Supernova explosions of massive stars and cosmic rays
  Most cosmic ray particles observed derive from the explosions of massive
stars, which commonly produce stellar black holes in their supernova
explosions. When two such black holes find themselves in a tight binary system
they finally merge in a gigantic emission of gravitational waves, events that
have now been detected. After an introduction (section 1) we introduce the
basic concept (section 2): Cosmic rays from exploding massive stars with winds
always show two cosmic ray components at the same time: (i) the weaker polar
cap component only produced by Diffusive Shock Acceleration with a cut-off at
the knee, and (ii) the stronger $4 \pi$ component with a down-turn to a steeper
power-law spectrum at the knee, and a final cutoff at the ankle. In section 3
we use the Alpha Magnetic Spectrometer (AMS) data to differentiate these two
cosmic ray spectral components. The ensuing secondary spectra can explain
anti-protons, lower energy positrons, and other secondary particles. Triplet
pair production may explain the higher energy positron AMS data. In section 4
we test this paradigm with a theory of injection based on a combined effect of
first and second ionization potential; this reproduces the ratio of Cosmic Ray
source abundances to source material abundances. In section 5 we interpret the
compact radio source 41.9+58 in the starburst galaxy M82 as a recent binary
black hole merger, with an accompanying gamma ray burst. This can also explain
the Ultra High Energy Cosmic Ray (UHECR) data in the Northern sky. Thus, by
studying the cosmic ray particles, their abundances at knee energies, and their
spectra, we can learn about what drives these stars to produce the observed
cosmic rays.
