  Aims: Our aim is to build upon the analysis presented in our previous work by
attempting to match the observational data obtained with VLTI GRAVITY for RU
Lup in 2021 with an expanded radiative transfer model of Br$\gamma$ emission.
Specifically, we will determine if the inclusion of an additional disk wind as
a Br$\gamma$ emitter in the inner disk will be able to reproduce the trend of
increasing sizes at higher velocities, as well as the observed photocenter
shifts.
  Methods: We make use of the MCFOST radiative transfer code to solve for
Br$\gamma$ line formation in the innermost disk of an RU Lupl-like system. From
the resulting images we compute synthetic interferometric observables. We first
investigate how individual parameter variations in a pure magnetospheric
accretion model and a pure parameteric disk wind model translate to changes in
these derived quantities. Then we attempt to reproduce the RU Lup GRAVITY data
with different parameter variants of magnetospheric accretion models, disk wind
models, and combined hybrid models.
  Results: We demonstrate that magnetospheric accretion models and disk wind
models on their own can emulate certain individual characteristics from the
observational results, but individually fail to comprehensively reproduce the
observational trends. Disk wind plus accretion hybrid models are in principle
capable of explaining the variation in characteristic radii across the line and
the corresponding flux ratios. While the model parameters of the hybrid models
are mostly in good agreement with the known attributes of RU Lup, we find that
our best-fitting models deviate in terms of rotational period and the size of
the magnetosphere. The best-fitting hybrid model does not respect the
co-rotation criterion, as the magnetospheric truncation radius is about 50%
larger than the co-rotation radius.
