  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 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 magneto-rotational 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.
