  We numerically construct images of thin accretion disks in rotating wormhole
backgrounds, for the Kerr-like and the Teo class of wormholes. Our construction
is illustrated by two methods, a semi-analytic scheme where separated null
geodesic equations obtained by analytically integrating the second order
equations once are used, as well as by a numerical ray-tracing method utilizing
a fourth order Runge-Kutta algorithm. Our result shows dramatic differences
between accretion disk images in wormhole backgrounds, compared to black hole
ones, specifically because a wormhole can in principle have accretion disks on
both sides of its throat. We establish the nature of the images if the observer
and the disk are on two opposite sides of the throat, and show that these can
provide conclusive observational evidence of wormhole geometries.
