SMuK 2023 – wissenschaftliches Programm
Bereiche | Tage | Auswahl | Suche | Aktualisierungen | Downloads | Hilfe
T: Fachverband Teilchenphysik
T 70: Cosmic Ray III
T 70.2: Vortrag
Mittwoch, 22. März 2023, 16:05–16:20, POT/0013
3D modelling of the Galactic Center region — •Julien Dörner1,2, Julia Becker Tjus1,2, Paul-Simon Blomenkamp1,2, Horst Fichtner1,2, Anna Franckowiak1,2, Mario Hoerbe1,2, and Memo Zaninger1,2 — 1Ruhr-Universität Bochum, 44801 Bochum, Deutschland — 2RAPP-Center at Ruhr University Bochum, Bochum, Germany
The Galactic Center (GC) region is a unique astrophysical environment, which has been intensively studied in the past decades. In the HE and UHE gamma-ray regime several point like sources and a diffuse emission have been discovered. In addition, observation in the emission with FermiLAT show an excess, which may hint to a population of unresolved sources. The detection of the first PeVatron by H.E.S.S. indicates that cosmic-rays (CRs) can be accelerated up to PeV energies in the GC. While 3-D transport models for the entire Galaxy do exist in well-advanced states, the GC region in these global models is not well-represented and dedicated 3-D models of this region are missing. We present the first model using a realistic 3D distribution of the gas and the magnetic field for the Central Molecular Zone. The magnetic field is composed by a large-scale structure, as well as a contribution from several molecular clouds and non-thermal filaments. We use an anisotropic diffusion tensor defined by the ratio of the perpendicular and the parallel diffusion coefficient with respect to the local magnetic field direction. In the end, we compare our model with the observation by H.E.S.S. and calculate synthetic 2D count maps with predictions for the observability by CTA and for the expected neutrino flux.