, we present a comprehensive analysis of cylindrically symmetric AdS BSs surrounded by CS and QF. Our analysis yields several significant results. We demonstrate that the presence of CS (parameter 
) and QF (parameters c and w) reduces the radius of circular photon orbits (CPO) and BH shadow size, with measurements constrained by Event Horizon Telescope (EHT) observations of Sagittarius A*. We find that time-like particle orbits show increased energy with higher and c values. We calculate that C-energy, representing gravitational energy within cylindrical radius, decreases with radial distance but exhibits distinct responses to CS and QF parameters. We observe that scalar perturbation potential increases r for specific and c values, indicating stronger field-spacetime interactions away from the BS. We determine that Hawking temperature increases linearly with Schwarzschild radius, with parameter-dependent behavior varying based on QF state parameter w. These results demonstrate how CS and QF significantly modify the geodesic, perturbative, and thermodynamic properties of AdS BS, with potential observational implications for gravitational lensing, accretion disk dynamics, and BH evaporation signatures in future astronomical observations.
© The Author(s) 2025
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