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Electron and positron fluxes in cosmic rays are currently measured withunprecedented precision by AMS-02 up to TeV energies, and represent uniqueprobes for the local properties of our Galaxy. The interpretation of theirspectra is at present still debated, especially for the excess of positronsabove 10 GeV. The hypothesis that pulsars can significantly contribute to thisexcess has been consolidated after the observation of gamma-ray halos at TeVenergies of a few degree size around Geminga and Monogem pulsars. However, thespatial and energetic Galactic distribution of pulsars and the details of thepositron production, acceleration and release from these sources are not yetfully understood. I will describe how we can use the high-precision AMS-02positron data to constrain the main properties of the Galactic pulsarpopulation and of the positron acceleration needed to explain the observedfluxes. This is achieved by simulating a large number of Galactic pulsarpopulations, following the most recent self-consistent modelings for the pulsarspin-down and evolution properties, calibrated on catalog observations. Byfitting the positron AMS-02 data together with a secondary component due tocollisions of primary cosmic rays with the interstellar medium, we determinethe physical parameters of the pulsars dominating the positron flux, and assessthe impact of different assumptions on radial distributions, spin-downproperties, Galactic propagation scenarios and positron emission time.

Constraints on the positron emission from pulsar populations with AMS-02 data