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Italiano: Formazione della radiazione cosmica secondaria.
La particella primaria (generalmente un it:protone) urta con un nucleo d'it:ossigeno o di it:azoto dell'alta atmosfera. Da questa collisione vengono generati neutroni, protoni, π0, π+, π-, antinuetroni, antiprotoni, kaoni e iperoni. I π0 decadono elettromagneticamente in due γ e questi ultimi possono materializzarsi in coppie e+ e-. I π carichi possono interagire con altri nuclei presenti nell'atmosfera o decadere in leptoni μ e neutrini ν. Gli elettroni irradiano energia sotto forma di raggi γ (radiazione di frenamento). Le linee tratteggiate indicano che altre reazioni possono avvenire. Da Esperimenti del corso di FPE, dello stesso autore dell'articolo it:Raggi cosmici. |
Date | |
Source | Own work by the original uploader |
Author | The original uploader was Gianluigi at Italian Wikipedia. |
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editTransferred from it.wikipedia to Commons by Fale using CommonsHelper.
- 2004-02-04 19:06 Gianluigi 520×302×??? (20876 bytes) Formazione della radiazione cosmica secondaria
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current | 15:25, 5 September 2008 | 520 × 302 (20 KB) | File Upload Bot (Magnus Manske) (talk | contribs) | {{BotMoveToCommons|it.wikipedia}} {{Information |Description={{it|Formazione della radiazione cosmica secondaria. La particella primaria (generalmente un it:protone) urta con un nucleo d'it:ossigeno o di it:azoto dell'alta atmosfera. Da q |
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