BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//CERN//INDICO//EN
BEGIN:VEVENT
SUMMARY:Constraining positron emission from pulsar populations with AMS-02
  data
DTSTART;VALUE=DATE-TIME:20210902T154500Z
DTEND;VALUE=DATE-TIME:20210902T160000Z
DTSTAMP;VALUE=DATE-TIME:20260421T040017Z
UID:indico-contribution-15745@indico.ific.uv.es
DESCRIPTION:Speakers: Luca Orusa (Turin U. and INFN)\nThe cosmic-ray flux 
 of positrons ($e^+$) is measured with high precision by the space-borne pa
 rticle spectrometer AMS-02. The hypothesis that pulsar wind nebulae (PWNe)
  can significantly contribute to the excess of the $e^+$ cosmic-ray flux h
 as been consolidated after the observation of a $\\gamma$-ray emission at 
 TeV energies of a few degree size around Geminga and Monogem PWNe. \nIn th
 is work we simulate Galactic pulsars populations adopting different distri
 butions for their position in the Galaxy as well as their intrinsic physic
 al properties\, in order to overcome the incompleteness of the ATNF catalo
 gue. We fit the $e^+$ AMS-02 data together with a secondary component due 
 to collisions of primary cosmic rays with the interstellar medium. We find
  that several mock galaxies have a pulsar population able to explain the o
 bserved $e^+$ flux\, characterized by few\, bright sources. We determine t
 he physical parameters of the sources dominating the $e^+$ flux\, and asse
 ss the impact of different assumptions on radial distributions\, spin-down
  properties\, propagation scenarios and $e^+$ emission time.\n\nhttps://in
 dico.ific.uv.es/event/6178/contributions/15745/
LOCATION:
URL:https://indico.ific.uv.es/event/6178/contributions/15745/
END:VEVENT
END:VCALENDAR