Abstract:
In this work, we investigate the optical appearance of qualitatively new observational features
of accretion disk images around the charged rotating traversable wormhole (TWH)
space-time for different spin, throat, and charge values. To accomplish this, we first consider
the Hamilton-Jacobi method to derive the geodesic equations for the motion of photons
and study the effects of parameters on the photon orbit in the observer’s sky. We found
that each parameter affects the size and shape of the wormhole (WH) shadow and flatness
is observed in the shadow because of spin and other parameters. To produce shadow images
of sufficient visual quality but within manageable computational times, we adopt the
ray-trace procedure and characterize the significant features of light trajectories on the observer’s
screen, depending on the interaction between the space-time structure and the accretion
disk. In addition, we consider the static spherically symmetric accretion flow model
to observe the specific intensity around the TWH space-time geometry. It is found that the
intensity and positions of the photon ring vary with respect to the involved parameters. In
future observation, this type of study may provide a fertile playground to test the nature of
compact objects, specifically the WH in the strong-field regime.
