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Fig. 7

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Illustration of the scheme adopted for the acceleration of GCR in Prantzos (2012) and here. At explosion, the star of initial mass M ∗  has a mass MEXP and leaves behind a remnant of mass MREM, i.e. the explosively ejected mass is MEJ, while the mass previously ejected by the wind is MWind = M ∗ MEXP. Particle acceleration starts at the beginning of the Sedov-Taylor phase, located at mass coordinate A1 = MExp+ MEj, i.e. when the forward shock (FS, arrows), launched at MExp, has swept up a mass MS1=MEj. Acceleration stops at mass coordinate A2, selected in P12 to reproduce – after an average with a Salpeter IMF – the GCR source ratio of 22Ne/20Ne = 5.3 in solar units; in the case of rotating stars adopted here, it corresponds to a shock velocity of 1900 km s-1. The mass sampled by the FS between those two regions is MAcc = A2A1. For rotating stars with mass M > 30 M, an increasing part of MAcc includes nuclearly processed material (shaded aerea), while for rotating stars with M < 18 M, MAcc contains only material of ISM composition. The yields of Fig. 4 correspond to the mass MWind = M ∗ MEXP, while the composition of GCR adopted here corresponds to the mass MACC.

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