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SUMMARY:Solar cosmic ray generation by solar flares and propagation in int
 erplanetary space
DTSTART;VALUE=DATE-TIME:20161011T131500Z
DTEND;VALUE=DATE-TIME:20161011T133000Z
DTSTAMP;VALUE=DATE-TIME:20260720T130058Z
UID:indico-contribution-702@cern.ch
DESCRIPTION:Speakers: Igor Podgorny (Institute of Astronomy of the Russian
  Academy of Sciences)\nThe analysis of GOES spacecraft measurements confir
 ms the data of worldwide network of neutron monitors about solar cosmic ra
 y generation in the solar flares above of an active region with the comple
 x magnetic field distribution. The proton acceleration in a particular fla
 re is beyond doubt. The so-called prompt proton component arrives to the E
 arth from western flares with a sharp (~5 min) front. The fronts of the pr
 oton fluxes from the western flares begin to register with a delay not lon
 ger than the time of flight of the particles with their velocity. The prot
 ons of the prompt component can propagate without collisions along the mag
 netic lines of the Archimedes spiral. The proton from the eastern flare ca
 nnot reach the Earth moving along magnetic field lines. They can be transf
 erred across the field lines by solar wind and propagate due to diffusion 
 at scatterings with field fluctuations. The front of proton flux from flar
 es that appeared on the eastern part of the disk is gently sloping. Its du
 ration is bigger than 10 hours. The front of such protons arrives with a d
 elay of several hours\, which is much less than time of solar wind propaga
 tion from the Sun to the Earth. The typical duration of fast proton emissi
 ons from the flare that obtained using γ-ray pulses measurements is order
  of ten minutes\, but the tails of proton flux from western and eastern fl
 ares (delayed components) last several days. Isotropic velocity distributi
 on and long time duration of proton fluxes demonstrate diffusion particle 
 propagation in the pulse tail of western and eastern flares. The proton sc
 attering with field fluctuation can appear due to proton beam instability 
 at the front\, where particle distribution is anisotropic.\n\nhttps://indi
 co.particle.mephi.ru/event/4/contributions/702/
LOCATION:Milan Hotel Verdi
URL:https://indico.particle.mephi.ru/event/4/contributions/702/
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