Precise quasielastic neutrino/nucleon cross-section

Струмиа, Алессандро; Vissani, Francesco

doi:10.1016/s0370-2693(03)00616-6

Cited by 471 publications

(521 citation statements)

References 39 publications

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“…The cross section is σ(E ν ) 9.42 × 10 −44 cm 2 (E ν /MeV−1.3) 2 at lowest order; we use the corrections to the cross section and kinematics from Refs. [179,180]. In LENA, the visible positron energy is its kinetic energy plus the annihilation energy with an electron, E vis = T e + 2m e c 2 (Super-Kamiokande defines visible energies via the positron total energy, E vis = T e + m e c 2 ).…”

Section: Dsnb Signalsmentioning

confidence: 99%

The next-generation liquid-scintillator neutrino observatory LENA

Wurm

Beacom

Bezrukov

et al. 2012

Astroparticle Physics

212

200

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2As part of the European LAGUNA design study on a next-generation neutrino detector, we propose the liquid-scintillator detector LENA (Low Energy Neutrino Astronomy) as a multipurpose neutrino observatory. The outstanding successes of the Borexino and KamLAND experiments demonstrate the large potential of liquid-scintillator detectors in low-energy neutrino physics. Low energy threshold, good energy resolution and efficient background discrimination are inherent to the liquidscintillator technique. A target mass of 50 kt will offer a substantial increase in detection sensitivity.At low energies, the variety of detection channels available in liquid scintillator will allow for an energy-and flavor-resolved analysis of the neutrino burst emitted by a galactic Supernova. Due to target mass and background conditions, LENA will also be sensitive to the faint signal of the Diffuse Supernova Neutrino Background. Solar metallicity, time-variation in the solar neutrino flux and deviations from MSW-LMA survival probabilities can be investigated based on unprecedented statistics. Low background conditions allow to search for dark matter by observing rare annihilation neutrinos. The large number of events expected for geoneutrinos will give valuable information on the abundances of Uranium and Thorium and their relative ratio in the Earth's crust and mantle. Reactor neutrinos enable a high-precision measurement of solar mixing parameters. A strong radioactive or pion decay-at-rest neutrino source can be placed close to the detector to investigate neutrino oscillations for short distances and sub-MeV to MeV energies.At high energies, LENA will provide a new lifetime limit for the SUSY-favored proton decay mode into kaon and antineutrino, surpassing current experimental limits by about one order of magnitude. Recent studies have demonstrated that a reconstruction of momentum and energy of GeV particles is well feasible in liquid scintillator. Monte Carlo studies on the reconstruction of the complex event topologies found for neutrino interactions at multi-GeV energies have shown promising results. If this is confirmed, LENA might serve as far detector in a long-baseline neutrino oscillation experiment currently investigated in LAGUNA-LBNO.3

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Section: Dsnb Signalsmentioning

confidence: 99%

The next-generation liquid-scintillator neutrino observatory LENA

Wurm

Beacom

Bezrukov

et al. 2012

Astroparticle Physics

212

200

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“…Theν e + p → e + + n cross section parametrization of Vogel & Beacom (1999), which is in good agreement with Strumia & Vissani (2003), was used. Positron annihilation and hydrogen capture of neutrons produce photons of 0.51 MeV and 2.22 MeV energy, respectively.…”

Section: Cherenkov Photon Signal In Icecubementioning

confidence: 99%

IceCube sensitivity for low-energy neutrinos from nearby supernovae

Abbasi¹,

Abdou²,

Abu‐Zayyad³

et al. 2011

A&A

138

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This paper describes the response of the IceCube neutrino telescope located at the geographic south pole to outbursts of MeV neutrinos from the core collapse of nearby massive stars. IceCube was completed in December 2010 forming a lattice of 5160 photomultiplier tubes that monitor a volume of ∼1 km 3 in the deep Antarctic ice for particle induced photons. The telescope was designed to detect neutrinos with energies greater than 100 GeV. Owing to subfreezing ice temperatures, the photomultiplier dark noise rates are particularly low. Hence IceCube can also detect large numbers of MeV neutrinos by observing a collective rise in all photomultiplier rates on top of the dark noise. With 2 ms timing resolution, IceCube can detect subtle features in the temporal development of the supernova neutrino burst. For a supernova at the galactic center, its sensitivity matches that of a background-free megaton-scale supernova search experiment. The sensitivity decreases to 20 standard deviations at the galactic edge (30 kpc) and 6 standard deviations at the Large Magellanic Cloud (50 kpc). IceCube is sending triggers from potential supernovae to the Supernova Early Warning System. The sensitivity to neutrino properties such as the neutrino hierarchy is discussed, as well as the possibility to A109, page 1 of 18 detect the neutronization burst, a short outbreak of ν e 's released by electron capture on protons soon after collapse. Tantalizing signatures, such as the formation of a quark star or a black hole as well as the characteristics of shock waves, are investigated to illustrate IceCube's capability for supernova detection.

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“…[28] for this particular aspect). The experimental parameters, such as efficiency curves and energy resolution functions, are as in [43], and the detection cross section was taken from [50] (Eq. (25) there).…”

Section: The Data Analysismentioning

confidence: 99%

The diffuse supernova neutrino flux, supernova rate and SN1987A

Lunardini

2006

Astroparticle Physics

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I calculate the diffuse flux of electron antineutrinos from all supernovae using the information on the neutrino spectrum from SN1987A and the information on the rate of supernovae from direct supernova observations. The interval of flux allowed at 99% confidence level is ∼ 0.05 − 0.35 cm −2 s −1 above the SuperKamiokande (SK) energy cut of 19.3 MeV. This result is at least a factor of ∼ 4 smaller than the current SK upper limit of 1.2 cm −2 s −1 , thus motivating the experimental efforts to lower the detection energy threshold or to upgrade to higher volumes. A Megaton water Cherenkov detector with ∼ 90% efficiency would record ∼ 2 − 44 inverse beta decay events a year depending on the energy cut.

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Precise quasielastic neutrino/nucleon cross-section

Cited by 471 publications

References 39 publications

The next-generation liquid-scintillator neutrino observatory LENA

The next-generation liquid-scintillator neutrino observatory LENA

IceCube sensitivity for low-energy neutrinos from nearby supernovae

The diffuse supernova neutrino flux, supernova rate and SN1987A

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