Search for the Cosmic Neutrino Background

Result code in 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>

Result on the web

<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>

Result language

angličtina

Original language name

Search for the Cosmic Neutrino Background

Original language description

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.

Czech name

—

Czech description

—

Type

D - Article in proceedings

CEP classification

BG - Nuclear, atomic and molecular physics, accelerators

OECD FORD branch

—

Project

<a href="/en/project/LM2011027" target="_blank" >LM2011027: Project LSM/ULISSE ? contribution of the Czech Republic to the extension of the large research infrastructure of European importance (underground laboratory and construction of SuperNEMO experiment, continuation of the Czech participation)</a><br>

Continuities

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

Publication year

2015

Confidentiality

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

Article name in the collection

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

ISBN

—

ISSN

1742-6588

e-ISSN

—

Number of pages

6

Pages from-to

1-6

Publisher name

IOP Publishing

Place of publication

London

Event location

Ischia

Event date

May 12, 2014

Type of event by nationality

WRD - Celosvětová akce

UT code for WoS article

000352130800040