General Relativistic magneto-hydrodynamical simulations of accretion flows through traversable wormholes

Abstract

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