Galactic centre star formation writ large in gamma-rays
Roland M. Crocker

TL;DR
This paper models the high-energy processes in the Galactic center, explaining diffuse gamma-ray and microwave emissions through cosmic ray interactions, magnetic fields, and galactic winds, suggesting a long-standing energetic source since the Galaxy's early days.
Contribution
It provides a comprehensive model linking cosmic rays, magnetic fields, and galactic winds to observed gamma-ray and microwave emissions in the Galactic center and Fermi bubbles, highlighting a persistent energetic source.
Findings
Magnetic field in GC is 100-300 microG.
Super-wind removes >95% of cosmic rays from the region.
Steady-state cosmic ray power is ~10^39 erg/s, explaining Fermi bubbles.
Abstract
We have modelled the high-energy astrophysics of the inner 200 pc of the Galaxy with a view to explaining the diffuse, broad-band (radio continuum to TeV gamma-ray), non-thermal signal detected from this region. Our modelling pins down the ISM parameters for the environment wherein cosmic ray (CR) electrons and ions reside in the Galactic centre (GC). We find that the magnetic field in this region is 100-300 microG, the gas density < 60 cm^-3, and that a powerful (> 200 km/s) 'super'-wind acts to remove > 95% of the cosmic rays accelerated in the region before they have time to lose their energy in situ. The ~ 10^39 erg/s carried away by the GC cosmic ray protons is precisely enough to energise the ~GeV gamma-ray emission from the Fermi 'bubbles' recently found to extend north and south of the GC out to distances of ~10 kpc, provided that the bubbles constitute thick targets to the GC…
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