  A core-collapse supernova releases the vast majority of the gravitational
binding energy of its compact remnant in the form of neutrinos over an interval
of a few tens of seconds. In the event of a core-collapse supernova within our
galaxy, multiple current and future neutrino detectors would see a large burst
in activity. Neutrinos escape a supernova hours before light does, so any
prompt information about the supernova's direction that can be inferred via the
neutrino signal will help to enable early electromagnetic observations of the
supernova. While there are methods to determine the direction via intrinsic
directionality of some neutrino-matter interaction channels, a complementary
method which will reach maturity with the next generation of large neutrino
detectors is the use of relative neutrino arrival times at different detectors
around the globe. To evaluate this triangulation method for realistic detector
configurations of the next few decades, we generate random supernova neutrino
signals with realistic detector assumptions, and quantify the error in expected
time delay between detections. We investigate a practical and robust method of
estimating the time differences between burst detections, also correcting for
detection efficiency bias. With this method, we determine the pointing
precision of supernova neutrino triangulation as a function of supernova
distance and location, detectors used, detector background level and neutrino
mass ordering assumption. Under favorable conditions, the 1$\sigma$ supernova
search area from triangulation could be reduced to a few percent of the sky. It
should be possible to implement this method with low latency under realistic
conditions.
