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Презентация была опубликована 3 года назад пользователемАнтонина Нездольева

1 One of the greatest GLE The time profiles of the greatest GLEs.

2 Big and long anisotropy The visual anisotropy in CR variations at four NMs: CAPS-Cape Shmidt, MCMD-McMurdo, NAIN, THUL- Thule. GLE 69 as seen on subpolar NMs McMurdo and Thule. В первые 40 минут больша анизотропия очевидна, на самом деле возрастание в McMurdo заметно выше чем в Thule и через 10 часов

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 cosmic rays with different energies (from neutron monitors). Behavior of integral fluxes of solar protons with different energies (GOES data).

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 (>3 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 Поток солнечных КЛ оставался анизотропным не менее 11 часов. Изменения характеристик анизотропии со временем, в основном, по-видимому, связаны с изменчивостью межпланетного магнитного поля. Полученные результаты можно и нужно улучшить.

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