Matter Accumulations and Accretion Tori around Wormholes

TL;DR

This paper investigates the properties of circular orbits and accretion disk structures around various symmetric wormhole solutions, revealing stable orbit regions and potential matter accumulations at the throat that could influence observational signatures.

Contribution

It introduces a detailed analysis of orbit spectra and accretion structures around three distinct wormhole spacetimes, highlighting the possibility of matter accumulation and its observational implications.

Findings

Existence of stable circular orbits at the wormhole throat.

Potential formation of matter accumulations at the throat.

Possible observational signatures resembling star-like objects.

Abstract

We study circular orbits and accretion structures around symmetric wormholes. As exemplary solutions we choose three different wormhole spacetimes, namely rotating traversable wormholes from the Teo class, the rotating Simpson-Visser metric with the parameter spectrum corresponding to wormholes and a static wormhole from beyond Horndeski theories. We show the existence of a spectrum of circular orbits at the wormhole throat for each of these wormhole solutions and analyze the boundaries of this spectrum across the respective wormhole parameter range. For each of the solutions we identified that vast regions of the parameter space correspond to stable orbits. The presence of this orbit spectrum can be linked through accretion disk models to matter accumulations which may form at the throat. We present here examples of such disk solutions by implementing the Polish Doughnut model. In some cases, these matter accumulations are encapsulating the throat and could imply central bright regions of the wormhole spacetime. Furthermore, the combined analysis of the equatorial Keplerian orbits and the throat orbits, leads to a set of different disk configurations, where matter accumulations at the throat may be present with outer tori around them, in some cases also as a connected structure. Our results may hint to possible instabilities of wormholes, especially if they have an ergoregion. Moreover, wormholes with such disks, may appear more star-like when it comes to their observational signature, due to the centralized and more spherical emission profile associated with the possible matter accumulations at the throat.