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Home All issues Volume 592 (August 2016) A&A, 592 (2016) A123 Full HTML
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Fig. 1

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Radial profile of the magnetic field strength (left plot) and star formation rate (right plot). These profiles are used in our model to determine the synchrotron losses, via B(r) in Eq. (2) and source distribution for the CREs, Q(r) in Eq. (3).

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