BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//CERN//INDICO//EN
BEGIN:VEVENT
SUMMARY:Secondary electron spectrum in the upper atmosphere
DTSTART;VALUE=DATE-TIME:20070704T194500Z
DTEND;VALUE=DATE-TIME:20070704T194500Z
DTSTAMP;VALUE=DATE-TIME:20260713T062027Z
UID:indico-contribution-230@cern.ch
DESCRIPTION:Speakers: Dr. KOMORI\, yoshiko (Kanagawa University of Human S
 ervices)\nThe secondary electron flux at altitude below 10 g/cm^2 is estim
 ated \nusing the result of atmospheric gamma ray spectrum above 30GeV\, \n
 which has been obtained by our emulsion chamber experiments at balloon \na
 ltitudes.  We have to subtract these electrons produced by nuclear \ninter
 actions from the observed electrons\, when deriving the primary \nelectron
  spectrum in the Galaxy.\nIn addition\, for balloon experiments it is impo
 rtant to investigate \nthe spectral changes of electrons and gamma rays in
  upper atmosphere.\nBoth electron and gamma ray intensities at the depth  
 are \ncalculated using the shower theory and integrated over the observed 
 \nrange of zenith angle. Further the results are compared with those \nfro
 m Monte Carlo simulation.\nThe results shows that the number of secondary 
 electrons increases \nproportionally with ^2 and is about % of that of gam
 ma rays. \nThe ratio of secondary electrons to primary electrons increases
  in the TeV \nregion\, so that the high altitude is essential for TeV elec
 tron experiments.\n\nhttps://indico.nucleares.unam.mx/event/4/session/8/co
 ntribution/230
LOCATION:Merida\, Mexico Regency (Hyatt)
URL:https://indico.nucleares.unam.mx/event/4/session/8/contribution/230
END:VEVENT
END:VCALENDAR