1 Astroparticle Physics in Space Claudia Cecchi Dipartimento di Fisica e Sezione INFN, Perugia Workshop Nazionale La Scienza e la Tecnologia sulla Stazione Spaziale Internazionale (ISS), Torino maggio 2001
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3 Physics of AMS Search for Nuclear Antimatter with a sensitivity (anti-He,….,C) Search for supersymmetric Dark Matter (p -, e +, spectra ) Astrophysics: light isotopes, 2 H, 3 He, 9 Be/ 10 Be, B/C
4 RECENT AMS RESULTS STS 91 Flight, June 1998
5 NEW LIMIT ON antiHe
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7 RESULTS on High Energy CR fluxes on LEO (trapped energetic particles)
8 Interazione RC con il campo geomagnetico Intrappolato (fasce) Caotico Primario poco deflesso Primario molto deflesso
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10 AMS belts vs Van Allen belts Van Allen belts: –Low energy from ~ 1 MeV to ~ 100 MeV –Contains e-, p –High L-shells high altitude –Life time O(years) Decays of neutrons produced in interactions of primary with the atmosphere (CRAND) Solar wind induced magnetic storms
11 AMS belts vs Van Allen belts AMS belts: –High energy from ~ 1 GeV to ~ 10 GeV –Contains e+, e-, p, 3 He –e+ over e- dominance –Low L- shell low altitude –Life time O(seconds) => Secondary production from CR interaction with atmosphere
12 RESULTS on Primary Cosmic Ray Spectra
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20 Energy Range of AMS on ISS p + up to several TeV p - up to 200 GeV e - up to O(TeV) e + up to 200 GeV He,….C up to several TeV anti – He…C up to O(TeV) up to 100 GeV Light Isotopes up to 20 GeV
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23 Physics of AMS Detection of extragalactic sources –AGN –Blazars Measurement of absorption n IR /Ho Search for supersymmetric dark matter - ray burst
24 Energy range of AMS 0.3 to 100 GeV GeV --> new range to be explored
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27 Mission profile AMS: on the ISS (52 o ) (three years) Agile 2003 GLAST 2006
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29 ElectronsPositrons on low earth orbit
30 Protons in low earth orbit
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