  Prolate rotation is characterized by a significant stellar rotation around a
galaxy's major axis, which contrasts with the more common oblate rotation.
Prolate rotation is thought to be due to major mergers and thus studies of
prolate-rotating systems can help us better understand the hierarchical process
of galaxy evolution. Dynamical studies of such galaxies are important to find
their gravitational potential profile, total mass, and dark matter fraction.
Recently, it has been shown in a cosmological simulation that it is possible to
form a prolate-rotating dwarf galaxy following a dwarf-dwarf merger event. The
simulation also shows that the unusual prolate rotation can be time enduring.
In this particular example, the galaxy continued to rotate around its major
axis for at least $7.4$\,Gyr (from the merger event until the end of the
simulation). In this project, we use mock observations of the hydro-dynamically
simulated prolate-rotating dwarf galaxy to fit various stages of its evolution
with Jeans dynamical models. The Jeans models successfully fit the early oblate
state before the major merger event, and also the late prolate stages of the
simulated galaxy, recovering its mass distribution, velocity dispersion, and
rotation profile. We also ran a prolate-rotating N-body simulation with similar
properties to the cosmologically simulated galaxy, which gradually loses its
angular momentum on a short time scale $\sim100$\,Myr. More tests are needed to
understand why prolate rotation is time enduring in the cosmological
simulation, but not in a simple N-body simulation.
