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I.V. Moskalenko (NASA/GSFC), A.W. Strong (MPE, Garching), J.F. Ormes (NASA/GSFC)
High energy collisions of cosmic ray particles with interstellar gas are believed to be the mechanism producing the majority of cosmic ray antiprotons. Due to the kinematics of the process they are created with a nonzero momentum providing a low energy ``window'' where exotic signals from the annihilation of supersymmetrical particles (WIMPs) and primordial black hole evaporation could be found. Recently new data with large statistics on both low and high energy antiproton flux have become available, and the possibility to launch a probe to measure low energy particles in interstellar space is actively discussed. It is therefore important to make a precise calculation of the ``background'', the flux of cosmic ray secondary antiprotons.
We use our GALPROP code to make a new accurate calculation of the antiproton flux resulting from interactions of cosmic rays with interstellar matter. The antiproton and proton flux measurements made during the most recent solar minimum greatly constrain the problem. The data at energies below 500 MeV are suggestive of a new component.
I.Moskalenko asknowledges support from National Research Council through NAS/NRC Senior Research Associateship program.
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