Search for the Cosmic Neutrino Background

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68407700%3A21670%2F15%3A00242529" target="_blank" >RIV/68407700:21670/15:00242529 - isvavai.cz</a>

Výsledek na webu

<a href="http://iopscience.iop.org/article/10.1088/1742-6596/580/1/012040/meta" target="_blank" >http://iopscience.iop.org/article/10.1088/1742-6596/580/1/012040/meta</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/1742-6596/580/1/012040" target="_blank" >10.1088/1742-6596/580/1/012040</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Search for the Cosmic Neutrino Background

Popis výsledku v původním jazyce

One expects three Cosmic Backgrounds: (1) The Cosmic Microwave Background (CMB) originated 380000 years after the Big Bang (BB). (2) The Neutrino Background decoupled about one second after the BB, while (3) the Cosmic Gravitational Wave Background created by the inflationary expansion decoupled directly after the BB. Only the Cosmic Microwave Background (CMB) has been detected and is well studied. Its spectrum follows Planck's black body radiation formula and shows a remarkable constant temperature of T-0 gamma approximate to 2.7 K independent of the direction. The present photon density is about 370 photons per cm(3). The size of the hot spots, which deviates only in the fifth decimal of the temperature from the average value, tells us, that the universe is flat. About 380 000 years after the Big Bang at a temperature of T-0 gamma = 3000 K already in the matter dominated era the electrons combine with the protons and He-4 and the photons move freely in the neutral universe and form the CMB. So the temperature and distribution of the photons give us information of the universe 380 000 years after the Big Bang. The Cosmic Neutrino Background (C nu B) decoupled from matter already one second after the BB at a temperature of about 10(10) K. Today their temperature is similar to 1.95 K and the average density is 56 electron-neutrinos and the total density of all neutrinos about 336 per cm(3). Measurement of these neutrinos is an extremely challenging experimental problem which can hardly be solved with the present technologies. On the other hand it represents a tempting opportunity to check one of the key elements of the Big Bang Cosmology and to probe the early stages of the universe. The search for the C nu B with the induced beta decay nu(e) + H-3 -> He-3 + e(-) using KATRIN (KArlsruhe TRItium Neutrino experiment) is the topic of this contribution.

Název v anglickém jazyce

Search for the Cosmic Neutrino Background

Popis výsledku anglicky

One expects three Cosmic Backgrounds: (1) The Cosmic Microwave Background (CMB) originated 380000 years after the Big Bang (BB). (2) The Neutrino Background decoupled about one second after the BB, while (3) the Cosmic Gravitational Wave Background created by the inflationary expansion decoupled directly after the BB. Only the Cosmic Microwave Background (CMB) has been detected and is well studied. Its spectrum follows Planck's black body radiation formula and shows a remarkable constant temperature of T-0 gamma approximate to 2.7 K independent of the direction. The present photon density is about 370 photons per cm(3). The size of the hot spots, which deviates only in the fifth decimal of the temperature from the average value, tells us, that the universe is flat. About 380 000 years after the Big Bang at a temperature of T-0 gamma = 3000 K already in the matter dominated era the electrons combine with the protons and He-4 and the photons move freely in the neutral universe and form the CMB. So the temperature and distribution of the photons give us information of the universe 380 000 years after the Big Bang. The Cosmic Neutrino Background (C nu B) decoupled from matter already one second after the BB at a temperature of about 10(10) K. Today their temperature is similar to 1.95 K and the average density is 56 electron-neutrinos and the total density of all neutrinos about 336 per cm(3). Measurement of these neutrinos is an extremely challenging experimental problem which can hardly be solved with the present technologies. On the other hand it represents a tempting opportunity to check one of the key elements of the Big Bang Cosmology and to probe the early stages of the universe. The search for the C nu B with the induced beta decay nu(e) + H-3 -> He-3 + e(-) using KATRIN (KArlsruhe TRItium Neutrino experiment) is the topic of this contribution.

Druh

D - Stať ve sborníku

CEP obor

BG - Jaderná, atomová a molekulová fyzika, urychlovače

OECD FORD obor

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Projekt

<a href="/cs/project/LM2011027" target="_blank" >LM2011027: Projekt LSM/ULISSE ? příspěvek k rozšíření velké výzkumné infrastruktury evropského významu (podzemní laboratoř a výstavba detektoru SuperNEMO, pokračování české účasti)</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2015

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název statě ve sborníku

11th International Spring Seminar on Nuclear Physics: Shell Model and Nuclear Structure

ISBN

—

ISSN

1742-6588

e-ISSN

—

Počet stran výsledku

6

Strana od-do

1-6

Název nakladatele

IOP Publishing

Místo vydání

London

Místo konání akce

Ischia

Datum konání akce

12. 5. 2014

Typ akce podle státní příslušnosti

WRD - Celosvětová akce

Kód UT WoS článku

000352130800040