  Understanding the large-scale three-dimensional structure of the inner
heliosphere, while important in its own right, is crucial for space weather
applications, such as forecasting the time of arrival and propagation of
coronal mass ejections (CMEs). This study uses sunRunner3D (3D), a 3-D
magnetohydrodynamic (MHD) model, to simulate solar wind (SW) streams and
generate background states. SR3D employs the boundary conditions generated by
CORona-HELiosphere (CORHEL) and the PLUTO code to compute the plasma properties
of the SW with the MHD approximation up to 1.1 AU in the inner heliosphere. We
demonstrate that SR3D reproduces global features of Corotating Interaction
Regions (CIRs) observed by Earth-based spacecraft (OMNI) and the Solar
TErrestial RElations Observatory (STEREO)-A for a set of Carrington rotations
(CRs) that cover a period that lays in the late declining phase of solar cycle
24. Additionally, we demonstrate that the model solutions are valid in the
corotating and inertial frames of references. Moreover, a comparison between
SR3D simulations and in-situ measurements shows reasonable agreement with the
observations, and our results are comparable to those achieved by Predictive
Science Inc.'s Magnetohydrodynamic Algorithm outside a Sphere (MAS) code. We
have also undertaken a comparative analysis with the Space Weather Adaptive
Simulation Framework for Solar Wind (SWASTi-SW), a PLUTO physics-based model,
to evaluate the precision of various initial boundary conditions. Finally, we
discuss the disparities in the solutions derived from inertial and rotating
frames.
