Production of antiprotons in interstellar space by propagating cosmic rays under conditions of diffusive reacceleration

The propagation of cosmic rays in the Galaxy is understood as a diffusive process in which the magnetic field irregularities serve as scatter centers. Particles that interact with turbulent magnetic field irregularities can gain energy because of stochastic, second-order, Fermi type of acceleration. We could show that such a propagation scenario, in which the particles are primary preenergized at the outsets and then reaccelerated during propagation, is completely compatible with the observation of cosmic-ray nuclear data, such as cosmic-ray spectra and the secondary/primary ratio of boron/carbon and subiron/iron. In this context, we present here results of the expected interstellar secondary antiproton flux via p + p --> (p) over bar + x interactions in the framework of this diffusive reacceleration model. We can show that the interstellar (P) over bar spectrum under these conditions looks very different from that calculated in the Standard Leaky Box situation.