Magnetic fields permeate the interstellar medium (ISM), extending far beyond the Galactic disc. The non-thermal phenomena, like e.g. the Galactic radio emission is doubtless a viable method of observation to clearly delineate the magnetic structure of our Galaxy.
In this regard, the aim addressed in this contribution is to simulate the polarized Galactic synchrotron emission, due to the diffuse radiation by charged relativistic particles, at all relevant frequencies, 10 MHz up to 100 GHz.
Magnetic fields permeate the interstellar medium (ISM), extending far beyond the Galactic disc....
MPI für Astrophysik, Karl-Schwarzschild-Strasse 1, 85740 Garching, Germany
D. Grasso
Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, Largo B. Pontecorvo, 56127 Pisa, Italy
C. Evoli
II. Institut für Theoretische Physik, Universität Hamburg, Luruper Chaussee 149, 22761 Hamburg, Germany
D. Gaggero
SISSA, Via Bonomea 265, 34136 Trieste, Italy
INFN, sezione di Trieste, via Valerio 2, 34127 Trieste, Italy
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Magnetic fields permeate the interstellar medium (ISM), extending far beyond the Galactic disc. The non-thermal phenomena, like e.g. the Galactic radio emission is doubtless a viable method of observation to clearly delineate the magnetic structure of our Galaxy.
In this regard, the aim addressed in this contribution is to simulate the polarized Galactic synchrotron emission, due to the diffuse radiation by charged relativistic particles, at all relevant frequencies, 10 MHz up to 100 GHz.
Magnetic fields permeate the interstellar medium (ISM), extending far beyond the Galactic disc....
