Galactic abundances as a relic neutrino detection scheme

We propose to use the threshold-free process of neutrino capture on β-decaying nuclei (NCB) with all available candidate nuclei in the Milky Way as target material in order to detect the presence of the Cosmic Neutrino Background (CνB). By integrating over the lifetime of the galaxy one might be abl...

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Bibliographic Details
Published in:Journal of cosmology and astroparticle physics 2011-09, Vol.2011 (9), p.19-19
Main Authors: Riis, Anna S, Zinner, Nikolaj T, Hannestad, Steen
Format: Article
Language:English
Subjects:
APPROXIMATIONS
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BETA DECAY
CAPTURE
COHERENT SCATTERING
COMPARATIVE EVALUATIONS
COSMIC NEUTRINOS
CROSS SECTIONS
DE BROGLIE WAVELENGTH
LANTHANUM 138
LIFETIME
MILKY WAY
NEUTRINO DETECTION
RHENIUM 187
SUPERNOVAE
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Summary:We propose to use the threshold-free process of neutrino capture on β-decaying nuclei (NCB) with all available candidate nuclei in the Milky Way as target material in order to detect the presence of the Cosmic Neutrino Background (CνB). By integrating over the lifetime of the galaxy one might be able to see the effect of NCB processes as a slightly eschewed abundance ratio of selected β-decaying nuclei. First, the candidates must be chosen so that both the mother and daughter nuclei have a lifetime comparable to that of the Milky Way or the signal could be easily washed out by additional decays. Secondly, relic neutrinos have so low energy that their de Broglie wavelengths are macroscopic and they may therefore scatter coherently on the electronic cloud of the candidate atoms. One must therefore compare the cross sections for the two processes (induced β-decay by neutrino capture, and coherent scattering of the neutrinos on atomic nuclei) before drawing any conclusions. Finally, the density of target nuclei in the galaxy must be calculated. We assume supernovae as the only production source and approximate the neutrino density as a homogenous background. Here we perform the full calculation for {sup 187}Re and {sup 138}La and find that one needs abundance measurements with 24 digit precision in order to detect the effect of relic neutrinos. Or alternatively an enhancement of ρ{sub ν} by a factor of ∼ 10{sup 15} to produce an effect within the current abundance measurement precision.
ISSN:1475-7516
1475-7516
DOI:10.1088/1475-7516/2011/09/019