Investigation of the Galactic Magnetic Field based on the Radio Emission from Pulsars

Abstract

To enable the study of the Galactic Magnetic Field, a fully-automated procedure is developed and implemented in python. The whole approach is focused on extracting physically relevant information efficiently from the ATNF catalogue. Obtained data is analysed on different length scales, notably with a ‘differential’ approach, to secure relevant information on the Galactic Magnetic Field's strength and structure. Pulsars are widely distributed in the Milky Way and thus allow to probe this large-scale magnetic field. The magnetic field strength of the large-scale field is found to be relatively low with B ≈ 0 − 2 μG. However, exceptions to this large-scale trend with significantly stronger magnetic fields are present as well. These are discussed, including their possible origin. In terms of structure, the applied methods support a spiral arm configuration of the large-scale field. This field is preferably aligned to the Galactic disk. Indication for reversals in the field are found but are largely limited by the sample size.