Fig. 10
Dependence of the turbulent magnetic field strength Bran on the star formation rate per unit area, ΣSFR. The points represent average values in 2 kpc-wide rings in the plane of M 101. The dashed line shows the power-law fit for R< 24 kpc given in the text. Statistical errors of 1σ are shown for ΣSFR, but are negligble in Bran.
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