  The nature of the emission region around Sagittarius A* (Sgr A*), the
supermassive black hole at the Galactic Center, remains under debate. A
prediction of jet models is that a frequency-dependent shift in the position of
the radio core (core-shift) of active galactic nucleii occurs when observing
emission dominated by a highly collimated relativistic outflow. We use
millimeter Very Long Baseline Interferometry to study the frequency-dependent
position of Sgr A*'s radio core, estimate the core-shift for different emission
models, investigate the core-shift evolution as a function of viewing angle and
orientation, and study its behaviour in the presence of interstellar
scattering. We simulate images of the emission around Sgr A* for accretion
inflow models (disks) and relativistic outflow models (jets). They are based on
three-dimensional general relativistic magnetohydrodynamic simulations. We
create flux density maps at 22, 43 and 86 GHz sampling different viewing angles
and orientations, and examine the effects of scattering. Jet-dominated models
show significantly larger core-shifts (in some cases by a factor of 16) than
disk-dominated models, intermediate viewing angles (i=30, 45 degrees) show the
largest core-shifts. Our jet models follow a power-law relation for the
frequency dependent position of Sgr A*'s core. Their core-shifts decrease as
the position angle increases from 0 to 90 degrees. Disk models do not fit well
a power-law relation and their core-shifts are insensitive to changes in
viewing angle. We place an upper limit of 241.65 +-1.93 microarcseconds per cm
for the core-shift of jet models including refractive scattering. Our jet
models agree with earlier predictions of AGN with conical jets, and the
core-shift is retrievable even in the presence of interstellar scattering.
