Ellis-Bronnikov Wormhole Shadows with Spherically Symmetric Accretion Flow
Abstract
We investigate the observational differences between the Ellis--Bronnikov (EB) wormhole and the Schwarzschild black hole (BH) by performing general relativistic radiative transfer (GRRT) simulations. We consider a spherically symmetric steady-state accretion flow and perform GRRT simulations incorporating synchrotron emission. For both the EB wormhole and the Schwarzschild BH, the simulated images consist of a central shadow region and a bright photon ring. We find that both the shadow region and the photon ring of the EB wormhole are brighter than those of the Schwarzschild BH. These differences arise from the absence of an event horizon in the EB wormhole, allowing the emission from the accreting matter around and beyond the throat to contribute to the intensity. We also compare the simulated images with the Event Horizon Telescope (EHT) observations of M87*. Although the total flux and the ring diameter are comparable with the EHT results, our models with the spherically symmetric accretion flow cannot reproduce the deep central brightness depression observed by the EHT, for both the EB wormhole and the Schwarzschild BH. This indicates that a non-spherical accretion flow is required for a detailed comparison with the EHT image.
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BibTeX
@misc{takahashi2026ellisbronnikov,
title = {{Ellis-Bronnikov Wormhole Shadows with Spherically Symmetric Accretion Flow}},
author = {Mikiya M. Takahashi and Keisuke Nakashi},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2606.01699},
eprint = {2606.01699},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2606.01699},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Ellis-Bronnikov Wormhole Shadows with Spherically Symmetric Accretion Flow
AU - Mikiya M. Takahashi
AU - Keisuke Nakashi
PY - 2026
DA - 2026/10/21
PB - arXiv
DO - 10.48550/arxiv.2606.01699
UR - https://arxiv.org/abs/2606.01699
AB - We investigate the observational differences between the Ellis--Bronnikov (EB) wormhole and the Schwarzschild black hole (BH) by performing general relativistic radiative transfer (GRRT) simulations. We consider a spherically symmetric steady-state accretion flow and perform GRRT simulations incorporating synchrotron emission. For both the EB wormhole and the Schwarzschild BH, the simulated images consist of a central shadow region and a bright photon ring. We find that both the shadow region and the photon ring of the EB wormhole are brighter than those of the Schwarzschild BH. These differences arise from the absence of an event horizon in the EB wormhole, allowing the emission from the accreting matter around and beyond the throat to contribute to the intensity. We also compare the simulated images with the Event Horizon Telescope (EHT) observations of M87*. Although the total flux and the ring diameter are comparable with the EHT results, our models with the spherically symmetric accretion flow cannot reproduce the deep central brightness depression observed by the EHT, for both the EB wormhole and the Schwarzschild BH. This indicates that a non-spherical accretion flow is required for a detailed comparison with the EHT image.
ER -