We present the first dynamical model of plasma accretion onto traversable wormholes by performing general relativistic magnetohydrodynamical (GRMHD) simulations of the flow on both sides of the wormhole. We evolve the ideal MHD equations on a wormhole spacetime described by the spherically symmetric Simpson-Visser metric. The disk is initialized on one side of the wormhole and accretes onto the throat driven by the magnetorotational instability (MRI). We show that the inflowing plasma quickly settles in the throat and forms a hot, rotating cloud. The wormhole cloud acts as an engine in which gas coming from one side accumulates at the center, dissipates energy, and powers a mildly relativistic thermal wind toward the other side. Our novel predictions show that accreting wormholes behave very differently from black holes (BHs) in astrophysical environments. In particular, one mouth presents outflows without accretion signatures, contradicting the jet-disk symbiotic relation that holds for black holes.

• Received 21 September 2023
• Accepted 18 April 2024

DOI:https://doi.org/10.1103/PhysRevD.109.103034