About: Greisen–Zatsepin

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The Greisen–Zatsepin–Kuzmin limit (GZK limit) is a theoretical upper limit on the energy of cosmic ray protons traveling from other galaxies through the intergalactic medium to our galaxy. The limit is 5×1019 eV (50 EeV), or about 8 joules (the energy of a proton travelling at ≈ 99.99999999999999999998% the speed of light). The limit is set by the slowing effect of interactions of the protons with the microwave background radiation over long distances (≈ 160 million light-years). The limit is at the same order of magnitude as the upper limit for energy at which cosmic rays have experimentally been detected, although indeed some detections appear to have exceeded the limit, as noted below. For example, one extreme-energy cosmic ray, the Oh-My-God Particle, which has been found to possess a

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rdfs:label	GZK-Cutoff (de) Límite Greisen-Zatsepin-Kuzmin (es) Limite de Greisen-Zatsépine-Kouzmine (fr) Greisen–Zatsepin–Kuzmin limit (en) Effetto GZK (it) GZK限界 (ja) GZK-limiet (nl) Предел Грайзена — Зацепина — Кузьмина (ru) GZK極限 (zh)
rdfs:comment	GZK-Cutoff (nach den Physikern Kenneth Greisen, Georgi Sazepin und Wadim Kusmin, die sie im Jahre 1966 errechneten) ist die Obergrenze (engl. cutoff) für die Energie kosmischer Protonen-Strahlung sehr weit entfernter (⪆ 50 Mpc) Quellen.Es geht hierbei um Protonen mit so hohen Energien, dass die Geschwindigkeitsdifferenz dieser Protonen zu Photonen nur noch so gering ist, dass es 600 Jahre (5 · 1019 eV) bis 2400 Jahre (1020 eV) dauert, bis sie 1 Millimeter gegenüber Photonen zurückgefallen sind. (de) En cosmología y física de partículas, el límite Greisen–Zatsepin–Kuzmin (límite GZK) es un límite superior teórico a la energía de los rayos cósmicos (partículas de alta energía procedentes del espacio) procedentes de fuentes distantes. El límite es 5×1019 electronvoltios (eV), o aproximadamente 8 julios. El límite se debe a interacciones de los protones de los rayos cósmicos con el fondo cósmico de microondas a lo largo de grandes distancias (~160 millones de años luz). El límite está en el mismo orden de magnitud que los rayos cósmicos más energéticos que se han observado. (es) La limite de Greisen-Zatsépine-Kouzmine (ou limite GZK, en anglais GZK limit ou GZK cutoff) est une limite théorique supérieure de l'énergie des rayons cosmiques provenant de sources distantes (au-delà de notre galaxie, la Voie lactée). En d'autres termes, on ne devrait pas observer sur Terre de rayons cosmiques avec une énergie supérieure à cette limite. En réalité, des dépassements de cette limite théorique ont bien été observés. Cette anomalie encore inexpliquée (en 2015) fait l'objet de recherches. (fr) De GZK-limiet (afgeleid van de namen Greisen-Zatsepin-Kuzmin) is de theoretische bovengrens van de energie die kosmische straling kan hebben. (nl) GZK限界（ジーズィーケーげんかい：英語: Greisen-Zatsepin-Kuzmin limit、略称GZK limit）またはGZKカットオフ（ジーズィーケーカットオフ：GZK cutoff）とは4×1019eV以上の高エネルギー宇宙線は宇宙背景放射のマイクロ波（光子）との相互作用によりエネルギーを失うため地球には届かないという予想である。1966年に米国の Greisen、ソビエト連邦の Zatsepin と Kuzmin が提唱した。提唱者の名前の頭文字が呼称の由来である。 (ja) The Greisen–Zatsepin–Kuzmin limit (GZK limit) is a theoretical upper limit on the energy of cosmic ray protons traveling from other galaxies through the intergalactic medium to our galaxy. The limit is 5×1019 eV (50 EeV), or about 8 joules (the energy of a proton travelling at ≈ 99.99999999999999999998% the speed of light). The limit is set by the slowing effect of interactions of the protons with the microwave background radiation over long distances (≈ 160 million light-years). The limit is at the same order of magnitude as the upper limit for energy at which cosmic rays have experimentally been detected, although indeed some detections appear to have exceeded the limit, as noted below. For example, one extreme-energy cosmic ray, the Oh-My-God Particle, which has been found to possess a (en) L'effetto GZK (o taglio GZK) è stato teorizzato nel 1966 dagli scienziati , e , dalle cui iniziali prende il nome. Stabilisce un limite massimo all'energia dei protoni che viaggiano nell'universo, dovuto alla presenza della radiazione cosmica di fondo. Quando un protone ad alta energia (circa maggiore di 1020 eV) si scontra con un fotone della radiazione cosmica di fondo con energia ≈ 10−3 eV si ha la produzione di pioni. I due risultati possibili sono: (it) Предел Грайзена — Зацепина — Кузьмина (предел ГЗК, реликтовое (или чернотельное) обрезание спектра в области предельно высоких энергий, GZK-эффект, англ. Greisen – Zatsepin – Kuzmin limit, GZK limit) — это теоретический верхний предел энергии космических лучей от отдалённых источников. или Средняя дистанция гашения энергии частиц — 50 Мпк, а так как в этих пределах нет никаких источников космических лучей таких высоких энергий, подобные частицы наблюдаться не должны. (ru) GZK極限，是以提出者Greisen、Zatsepin、Kuzmin三人姓氏之首字母為名的理論上限，描述源自遠處的宇宙射線應有的理論上限值。這項極限是在1966年由Kenneth Greisen、Vadim Kuzmin與Georgiy Zatsepin三人所計算，其基礎為宇宙微波背景輻射與宇宙射線的預期交互作用。預測中指出宇宙射線所帶的能量如果超過閾值5×1019 電子伏特則會與宇宙微波背景的光子發生交互作用，產生Π介子。這樣的作用會持續發生，一直到射線粒子的能量低於Π介子產生閾值。因為此交互作用相關的平均自由程其值甚低，舉例來說，起源處距離地球遠大於50 百萬秒差距的若其能量大於此閾值者，則不可能在地球上觀測到；而此距離內又不存在目前已知可以產生此般能量的宇宙射線源。已有一些由明野廣域空氣簇射陣列實驗所作的觀測顯示遠源的宇宙射線帶有高於此極限的能量（稱作超高能宇宙射線）。這樣的觀測事實被稱作GZK悖論（GZK paradox）或宇宙射線悖論（cosmic ray paradox）。這些觀測似乎與目前所知的狹義相對論及粒子物理的預測相違背。不過，也有一些對於此類觀測所作的可能解釋，似乎可以解決這種不一致。首先，這些觀測可能出自於儀器上的誤差，或者是對於實驗結果不正確的解讀。再者，宇宙射線也可能有局域的粒子源（雖然尚不明白這些粒子源會是什麼）。 (zh)
dcterms:subject	Physical paradoxes Astroparticle physics Cosmic rays Special relativity Unsolved problems in astronomy Energy Unsolved problems in physics
Wikipage page ID	180236 (xsd:integer)
Wikipage revision ID	1123804186 (xsd:integer)
Link from a Wikipage to another Wikipage	Proton Extreme Universe Space Observatory Delta baryon Physical paradoxes Joule Vadim Kuzmin (physicist) Doubly special relativity Philippe Véron Cosmic microwave background radiation Cosmic ray Astroparticle physics Energy Georgiy Zatsepin Oh-My-God particle Standard Model Particle physics Active galactic nucleus Centrifugal mechanism of acceleration HZE ions Alan Andrew Watson Akeno Giant Air Shower Array Cosmic rays Extreme-energy cosmic ray Fermi Gamma-ray Space Telescope Fluorescence Pair production International Space Station EGRET Telescope Array Project Special relativity Unsolved problems in astronomy Energy Unsolved problems in physics Kenneth Greisen High Resolution Fly's Eye Cosmic Ray Detector Pierre Auger Observatory Pion Special relativity Neutrino Blueshift Conservation of linear momentum Lorentz covariance Science (journal) Ultra-high-energy cosmic ray AGASA
Link from a Wikipage to an external page	http://www.cosmic-ray.org/ http://www.auger.org http://www.physics.rutgers.edu/hex/HIRES.html http://www.p-ng.si/public/pao/history.php
sameAs	Greisen–Zatsepin–Kuzmin limit Greisen–Zatsepin–Kuzmin limit Greisen–Zatsepin–Kuzmin limit Greisen–Zatsepin–Kuzmin limit Greisen–Zatsepin–Kuzmin limit Greisen–Zatsepin–Kuzmin limit Greisen–Zatsepin–Kuzmin limit Greisen–Zatsepin–Kuzmin limit Greisen–Zatsepin–Kuzmin limit

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