  The distribution and evolution of the magnetic field at the solar poles
through a solar cycle is an important parameter in understanding the solar
dynamo. The accurate observations of the polar magnetic flux is very
challenging from the ecliptic view, mainly due to (a) geometric foreshortening
which limits the spatial resolution, and (b) the oblique view of predominantly
vertical magnetic flux elements, which presents rather small line-of-sight
component of the magnetic field towards the ecliptic. Due to these effects the
polar magnetic flux is poorly measured. Depending upon the measurement
technique, longitudinal versus full vector field measurement, where the latter
is extremely sensitive to the SNR achieved and azimuth disamiguation problem,
the polar magnetic flux measurements could be underestimated or overestimated.
To estimate the extent of systematic errors in magetic flux measurements at the
solar poles due to aforementioned projection effects we use MHD simulations of
quiet sun network as a reference solar atmosphere. Using the numerical model of
the solar atmosphere we simulate the observations from the ecliptic as well as
from out-of-ecliptic vantage points, such as from a solar polar orbit at
various heliographic latitudes. Using these simulated observations we make an
assessment of the systematic errors in our measurements of the magnetic flux
due to projection effects and the extent of under- or over estimation. We
suggest that such effects could contribute to reported missing open magnetic
flux in the heliosphere and that the multi-viewpoint observations from
out-of-the-ecliptic plane together with innovative Compact Doppler
Magnetographs provide the best bet for the future measurements.
