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Mmẹkụwátá

Nkówá
English: The flux of cosmic ray particles as a function of their energy. The flux for the lowest energies (yellow zone) are mainly attributed to solar cosmic rays, intermediate energies (blue) to galactic cosmic rays, and highest energies (purple) to extragalactic cosmic rays
Français : Le flux de particules du rayonnement cosmique (incident au sommet de l'atmosphère terrestre, par unité de surface, par unité de temps et par unité d'angle solide et par intervalle d'énergie des particules incidentes de 1 gigaélectron-volt (1 GeV)) représenté en fonction de leur énergie.
Le flux des énergies les plus basses (zone jaune) sont principalement imputables aux rayons cosmiques solaires, les énergies intermédiaires (en bleu) aux rayons cosmiques galactiques, et les plus hautes énergies (violet) aux rayons cosmiques extragalactiques
Ǹgụ́ụ̀bọ̀chị̀
Mkpọlọ́gwụ̀ own work, after Swordy[1] and De Angelis[2]
Odé ákwụ́kwọ́ Sven Lafebre

References

  1. ↑ S. Swordy, The energy spectra and anisotropies of cosmic rays, 2001, Space Science Reviews 99, pp85–94.
  2. ↑ A. de Angelis and M. Pimenta, Introduction to particle and astroparticle physics (Multimessenger astronomy and its particle physics foundations), Springer 2018, p577.

Nkwényé

I, the copyright holder of this work, hereby publish it under the following licenses:
GNU head Í nwèrèíkí jé, gbạsáa na/ma í mezí akwukwo nka na okpúrù íwú GNU Ákwúkwó Íwú nke Owéré, Nké 1.2 ma nke íchè ndi Free Software Foundation; wéfùtàrà; na adighi nkejị di íchẹ, adighi édé nke Ihú-Ihü Ákwúkwó, na adighi Ázú-Ihü Ákwúkwó. Ákwúkwó iwu hé jéré jé di na nkeji kpóró GNU Ákwúkwó Íwú nke Owéré".
w:en:Creative Commons
í-kpó-áhà gbásàa kà 		Edebere faịlụ a n'okpuru ikikeree Creative Commons Attribution-Share Alike 3.0 Unported license.
I wepulara nóru:
  • i nye – ikọpị,ikekasi na izịpụ ọru a
  • i dowaria – igbanwee ọrụ a
Ọ ga bụ na ọnọdụ ndi a:
  • í-kpó-áhà – Ị ga-enyerịrị ugo kwesịrị ekwesị, nye njikọ na ikikere ahụ, ma gosikwa ma emere mgbanwe. Ị nwere ike ime ya n'ụzọ ezi uche ọ bụla, mana ọ bụghị n'ụzọ ọ bụla na-egosi na onye nyere ikikere kwadoro gị maọbụ ojiji gị.
  • gbásàa kà – Ọ bụrụ na ị tụgharịgharịa, gbanwee, ma ọ bụ wulite n'elu ihe ahụ, ị ga-ekesa ndenye gị n'okpuru otu ma ọ bụ ikike dakọtara dị ka nke mbụ.
This licensing tag was added to this file as part of the GFDL licensing update.
w:en:Creative Commons
í-kpó-áhà gbásàa kà
This file is licensed under the Creative Commons Attribution-Share Alike 2.5 Generic, 2.0 Generic and 1.0 Generic license.
I wepulara nóru:
  • i nye – ikọpị,ikekasi na izịpụ ọru a
  • i dowaria – igbanwee ọrụ a
Ọ ga bụ na ọnọdụ ndi a:
  • í-kpó-áhà – Ị ga-enyerịrị ugo kwesịrị ekwesị, nye njikọ na ikikere ahụ, ma gosikwa ma emere mgbanwe. Ị nwere ike ime ya n'ụzọ ezi uche ọ bụla, mana ọ bụghị n'ụzọ ọ bụla na-egosi na onye nyere ikikere kwadoro gị maọbụ ojiji gị.
  • gbásàa kà – Ọ bụrụ na ị tụgharịgharịa, gbanwee, ma ọ bụ wulite n'elu ihe ahụ, ị ga-ekesa ndenye gị n'okpuru otu ma ọ bụ ikike dakọtara dị ka nke mbụ.
Ị nwere ike họrọ ikikere nke masịrị gị.

Nkowapụta

Tinye nkọwa otu ahịrị ihe faịlụ a na-anochi anya ya.
Graph of cosmic flux versus particle energy

Ihe ndị egosiri na faịlụ a

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Oge/afọ mmalite

8 Jenụwarị 2019

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usoro mkpebi: SHA-1

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614 pixel

width Bekee

512 pixel

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dị ùgbu â10:31, 15 Febụwarị 2019NvóÁká màkà otù ȯ dị nà 10:31, 15 Febụwarị 2019512 × 614 (113 KB)Cherkashan updated 2018 version uploaded based on the original author's request (see [https://commons.wikimedia.org/wiki/Commons:Help_desk/Archive/2019/01#New_version_of_%22Cosmic_ray_flux_versus_particle_energy%22_image here])
14:12, 12 Jenụwarị 2007NvóÁká màkà otù ȯ dị nà 14:12, 12 Jenụwarị 2007400 × 480 (94 KB)Svenlafe~commonswiki== Summary == {{Information |Description=The flux of cosmic ray particles as a function of their energy. The flux for the lowest energies (yellow zone) are mainly attributed to solar cosmic rays, intermediate energies (blue) to galactic cosmic rays, and h
14:05, 12 Jenụwarị 2007NvóÁká màkà otù ȯ dị nà 14:05, 12 Jenụwarị 2007400 × 480 (26 KB)Svenlafe~commonswiki{{Information |Description=The flux of cosmic ray particles as a function of their energy. The flux for the lowest energies (yellow zone) are mainly attributed to solar cosmic rays, intermediate energies (blue) to galactic cosmic rays, and highest energie

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