Speaker
Description
Pulsars dominate the local cosmic-ray positron flux at high energies by producing electron-positron pairs from their spindown energy. While the AMS-02 experiment, that measures the cosmic-ray flux to great precision, shows that the positron flux is very smooth, simple simulations of pulsar models predict sharp spectral features. In this work, we add several mechanisms to model the local positron flux more realistically. Specifically, we implement a more realistic positron production mechanism of the pulsars, and take into account variations in the magnetic fields and interstellar radiation fields that affect the energy losses of the positrons as they propagate through the Galaxy. Our models show that the sharp spectral features predicted by the simple models vanish, which is consistent with the observed smoothness of the local cosmic-ray positron flux.
