Accretion flows around exotic tidal wormholes I. Ray-tracing

Aims. This paper investigates the various spherically symmetric wormhole solutions in the presence of tidal forces and applies numerous methods, such as test particle orbital dynamics, ray-tracing, and microlensing. Methods. We make theoretical predictions on the test particle orbital motion around the tidal wormholes with the use of the effective potential normalized by Script capital L-2. In order to obtain the ray-tracing images of both geometrically thin and thick accretion disks and relativistic jets, we modified the open source GYOTO code using a python interface. Results. We applied this technique to probe the accretion flows near Schwarzschild-like and charged Reissner-Nordstrom (RN) wormholes; we assumed both a charged RN wormhole and a special case with a vanishing electromagnetic charge, namely the Damour-Solodukhin (DS) wormhole. We show that the photon sphere for the Schwarzschild-like wormhole present for both thin and thick accretion disks, even for the vanishing tidal forces. Moreover, we observe that r(ph) -> infinity as alpha -> infinity, which constraints the alpha parameter to be sufficiently small and positive in order to respect Event Horizon Telescope observations. On the other hand, for the case of the RN wormhole, the photon sphere radius shrinks as Lambda -> infinity, as predicted by the effective potential. In addition to the accretion disks, we also probe the relativistic jets around the two wormhole solutions under consideration. Finally, with the help of star bulb microlensing, we approximate the radius of the wormhole shadow and find that for the Schwarzschild wormhole, R-Sh approximate to r(0) for zero tidal forces and grows linearly with alpha. On the contrary, the shadow radius for charged wormholes slowly decreases with the growing DS parameter, Lambda.

Automated summary

This paper investigates various spherically symmetric wormhole solutions under the influence of tidal forces, and applies multiple methods for detection. Theoretical predictions are made on test particle orbital motion and ray-tracing images are obtained to analyze the results. The approximate radius of the wormhole shadow is also calculated using microlensing techniques.