The diffuse supernova neutrino flux, supernova rate and SN1987A

Lunardini, Cecilia

doi:10.1016/j.astropartphys.2006.06.008

Cited by 62 publications

(107 citation statements)

References 73 publications

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“…This limit approaches the theoretical predictions [2,3,4,5,6,7,8,9,10,11,12,13,14,15,16], thus arising the expectation that the DSNνF may be seen in the near future, and triggering several theoretical studies on the subject (see e.g. the review [17] and references therein).…”

Section: Introductionmentioning

confidence: 72%

“…This is expected, since softer neutrino spectrum means smaller fraction of the total energy above the SK threshold. A further loosening of the luminosity constraint is expected if the uncertainty on the supernova rate is included [15].…”

Section: Interpretation Of the Results: Luminosity Boundsmentioning

confidence: 99%

“…In both columns we see large differences, due to the different input quantities and constraints that are used in calculating the DSNνF. For example, to describe the DSNνF energy spectrum some authors use neutrino spectra that result from calculations of neutrino transport (e.g., [21]), while others use spectra that fit the SN1987A data [15] or simply adopt thermal spectra with temperatures varying within indicative intervals [44]. This diversity of approaches results in the variation E 0 = 3.8−8.…”

Section: Neutrinos From Core Collapse and The Diffuse Fluxmentioning

confidence: 99%

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Upper limits on the diffuse supernova neutrino flux from the SuperKamiokande data

Lunardini

Peres

2008

J. Cosmol. Astropart. Phys.

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We analyze the 1496 days of SuperKamiokande data to put limits on the ν e ,ν e , ν µ + ν τ andν µ +ν τ components of the diffuse flux of supernova neutrinos, in different energy intervals and for different neutrino energy spectra. By considering the presence of only one component at a time, we find the following bounds at 90% C.L. and for neutrino energy E > 19.3 MeV: Φ νe < 73.3 − 154 cm −2 s −1 , Φν e < 1.4 − 1.9 cm −2 s −1 , Φ νµ+ντ < (1.0 − 1.4) · 10 3 cm −2 s −1 and Φν µ+ντ < (1.3 − 1.8)·10 3 cm −2 s −1 , where the intervals account for varying the neutrino spectrum. In the interval E = 22.9 − 36.9 MeV, we find Φ νe < 39 − 54 cm −2 s −1 , which improves on the existing limit from SNO in the same energy window. Our results for ν µ + ν τ andν µ +ν τ improve by about four orders of magnitude over the previous best constraints from LSD.

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Section: Introductionmentioning

confidence: 72%

Section: Interpretation Of the Results: Luminosity Boundsmentioning

confidence: 99%

Section: Neutrinos From Core Collapse and The Diffuse Fluxmentioning

confidence: 99%

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Upper limits on the diffuse supernova neutrino flux from the SuperKamiokande data

Lunardini

Peres

2008

J. Cosmol. Astropart. Phys.

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“…It is also worth studying possible self-interaction effects in the phenomenology of SN 1987A neutrino events [55][56][57] and of the diffuse supernova neutrino background spectrum [58,59]. Further analytical and numerical developments may require to solve the neutrino evolution equations in the complete 3ν flavor scenario, where new effects associated to the "solar" δm 2 can occur; a recent example has been worked out in [60].…”

Section: Conclusion and Prospectsmentioning

confidence: 99%

Collective neutrino flavor transitions in supernovae and the role of trajectory averaging

Fogli

Lisi

Marrone

et al. 2007

J. Cosmol. Astropart. Phys.

273

397

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Abstract. Non-linear effects on supernova neutrino oscillations, associated with neutrino-neutrino interactions, are known to induce collective flavor transformations near the supernova core for θ 13 = 0. In scenarios with very shallow electron density profiles, these transformations have been shown to couple with ordinary matter effects, jointly producing spectral distortions both in normal and inverted hierarchy. In this work we consider a complementary scenario, characterized by higher electron density, as indicated by shock-wave simulations during a few seconds after bounce. In this case, early collective flavor transitions are decoupled from later, ordinary matter effects. Moreover, such transitions become more amenable to both numerical computations and analytical interpretations in inverted hierarchy, while they basically vanish in normal hierarchy. We numerically evolve the neutrino density matrix in the region relevant for self-interaction effects, using thermal spectra and a representative value sin 2 θ 13 = 10 −4 . In the approximation of averaged intersection angle between neutrino trajectories, our simulations neatly show the collective phenomena of synchronization, bipolar oscillations, and spectral split, with analytically understandable features, as recently discussed in the literature. In the more realistic (but computationally demanding) case of non-averaged neutrino trajectories, our simulations do not show new significant qualitative features, apart from the smearing of "fine structures" such as bipolar nutations. Our results seem to suggest that, at least for non-shallow matter density profiles, averaging over neutrino trajectories plays a minor role in the final outcome. In this case, the swap of ν e and ν µ,τ spectra above a critical energy may represent an unmistakable signature of the inverted neutrino hierarchy, especially for θ 13 small enough to render further (ordinary or even turbulent) matter effects irrelevant.PACS numbers: 14.60. Pq, 13.15.+g, 97.60.Bw Collective neutrino flavor transitions in supernovae and the role of trajectory averaging 2

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“…4.1), but such events are rare in the Milky Way. The guaranteed DSNB flux provides a way to detect SN neutrinos without a fortuitous burst [129][130][131][132][133][134][135][136][137][138][139][140][141][142][143][144][145][146][147]. DSNB signals depend on three ingredients.…”

Section: Basic Picturementioning

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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The diffuse supernova neutrino flux, supernova rate and SN1987A

Cited by 62 publications

References 73 publications

Upper limits on the diffuse supernova neutrino flux from the SuperKamiokande data

Upper limits on the diffuse supernova neutrino flux from the SuperKamiokande data

Collective neutrino flavor transitions in supernovae and the role of trajectory averaging

The next-generation liquid-scintillator neutrino observatory LENA

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