  Mapping of magnetic field lines is important for studies of the solar wind
and the sources and propagation of energetic particles between the Sun and
observers. A recently developed mapping approach is generalised to use a more
advanced solar wind model that includes the effects of solar wind acceleration,
non-radial intrinsic magnetic fields and flows at the source surface/inner
boundary, and conservation of angular momentum. The field lines are mapped by
stepping along local magnetic field $\bm{B}$ and via a Runge-Kutta algorithm,
leading to essentially identical maps. The new model's maps for Carrington
rotation CR 1895 near solar minimum (19 April to 15 May 1995) and a solar
rotation between CR 2145 and CR 2146 near solar maximum (14 January to 9
February 2014) are compared with the published maps for a constant solar wind
model. The two maps are very similar on a large scale near both solar minimum
and solar maximum, meaning that the field line orientations, winding angles,
and connectivity generally agree very well. However, close inspection shows
that the field lines have notable small-scale structural differences. An
interpretation is that inclusion of the acceleration and intrinsic azimuthal
velocity has significant effects on the local structure of the magnetic field
lines. Interestingly, the field lines are more azimuthal for the accelerating
solar wind model for both intervals. In addition, predictions for the pitch
angle distributions (PADs) for suprathermal electrons agree at the $90$ --
$95\%$ level with observations for both solar wind models for both intervals.
