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The transport of energetic particles such as Cosmic Rays is governed by theproperties of the plasma being traversed. While these properties are ratherpoorly known for galactic and interstellar plasmas due to the lack of in situmeasurements, the heliospheric plasma environment has been probed by spacecraftfor decades and provides a unique opportunity for testing transport theories.Of particular interest for the 3D heliospheric transport of energetic particlesare structures such as corotating interaction regions (CIRs), which, due tostrongly enhanced magnetic field strengths, turbulence, and associated shocks,can act as diffusion barriers on the one hand, but also as accelerators of lowenergy CRs on the other hand as well. In a two-fold series of papers weinvestigate these effects by modeling inner-heliospheric solar wind conditionswith a numerical magnetohydrodynamic (MHD) setup (this paper), which will serveas an input to a transport code employing a stochastic differential equation(SDE) approach (second paper). In this first paper we present results from 3DMHD simulations with our code CRONOS: for validation purposes we use analyticboundary conditions and compare with similar work by Pizzo. For a morerealistic modeling of solar wind conditions, boundary conditions derived fromsynoptic magnetograms via the Wang-Sheeley-Arge (WSA) model are utilized, wherethe potential field modeling is performed with a finite-difference approach(FDIPS) in contrast to the traditional spherical harmonics expansion oftenutilized in the WSA model. Our results are validated by comparing withmulti-spacecraft data for ecliptical (STEREO-A/B) and out-of-ecliptic (Ulysses)regions.

Cosmic Ray Transport in Heliospheric Magnetic Structures: I. Modeling Background Solar Wind Using the CRONOS MHD Code