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One of the greatest GLE

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at four NMs: CAPS-Cape Shmidt, MCMD-McMurdo, NAIN, THUL-Thule. GLE 69 as seen on subpolar NMs McMurdo and Thule. ... ??????? ???? ??? ? Thule ? ????? 10 ????? ... – PowerPoint PPT presentation

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Title: One of the greatest GLE


1
One of the greatest GLE
The time profiles of the greatest GLEs.
2
Big and long anisotropy
GLE 69 as seen on subpolar NMs McMurdo and Thule.
? ?????? 40 ????? ?????? ??????????? ????????,
?? ????? ???? ??????????? ? McMurdo ??????? ????
??? ? Thule ? ????? 10 ?????
The visual anisotropy in CR variations at four
NMs CAPS-Cape Shmidt, MCMD-McMurdo, NAIN,
THUL-Thule.
3
Energy spectrum changes
Spectra of the solar CR during the first and
second 5-minute intervals after the onset.
4
Mean Flux and Energy Spectrum
Behavior of the power law energy spectrum index
together with 1 GeV mean (averaged by the all
directions) particle flux.
5
Upper Proton Energy
Behavior of the upper energy Eu, chosen by model
and observed by neutron monitor.
6
Maximal, Minimal and Mean Fluxes
Behavior of the minimal, maximal and mean fluxes
of solar cosmic rays with 1 GeV
energy. Anysotropy up to late time. .
7
Differential Fluxes
Behavior of differential fluxes of solar cosmic
rays with different energies. Simultaneous
maximum in broad energy range. .
8
Integral Fluxes
Behavior of integral fluxes of solar protons
with different energies(GOES data).
Behavior of integral fluxes of solar cosmic rays
with different energies (from neutron monitors).
9
Anisotropy
Behavior of of solar cosmic ray anisotropy
magnitude and coefficient n, characterizing a
width of anisotropic flux angular distribution. .

10
Anisotropy Source Location
Behavior of of latitude and longitude of maximal
solar particle flux. .
11
Angular distribution
Angular distributions in 3 first intervals and
half of hour later.
12
Longitudinal distribution
Longitudinal distributions in 3 first intervals
and on late phase of GLE.
13
Longitudinal Distribution
14
Asymptotic Map
15
Conclusions
  • The record enhancement in the counting rate at
    some southern polar NMs on 20 January 2005 ranges
    this event among the greatest GLEs. Nevertheless,
    high energy particles (gt3 GeV) turned out to be
    of much less amount than in 1956 and 1989 events.
  • The first particles came by very narrow beam and
    had a very hard spectrum. Already in some minutes
    after the onset the spectrum became soft and kept
    its form during the several hours with index
    -3.0-4.0.
  • ????? ????????? ?? ????????? ???????????? ??
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    ??????? ? ????????????? ????????????? ??????????
    ????.
  • ?????????? ?????????? ????? ? ????? ????????.
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