Can we explain AMS-02 antiproton and positron excesses simultaneously by
  nearby supernovae without pulsars nor dark matter?
  We explain the excess of the antiproton fraction recently reported by the
AMS-02 experiment by considering collisions between cosmic-ray protons
accelerated by a local supernova remnant (SNR) and the surrounding dense cloud.
The same "$pp$-collisions" provide the right ratio of daughter particles to fit
the observed positron excess simultaneously in the natural model parameters.
The supernova happened in relatively lower metalicity than the major cosmic-ray
sources. The cutoff energy of electrons marks the supernova age of $\sim
10^{5}$ years, while the antiproton excess may extend to higher energy. Both
antiproton and positron fluxes are completely consistent with our predictions
in Fujita, Kohri, Yamasaki and Ioka (2009).
