Abstract
We discuss the global modeling of the properties of the Galactic Magnetic Field (GMF). Several improvements and variations of the model of the GMF from Jansson & Farrar (2012) (JF12) are investigated in an analysis constrained by all-sky rotation measures of extragalactic sources and polarized and unpolarized synchrotron emission data from WMAP and Planck. We present the impact of the investigated model variations on the propagation of ultrahigh-energy cosmic rays in the Galaxy
Highlights
Magnetic fields are a major constituent of the interstellar medium of galaxies
The most complete attempt to determine the global structure of the Galactic magnetic field (GMF) from these observations is the model of Jansson & Farrar [4, 5] (JF12)
The density and spectrum of cosmic-ray electrons depends in two ways on the Galactic magnetic field: Firstly, the GMF determines the diffusion of the electrons from their sources through the Galaxy and, secondly, synchrotron losses in the GMF are the main cause of electron cooling apart from inverse Compton scattering above ∼ 10 GeV
Summary
Magnetic fields are a major constituent of the interstellar medium of galaxies. Their energy density in the Galactic plane is about 0.6 eV/cm for a typical total magnetic field strength of 5 μG and comparable to the energy density of cosmic rays (0.8-1.0 eV/cm3 [1]) and interstellar radiation fields (star light and CMB, each contributing about 0.25 eV/cm). The total polarized intensity (PI) is proportional to the integral of the ordered component of the magnetic field perpendicular to the line of sight and weighted by the density of cosmic-ray electrons. The most complete attempt to determine the global structure of the Galactic magnetic field (GMF) from these observations is the model of Jansson & Farrar [4, 5] (JF12). In this model, the GMF is described by a superposition of three divergence-free large-scale regular components: a spiral disk field, a toroidal halo field and a poloidal field (“X-field”). Further information about the model fitting and calculation of simulated sky maps can be found in [6]
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