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Astroparticle Physics in SpaceAstroparticle Physics in Space

Claudia CecchiClaudia Cecchi

Dipartimento di Fisica e Sezione INFN, PerugiaDipartimento di Fisica e Sezione INFN, Perugia

Workshop Nazionale La Scienza e la Tecnologia sulla Stazione Workshop Nazionale La Scienza e la Tecnologia sulla Stazione Spaziale Internazionale (ISS), Torino 16-18 maggio 2001Spaziale Internazionale (ISS), Torino 16-18 maggio 2001

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Physics of AMS

• Search for Nuclear Antimatter with a 10-9 sensitivity (anti-He,….,C)

• Search for supersymmetric Dark Matter (p-, e+, spectra )

• Astrophysics: light isotopes, 2H, 3He, 9Be/10Be, B/C

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RECENT AMS RESULTS

STS 91 Flight, June 1998

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NEW LIMIT ON antiHe

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RESULTS on

High Energy CR fluxes on LEO(trapped energetic particles)

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Interazione RC con il campo geomagnetico

Intrappolato(fasce)

Caotico

Primariopoco deflesso

Primariomolto deflesso

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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

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AMS belts vs Van Allen belts

• AMS belts: – High energy from ~ 1 GeV to ~ 10 GeV– Contains e+, e-, p, 3He– e+ over e- dominance– Low L- shell low altitude– Life time O(seconds)

=> Secondary production from CR interaction with atmosphere

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RESULTS on

Primary Cosmic Ray Spectra

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Energy Range of AMS on ISS

p+ up to several TeVp- up to 200 GeVe- up to O(TeV)e+ up to 200 GeVHe,….C up to several TeVanti – He…C up to O(TeV) up to 100 GeVLight Isotopes up to 20 GeV

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Physics of AMS

• Detection of extragalactic sources– AGN– Blazars

• Measurement of absorption nIR/Ho

• Search for supersymmetric dark matter

• - ray burst

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Energy range of AMS

0.3 to 100 GeV

30-100 GeV --> new range to be explored

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Mission profile

• AMS: 2003- 2007 on the ISS (52o) (three years)

• Agile 2003

• GLAST 2006

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Electrons Positrons

on low earth orbit

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Protons in low earth orbit

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