The large-scale structure of Saturn's magnetosphere is determined by internal and external
factors, including the rapid planetary rotation rate, significant internal hot and cold plasma sources, and
varying solar wind pressure. Under certain conditions the dayside magnetospheric magnetic field changes
from a dipolar to more disk-like structure, due to global force balance being approximately maintained
during the reconfiguration. However, it is still not fully understood which factors dominantly influence
this behavior, and in particular how it varies with local time. We explore this in detail using a 2-D
force-balance model of Saturn's magnetodisk to describe the magnetosphere at different local time sectors.
For model inputs, we use recent observational results that suggest a significant local time asymmetry in
the pressure of the hot (>3 keV) plasma population, and magnetopause location. We make calculations
under different solar wind conditions, in order to investigate how these local time asymmetries influence
magnetospheric structure for different system sizes. We find significant day/night asymmetries in
the model magnetic field, consistent with recent empirical studies based on Cassini magnetometer
observations. We also find dawn-dusk asymmetries in equatorial current sheet thickness, with the varying
hot plasma content and magnetodisk radius having comparable influence on overall structure, depending
on external conditions. We also find significant variations in magnetic mapping between the ionosphere
and equatorial disk, and ring current intensity, with substantial enhancements in the night and dusk
sectors. These results have consequences for interpreting many magnetospheric phenomena that vary with
local time, such as reconnection events and auroral observations