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Reliable identification of the origin of the high-energy non-thermal emissionfrom the Galactic Center (GC) is not achievable without adequate considerationof the ambient conditions such as the magnetic field configuration or gasdistribution. In a first step, we present a model that can explain the diffusegamma-ray emission as measured by H.E.S.S. for small longitudes in the GalacticCenter region but comes to grief with higher longitudes. The model is given viathe solution of a transport equation that allows for a radial dependency of themass distribution. In order to move from this semi-analytical approximationtoward a full understanding of the PeVatron signature, we present a new 3Danalytical model of the gas distribution in the Central Molecular Zone (CMZ).Furthermore, we derive for the first time a 3D model of the magnetic fieldconfiguration and strength in the CMZ, which is analytical and divergence-free.The model is built via a combination of a model for the diffuse inter-cloudmedium, local molecular clouds and non-thermal filaments at which localinformation are based on investigations from previous works and the moleculargas density. It can be shown that without an efficient longitudinal CRentrapment, a single source at the center does not facilely suffice the diffusegamma-ray detection. Further, we show that the new magnetic field model GBFD19is compatible with recent polarization data and has a significant impact on thelongitudinal profiles of CR propagation.

A Novel Analytical Model of the Magnetic Field Configuration in the Galactic Center Explaining the Diffuse Gamma-Ray Emission (ICRC-2019)