On the detection of cosmological neutrinos by coherent scattering

Langacker, Paul; Leveille, Jacques P.; Sheiman, Jon

doi:10.1103/physrevd.27.1228

Cited by 177 publications

(131 citation statements)

References 27 publications

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“…The distribution of background relic (anti)neutrinos f ν (P ) (fν(P )) assumes a relativistic Fermi-Dirac form, with β = 1/T ν and α = µ/T ν , µ being the chemical potential for neutrinos and T ν the temperature of the relic neutrino bath. It is worth remarking here that, although relic neutrinos are not relativistic anymore at present time, their distribution maintains a relativistic form since their interactions froze out at their decoupling time, corresponding to T νd ∼ 1 MeV [24]. After replacing the expressions above in eq.…”

mentioning

confidence: 99%

UHE neutrino damping in a thermal gas of relic neutrinos

D’Olivo

Nellen

Sahu

et al. 2006

Astroparticle Physics

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We present a calculation of the damping of an ultra-energetic cosmic neutrino (UHEν) travelling through the thermal gas of relic neutrinos, using the formalism of finite-temperature field theory. From the self-energy diagram due to Z exchange, we obtain the annihilation cross section for an UHEν interacting with an antineutrino from the background. This method allows us to derive the full expression for the UHEν transmission probability, taking into account the momentum of relic neutrinos. We discuss the effect of thermal motion on the shape of the absorption dips for different UHEν fluxes as well as in the context of relic neutrino clustering. We find that for ratios of the neutrino mass to the relic background temperature 10 2 or smaller, the thermal broadening of the absorption lines could significantly affect the determination of the neutrino mass and of the characteristics of the population of UHEν sources.

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confidence: 99%

UHE neutrino damping in a thermal gas of relic neutrinos

D’Olivo

Nellen

Sahu

et al. 2006

Astroparticle Physics

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“…Various strategies have been proposed so far, based on laboratories searches [5][6][7][8][9][10][11] and astrophysical observations [12][13][14][15][16], such as absorption dips in the flux of ultra high energy neutrinos (for a review see, e.g., [17]). As far as their detection in laboratory experiments is concerned, one needs to overcome two main obstacles: the low cross section characteristic of weak interactions and the low energy of relic neutrinos.…”

Section: Introductionmentioning

confidence: 99%

Charged current cross section for massive cosmological neutrinos impinging on radioactive nuclei

Lazauskas

Vogel

Volpe

2007

J. Phys. G: Nucl. Part. Phys.

107

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We discuss the cross section formula for both massless and massive neutrinos on stable and radioactive nuclei. The latter could be of interest for the detection of cosmological neutrinos whose observation is one of the main challenges of modern cosmology. We analyse the signal-to-background ratio as a function of the ratio m ν / , i.e. the neutrino mass over the detector resolution and show that an energy resolution 0.5 eV would be required for sub-eV neutrino masses, independently of the gravitational neutrino clustering. Finally, we mention the non-resonant character of neutrino capture on radioactive nuclei.

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“…Effects linear in G F do not exist, as was shown early on in Refs. [9,10], with one exception, proposed by Stodolsky [11] that, however, appears to be too complicated to be practical. Acceleration depending correctly on G 2 F was considered in e.g.…”

Section: Detection By Coherent Scatteringmentioning

confidence: 99%

How difficult it would be to detect cosmic neutrino background?

Vogel¹

2015

AIP Conference Proceedings

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Abstract. Possible ways of detecting the cosmic neutrino background are described and their difficulties discussed. Among them, the capture on the radioactive tritium nuclei is challenging, but perhaps doable. The principal difficulty is the need for the combination of a very strong source and very good detector resolution. It is argued that if it turns out that the neutrino masses follow the degenerate scenario, i.e. if m ν ≥ 0.1 eV for all three massive neutrinos, then it is important to devote a substantial effort to develop a realistic detection experiment.

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On the detection of cosmological neutrinos by coherent scattering

Cited by 177 publications

References 27 publications

UHE neutrino damping in a thermal gas of relic neutrinos

UHE neutrino damping in a thermal gas of relic neutrinos

Charged current cross section for massive cosmological neutrinos impinging on radioactive nuclei

How difficult it would be to detect cosmic neutrino background?

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