Journal articles: 'Neutrino'

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Daywitt, William C. "The Neutrino Decay of the Free Neutron and the Neutrino Structure According to the Planck Vacuum Theory." European Journal of Engineering and Technology Research 6, no. 5 (July 27, 2021): 73–75. http://dx.doi.org/10.24018/ejers.2021.6.5.2524.

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The Planck vacuum (PV) theory derives equations for the neutrino and antineutrino, and relates them to the unstable free neutron and antineutron. Remarkably, these neu- trons and neutrinos share the same wavefunction solutions that describe the proton and electron and their antiparticle cores. The neutrino and antineutrino are chargeless and massless; so their propagation through matter goes unnoticed, making these neutrinos invisible. The equations to follow that describe these pseudo-particles are the theoretical embodiment of the circa 1930 Pauli neutrino hypothesis. Finally, depending on one’s perspective, the neutrons can be viewed as decaying meta-particles or as stable nuclear particles.

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Daywitt, William C. "The Neutrino Decay of the Free Neutron and the Neutrino Structure According to the Planck Vacuum Theory." European Journal of Engineering and Technology Research 6, no. 5 (July 27, 2021): 73–75. http://dx.doi.org/10.24018/ejeng.2021.6.5.2524.

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The Planck vacuum (PV) theory derives equations for the neutrino and antineutrino, and relates them to the unstable free neutron and antineutron. Remarkably, these neu- trons and neutrinos share the same wavefunction solutions that describe the proton and electron and their antiparticle cores. The neutrino and antineutrino are chargeless and massless; so their propagation through matter goes unnoticed, making these neutrinos invisible. The equations to follow that describe these pseudo-particles are the theoretical embodiment of the circa 1930 Pauli neutrino hypothesis. Finally, depending on one’s perspective, the neutrons can be viewed as decaying meta-particles or as stable nuclear particles.

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Hargrove, C. K., and D. J. Paterson. "Solar-neutrino neutral-current detection methods in the Sudbury neutrino observatory." Canadian Journal of Physics 69, no. 11 (November 1, 1991): 1309–16. http://dx.doi.org/10.1139/p91-196.

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The Sudbury Neutrino Observatory will study the solar-neutrino problem through the detection of charged-current (CC), neutral-current (NC), and elastic-scattering (ES) interactions of solar neutrinos with heavy water. The measurement of the NC rate relative to the CC rate provides a nearly model-independent method of observing neutrino oscillations. The NC interaction breaks up the deuteron producing a neutron and a proton. The interaction rate in the original design is measured by observing Čerenkov light from showers produced by neutron-capture γ rays from the capture of the NC neutrons by a selected additive to the heavy water. These signals overlap the CC and ES signals, so that the measurement of the NC rate requires the subtraction of two signals obtained at different times. This paper describes our investigation of an alternate detection method in which the thermalized neutrons are captured by (n, α) or (n, p) reactions on light nuclei. The resulting charged-particle products are uniquely detected by scintillators or proportional counters, completely separating this NC signal from the CC and ES Čerenkov signals, thus simplifying its measurement, improving its significance, and allowing observation of otherwise unobservable short-term NC fluctuations. Although background rates for the new techniques have not yet been determined, the experimental advantages justify further development work.

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Caravaca, J. "SNO: Recent new results." International Journal of Modern Physics A 35, no. 34n35 (December 15, 2020): 2044012. http://dx.doi.org/10.1142/s0217751x20440121.

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The Sudbury Neutrino Observatory (SNO), whose main purpose was to study the neutrinos produced in the Sun, demonstrated that neutrinos can change flavor and, thus, they are massive particles. SNO detected and recorded neutrino and cosmic ray interactions from 1999 to 2006 and several analyses have been completed in the past year using legacy data. We present the results of the most recent ones: the measurements of neutron production in atmospheric neutrino interactions and neutron production by cosmic muons, a search for Lorentz symmetry violation in neutrino oscillations and a search for neutrino decay. A few other analyses are ongoing and we comment about their goal and status.

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Vergados, J. D., and Y. Giomataris. "Neutral current coherent cross-sections — Implications on detecting SN and earth neutrinos with gaseous spherical TPC’s." International Journal of Modern Physics E 26, no. 01n02 (January 2017): 1740030. http://dx.doi.org/10.1142/s0218301317400304.

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The detection of galactic supernova (SN) neutrinos represents one of the future frontiers of low energy neutrino physics and astrophysics. The neutron coherence of neutral currents (NCs) allows quite large cross-sections in the case of neutron rich targets, which can be exploited in detecting earth and sky neutrinos by measuring nuclear recoils. They are relatively cheap and easy to maintain. These (NC) cross-sections are not dependent on flavor conversions and, thus, their measurement will provide useful information about the neutrino source. In particular, they will yield information about the primary neutrino fluxes and perhaps about the spectrum after flavor conversions in neutrino sphere. They might also provide some clues about the neutrino mass hierarchy. The advantages of large gaseous low threshold and high resolution time projection counters (TPC) detectors are discussed.

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Chen, Zekun, Konstantin Kouzakov, Yu-Feng Li, Vadim Shakhov, Konstantin Stankevich, and Alexander Studenikin. "Collective neutrino oscillations in moving and polarized matter." Journal of Physics: Conference Series 2156, no. 1 (December 1, 2021): 012180. http://dx.doi.org/10.1088/1742-6596/2156/1/012180.

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Abstract We consider neutrino evolution master equations in dense moving and polarized matter consisted of electrons, neutrons, protons and neutrinos. We also take into account the neutrino magnetic moment interaction with a magnetic field. We point out the mechanisms responsible for the neutrino spin precession and provide the expressions for the corresponding interaction Hamiltonians that should be taken into account in theoretical treatments of collective neutrino oscillations.

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Tsakstara, V., and T. S. Kosmas. "Studying the coherent channel of neutral current ν-nucleus interaction." HNPS Proceedings 21 (March 8, 2019): 177. http://dx.doi.org/10.12681/hnps.2029.

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Original cross-sections calculations for neutral current neutrino scattering on 40Ar isotope are performed in the context of the quasi-particle random phase approximation (QRPA) by utilizing realistic two-nucleon forces. The incoming neutrino energy range adopted, εν ≤ 100 MeV, covers the supernova neutrinos, the low-energy beta-beam-neutrinos and the pion-muon stopped neutrino-beams existing or planned to be conducted at future neutron spallation sources. Subsequently, are the original cross sections convoluted with various supernova neutrino-energy distributions such as the two-parameter Fermi-Dirac and the power law distributions. The folded cross sections are obtained for various values of the parameters of these neutrino energy distributions corresponding to different supernova scenarios. One of the main purposes of this work is to explore the response of the 40Ar isotope as supernova neutrino detector.

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Mathews, G. J., L. Boccioli, J. Hidaka, and T. Kajino. "Review of uncertainties in the cosmic supernova relic neutrino background." Modern Physics Letters A 35, no. 25 (July 15, 2020): 2030011. http://dx.doi.org/10.1142/s0217732320300116.

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We review the computation of and associated uncertainties in the current understanding of the relic neutrino background due to core-collapse supernovae, black hole formation and neutron star merger events. We consider the current status of uncertainties due to the nuclear equation of state (EoS), the progenitor masses, the source supernova neutrino spectrum, the cosmological star formation rate, the stellar initial mass function, neutrino oscillations, and neutrino self-interactions. We summarize the current viability of future neutrino detectors to distinguish the nuclear EoS and the temperature of supernova neutrinos via the detected relic supernova neutrino spectrum.

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Chakraborty, Sabyasachi, Aritra Gupta, and Miguel Vanvlasselaer. "Anomaly induced cooling of neutron stars: a Standard Model contribution." Journal of Cosmology and Astroparticle Physics 2023, no. 10 (October 1, 2023): 030. http://dx.doi.org/10.1088/1475-7516/2023/10/030.

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Abstract Young neutron stars cool via the emission of neutrinos from their core. A precise understanding of all the different processes producing neutrinos in the hot and degenerate matter is essential for assessing the cooling rate of such stars. The main Standard Model processes contributing to this effect are ν bremsstrahlung, mURCA among others. In this paper, we investigate another Standard Model process initiated by the Wess-Zumino-Witten term, leading to the emission of neutrino pairs via Nγ → Nνν̅. We find that for proto-neutron stars, such processes with degenerate neutrons can be comparable and even dominate over the typical and well-known cooling mechanisms.

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Gutiérrez, Miguel, Manuel Masip, and Sergio Muñoz. "The Solar Disk at High Energies." Astrophysical Journal 941, no. 1 (December 1, 2022): 86. http://dx.doi.org/10.3847/1538-4357/aca020.

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Abstract High energy cosmic rays illuminate the Sun and produce an image that could be observed in up to five different channels: a cosmic-ray shadow (whose energy dependence has been studied by HAWC); a gamma-ray flux (observed at E ≤ 200 GeV by Fermi-LAT); a muon shadow (detected by ANTARES and IceCube); a neutron flux (undetected, as there are no hadronic calorimeters in space); a flux of high energy neutrinos. Since these signals are correlated, the ones already observed can be used to reduce the uncertainty in the still undetected ones. Here we define a simple setup that uses the Fermi-LAT and HAWC observations to imply very definite fluxes of neutrons and neutrinos from the solar disk. In particular, we provide a fit of the neutrino flux at 10 GeV–10 TeV that includes its dependence on the zenith angle and on the period of the solar cycle. This flux represents a neutrino floor in indirect dark matter searches. We show that in some benchmark models the current bounds on the dark matter–nucleon cross section push the solar signal below this neutrino floor.

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11

Regmi, Jeevan. "Neutrinos." Himalayan Physics 3 (January 1, 2013): 64–68. http://dx.doi.org/10.3126/hj.v3i0.7308.

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Neutrinos are one of the fundamental particles that make the universe. They are produced by the decay of radioactive elements and are elementary particles that lack the electric charge. The name neutrino was coined by Enrico Fermi as a word play on neutrone, the Italian name of the neutron. Of all high-energy particles, only weakly interacting neutrinos can directly convey astronomical information from the edge of the universe and from deep inside the most cataclysmic high energy process.The Himalayan PhysicsVol. 3, No. 3, July 2012Page : 64-68

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12

KISSLINGER, LEONARD S. "SUPERNOVAE, LANDAU LEVELS, AND PULSAR KICKS." Modern Physics Letters A 22, no. 25n28 (September 14, 2007): 2071–80. http://dx.doi.org/10.1142/s0217732307025315.

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We derive the energy asymmetry given the proto-neutron star during the time when the neutrino sphere is near the surface of the proto-neutron star, using the modified URCA process. The electrons produced with the anti-neutrinos are in Landau levels due to the strong magnetic field, and this leads to asymmetry in the neutrino momentum, and a pulsar kick. Our main prediction is that the large pulsar kicks start at about 10 s and last for about 10 s, with the corresponding neutrinos correlated in the direction of the magnetic field.

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Grange, Joseph, and Teppei Katori. "Charged current quasi-elastic cross-section measurements in MiniBooNE." Modern Physics Letters A 29, no. 12 (April 20, 2014): 1430011. http://dx.doi.org/10.1142/s0217732314300110.

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The neutrino-induced charged-current quasi-elastic (CCQE, νl + n → l- + p or [Formula: see text]) interaction is the most abundant interaction around 1 GeV, and it is the most fundamental channel to study neutrino oscillations. Recently, MiniBooNE published both muon neutrino1 and muon anti-neutrino2 double differential cross-sections on carbon. In this review, we describe the details of these analyses and include some historical remarks.

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Kotila, Jenni. "Rare weak decays and neutrino mass." Journal of Physics: Conference Series 2453, no. 1 (March 1, 2023): 012012. http://dx.doi.org/10.1088/1742-6596/2453/1/012012.

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Abstract The question whether neutrinos are Majorana fermions (i.e., their own anti-particles) remains among the most fundamental open questions of subatomic physics. If neutrinos are Majorana particles it would revolutionize our understanding of physics. Although neutrinoless double beta decay, 0νββ, was proposed more than 80 years ago to establish the nature of neutrinos, it remains the most sensitive probe into the non-conservation of lepton number. 0νββ-decay is a postulated extremely slow and yet unobserved radioactive process in which two neutrons (or protons) inside a nucleus transform into two protons (or neutrons) emitting two electrons (or positrons), respectively, but no neutrinos. Its observation would be a breakthrough in the description of elementary particles and would provide fundamental information on the neutrino masses, their nature, and origin. In this paper double beta decay, its connection to neutrino mass, and mechanisms beyond the standard mass mechanism are discussed from a theoretical point of view. The current situation is then addressed by combining theoretical results with recent experimental limits.

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15

DUTTA, SUKANTA, ASHOK GOYAL, and S. R. CHOUDHURY. "ON PION COOLING IN THE SUPERNOVA CORE." International Journal of Modern Physics A 13, no. 06 (March 10, 1998): 915–21. http://dx.doi.org/10.1142/s0217751x9800041x.

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We examine the cooling mechanism of a nascent neutron star core by the emission of wrong helicity neutrinos, when the core is at the verge of pion condensation. We study the dominant process [Formula: see text] due to neutrino magnetic moment in terms of the model-independent multipole amplitudes based on dispersion relation theory. This calculation gives a more realistic emission rate for neutrinos and hence an upper bound for neutrino magnetic moment

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Adhya, Souvik Priyam. "Astrophysical Aspects of Neutrino Dynamics in Ultradegenerate Quark Gluon Plasma." Advances in High Energy Physics 2017 (2017): 1–11. http://dx.doi.org/10.1155/2017/1273931.

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The cardinal focus of the present review is to explore the role of neutrinos originating from the ultradense core of neutron stars composed of quark gluon plasma in the astrophysical scenario. The collective excitations of the quarks involving the neutrinos through the different kinematical processes have been studied. The cooling of the neutron stars as well as pulsar kicks due to asymmetric neutrino emission has been discussed in detail. Results involving calculation of relevant physical quantities like neutrino mean free path and emissivity have been presented in the framework of non-Fermi liquid behavior as applicable to ultradegenerate plasma.

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Verma, Rishu, Monal Kashav, Ankush B, Gazal Sharma, Surender Verma, and B. C. Chauhan. "Texture One Zero Model Based on A4 Flavor Symmetry and its Implications to Neutrinoless Double Beta Decay." Journal of Nuclear Physics, Material Sciences, Radiation and Applications 9, no. 1 (August 31, 2021): 67–71. http://dx.doi.org/10.15415/jnp.2021.91012.

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Neutrinos are perhaps the most elusive particles in our Universe. Neutrino physics could be counted as a benchmark for various new theories in elementary particle physics and also for the better understanding of the evolution of the Universe. To complete the neutrino picture, the missing information whether it is about their mass or their nature that the neutrinos are Majorana particles could be provided by the observation of a process called neutrinoless double beta (0νββ) decay. Neutrinoless double beta decay is a hypothesised nuclear process in which two neutrons simultaneously decay into protons with no neutrino emission. In this paper we proposed a neutrino mass model based on A4 symmetry group and studied its implications to 0νββ decay. We obtained a lower limit on |Mee| for inverted hierarchy and which can be probed in 0νββ experiments like SuperNEMO and KamLAND-Zen.

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18

Abe, K., Y. Haga, Y. Hayato, K. Hiraide, K. Ieki, M. Ikeda, S. Imaizumi, et al. "Neutron tagging following atmospheric neutrino events in a water Cherenkov detector." Journal of Instrumentation 17, no. 10 (October 1, 2022): P10029. http://dx.doi.org/10.1088/1748-0221/17/10/p10029.

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Abstract We present the development of neutron-tagging techniques in Super-Kamiokande IV using a neural network analysis. The detection efficiency of neutron capture on hydrogen is estimated to be 26%, with a mis-tag rate of 0.016 per neutrino event. The uncertainty of the tagging efficiency is estimated to be 9.0%. Measurement of the tagging efficiency with data from an Americium-Beryllium calibration agrees with this value within 10%. The tagging procedure was performed on 3,244.4 days of SK-IV atmospheric neutrino data, identifying 18,091 neutrons in 26,473 neutrino events. The fitted neutron capture lifetime was measured as 218±9 μs.

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Saez, M. M., O. Civitarese, and M. E. Mosquera. "Neutrino mixing in nuclear rapid neutron-capture processes." International Journal of Modern Physics E 29, no. 04 (April 2020): 2050022. http://dx.doi.org/10.1142/s0218301320500226.

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A possible mechanism for the formation of heavy-mass elements in supernovae is the rapid neutron-capture-mechanism ([Formula: see text]-process). It depends upon the electron-fraction [Formula: see text], a quantity which is determined by beta-decay-rates. In this paper, we focus on the calculation of electroweak decay-rates in presence of massive neutrinos. The resulting expressions are then used to calculate nuclear reactions entering the rapid-neutron capture. We fix the astrophysical parameters to the case of a core-collapse supernova. The neutrino sector includes a mass scheme and mixing angles for active neutrinos, and also by including the mixing between active and sterile neutrinos. The results of the calculations show that the predicted abundances of heavy-mass nuclei are indeed affected by the neutrino mixing.

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Volpe, Maria Cristina. "Neutrinos : from the r-process to the diffuse supernova neutrino background." Journal of Physics: Conference Series 2156, no. 1 (December 1, 2021): 012126. http://dx.doi.org/10.1088/1742-6596/2156/1/012126.

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Abstract Neutrinos from dense environments are connected to the longstanding open questions of how massive stars explode and what are the sites where r-process elements are made. Flavor evolution and neutrino properties can influence nucleosynthetic abundances. GW170817 has given indirect evidence for r-process elements in binary neutron star mergers. We discuss the impact of non-standard interactions in such sites. Nearby compact objects, strong gravitational fields are present. We discuss their influence upon neutrino decoherence in a wave packet treatment of neutrino propagation. We conclude by mentioning the upcoming measurement of the diffuse supernova neutrino background.

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Ayala, Alejandro, Santiago Bernal-Langarica, S. Hernández-Ortiz, L. A. Hernández, and D. Manreza-Paret. "Lower bound for the neutrino magnetic moment from kick velocities induced at the birth of neutron stars." International Journal of Modern Physics E 30, no. 05 (May 2021): 2150031. http://dx.doi.org/10.1142/s0218301321500312.

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We show that the neutrino chirality flip, which can take place in the core of a neutron star at birth, is an efficient process to allow neutrinos to anisotropically escape, thus providing a to induce the neutron star kick velocities. The process is not subject to the no-go theorem since although the flip from left- to right-handed neutrinos happens at equilibrium, the reverse process does not take place given that right-handed neutrinos do not interact with matter and therefore detailed balance is lost. For simplicity, we model the neutron star core as being made of strange quark matter. We find that the process is efficient when the neutrino magnetic moment is not smaller than [Formula: see text], where [Formula: see text] is the Bohr magneton. When this lower bound is combined with the most stringent upper bound, which uses the luminosity data obtained from the analysis of SN 1987A, our results set a range for the neutrino magnetic moment given by [Formula: see text]. The obtained kick velocities for natal conditions are consistent with the observed ones and span the correct range of radii for typical magnetic field intensities.

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Morales, G., and N. Fraija. "Neutrino propagation in winds around the central engine of sGRB." Monthly Notices of the Royal Astronomical Society 505, no. 4 (May 31, 2021): 4968–80. http://dx.doi.org/10.1093/mnras/stab1577.

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ABSTRACT Since neutrinos can escape from dense regions without being deflected, they are promising candidates to study the new physics at the sources that produce them. With the increasing development of more sensitive detectors in the coming years, we will infer several intrinsic properties from incident neutrinos. In particular, we centralize our study in those produced by thermal processes in short gamma-ray bursts (sGRBs) and their interactions within the central engine’s anisotropic medium. On the one hand, we consider baryonic winds produced with a strong magnetic contribution, and on the other hand, we treat only neutrino-driven winds. First, we obtain the effective neutrino potential considering both baryonic density profiles around the central engine. Then, we get the three-flavour oscillation probabilities in this medium to finally calculate the expected neutrino ratios. We find a stronger angular dependence on the expected neutrino ratios, which, incidentally, contrast from the expected theoretical ratios without considering the winds’ additional contribution. The joint analysis of this observable, together with the sGRB ejected jet angle, might lead to an effective mechanism to discriminate between the involved merger progenitors (black hole-neutron star (BH-NS) or neutron-star neutron-star(NS-NS)), acting as an additional detection channel to gravitational waves.

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Lu, Jianlong, Aik Hui Chan, and Choo Hiap Oh. "A Phenomenological Model of Effectively Oscillating Massless Neutrinos and Its Implications." EPJ Web of Conferences 240 (2020): 02002. http://dx.doi.org/10.1051/epjconf/202024002002.

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We discuss an alternative picture of neutrino oscillation. In this phenomenological model, the flavor-changing phenomena of massless neutrinos arise from scattering processes between neutrinos and four types of undetected spin-0 massive particles pervading throughout the Universe, instead of neutrinos’ own nature. These scattering processes are kinematically similar to Compton scattering. One type of left-handed massless sterile neutrino is needed in order to reproduce the neutrino oscillation modes predicted in the theory of neutrino mixing. Implications of our model include the existence of sterile neu- trinos, the nonconservation of active neutrinos, the possible mismatch among three neutrino mass squared diﬀerences ∆m2ij interpreted in the theory of neutrino mixing, the spacetime dependence of neutrino oscillation, and the impossibility of neutrinoless double beta decay. Several important open problems in neutrino physics become trivial or less severe in our model, such as the smallness of neutrino masses, neutrino mass hierarchy, the mechanism responsible for neutrino masses, and the Dirac/Majorana nature of neutrinos.

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Kajita, Takaaki. "Atmospheric Neutrinos." Advances in High Energy Physics 2012 (2012): 1–24. http://dx.doi.org/10.1155/2012/504715.

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Atmospheric neutrinos are produced as decay products in hadronic showers resulting from collisions of cosmic rays with nuclei in the atmosphere. Electron-neutrinos and muon-neutrinos are produced mainly by the decay chain of charged pions to muons to electrons. Atmospheric neutrino experiments observed zenith angle and energy-dependent deficit of muon-neutrino events. It was found that neutrino oscillations between muon-neutrinos and tau-neutrinos explain these data well. This paper discusses atmospheric neutrino experiments and the neutrino oscillation studies with these neutrinos.

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Mishra, Rakesh Kumar. "The Universe: Search for Neutrino on Earth." British Journal of Multidisciplinary and Advanced Studies 4, no. 1 (February 15, 2023): 33–62. http://dx.doi.org/10.37745/bjmas.2022.0114.

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Our planet is bombarded with trillions of particles, from Space from all direction called “Cosmic Rays”. The cosmic rays are made of tiny ‘elementary” particles such as photon, He, Neutrinos, Hydrogen and atomic nuclei have wide range of energies. Cosmic rays high energies suggest that they must be produced in the most energetic processes in the universe. As the cosmic rays particles have net electric charges they get deflected due to presence of geomagnetic fields during their travel and therefore do not travel in straight line. Cosmic rays particles can interact with matter and radiates at the sources to produced extremely particles called neutrino. Gamma rays radio Bursts of Electromagnetic energy in the form of gamma rays are the absolute, most energetic sources of energy known in the universe. The amount of energy that gamma ray bursts puts out in a few seconds is more than the Sun. every will in its entire life time.The neutrino, a fundamental elementary particles of nature, was born out of necessity to keep the conversvation of energy principle. In observed alpha,beta,and gamma decay. Although neutrinos are mot massless like photon of light, they have very special property. Neutrino are omnipresent in nature pass through every square centimeter of bodies without ever notice. Neutrino originate from events in the Universe such as Colloding of Black Holes,Gamma Ray Bursts from exploding stars and or violent event at core of distant Glaxies. A high energy of particles neutrino transform in to it’s particles lepton(electron,muon,ortauon).most accelerated Neutrino beam can also called muons , and few can create tauons. A detector which distinguished among these leptons can reveal the flavor of neutrino incident to charged particle current interaction because interaction involves the exchange of Boson the ‘target’ particle also change (e.g. neutron-proton).Netrinos detectors is a physics apparatus which is degined to study neutrinos, because neutrinos only weakly interact with other particles of matter, neutrino detector must very large to detect significant number of neutrinos. Confirmed extraterrestrial sources such as Sun,Super Nova1987A,

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Nakarmi, Prabandha, and Jeevan Jyoti Nakarmi. "Significance of neutrino-neutrino interaction in neutrino oscillation in core-collapse supernova." BIBECHANA 12 (December 17, 2014): 89–95. http://dx.doi.org/10.3126/bibechana.v12i0.11780.

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We study the possibility of neutrino-neutrino interaction inside the neutrino core of supernova (ρ ≥ 1010 g/cc) and outside the neutrinosphere. The angular dependence of the neutrino-neutrino interaction Hamiltonian causes multi-angle effects that can lead either to oscillation or free streaming of neutrinos. If the angle between interactions is π/2, the neutrinos are trapped inside neutrino core and chances of oscillation increases due to interaction. As the angle gradually changes, the chance of oscillation decreases and free streaming of neutrino can be observed out of core of supernova as shock waves.DOI: http://dx.doi.org/10.3126/bibechana.v12i0.11780 BIBECHANA 12 (2015) 89-95

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Shin, C. D., S. Ajimura, M. K. Cheoun, J. H. Choi, J. Y. Choi, T. Dodo, J. Goh, et al. "The acrylic vessel for JSNS²-II neutrino target." Journal of Instrumentation 18, no. 12 (December 1, 2023): T12001. http://dx.doi.org/10.1088/1748-0221/18/12/t12001.

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Abstract The JSNS2 (J-PARC Sterile Neutrino Search at J-PARC Spallation Neutron Source) is an experiment designed for the search for sterile neutrinos. The experiment is currently at the stage of the second phase named JSNS2-II with two detectors at near and far locations from the neutrino source. One of the key components of the experiment is an acrylic vessel, that is used for the target volume for the detection of the anti-neutrinos. The specifications, design, and measured properties of the acrylic vessel are described.

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INOUE, K. "REACTOR NEUTRINO EXPERIMENTS." International Journal of Modern Physics A 19, no. 08 (March 30, 2004): 1157–66. http://dx.doi.org/10.1142/s0217751x04019081.

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Previous searches for neutrino oscillations with reactor neutrinos have been done only with baselines less than 1 km. The observed neutrino flux was consistent with the expectation and only excluded regions were drawn on the neutrino-oscillation-parameter space. Thus, those experiments played important roles in understanding neutrinos from fission reactors. Based on the knowledge from those experiments, an experiment with about a 180 km baseline became possible. Results obtained from this baseline experiment showed evidence for reactor neutrino disappearance and finally provide a resolution for the long standing solar neutrino problem when combined with results from the solar neutrino experiments. Several possibilities to explore the last unmeasured mixing angle θ13 with reactor neutrinos have recently been proposed. They will provide complementary information to long baseline accelerator experiments when one tries to solve the degeneracy of oscillation parameters. Reactor neutrinos are also useful to study the neutrino magnetic moment and the most stringent limits from terrestrial experiments are obtained by measuring the elastic scattering cross section of reactor neutrinos.

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Brunner, Jürgen. "Measurement of Neutrino Oscillations with Neutrino Telescopes." Advances in High Energy Physics 2013 (2013): 1–16. http://dx.doi.org/10.1155/2013/782538.

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IceCube and ANTARES are the world-largest neutrino telescopes. They are successfully taking data, producing a wealth of scientific results. Whereas their main goal is the detection of cosmic neutrinos with energies in the TeV-PeV range, both have demonstrated their capability to measure neutrino oscillations by studying atmospheric neutrinos with energies of 10–50 GeV. After recalling the methods of these measurements and the first published results of these searches, the potential of existing, and planned low-energy extensions of IceCube and KM3Net are discussed. These new detectors will be able to improve the knowledge of the atmospheric neutrino oscillation parameters, and in particular they might help to understand the neutrino mass hierarchy. Such studies, which use atmospheric neutrinos, could be complemented by measurements in a long-baseline neutrino beam, which is discussed as a long-term future option.

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Ankush, Rishu Verma, Gazal Sharma, and B. C. Chauhan. "Investigating Sterile Neutrino Flux in the Solar Neutrino Data." Advances in High Energy Physics 2019 (June 2, 2019): 1–12. http://dx.doi.org/10.1155/2019/2598953.

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There are compelling evidences for the existence of a fourth degree of freedom of neutrinos, i.e., sterile neutrino. In the recent studies the role of sterile component of neutrinos has been found to be crucial, not only in particle physics, but also in astrophysics and cosmology. This has been proposed to be one of the potential candidates of dark matter. In this work we investigate the updated solar neutrino data available from all the relevant experiments including Borexino and KamLAND solar phase in a model independent way and obtain bounds on the sterile neutrino component present in the solar neutrino flux. The mystery of the missing neutrinos is further deepening as subsequent experiments are coming up with their results. The energy spectrum of solar neutrinos, as predicted by Standard Solar Models (SSM), is seen by neutrino experiments at different parts as they are sensitive to various neutrino energy ranges. It is interesting to note that more than 98% of the calculated standard model solar neutrino flux lies below 1 MeV. Therefore, the study of low energy neutrinos can give us better understanding and the possibility of knowing about the presence of antineutrino and sterile neutrino components in solar neutrino flux. As such, this work becomes interesting as we include the data from medium energy (~1 MeV) experiments, i.e., Borexino and KamLAND solar phase. In our study we retrieve the bounds existing in literature and rather provide more stringent limits on sterile neutrino (νs) flux available in solar neutrino data.

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Agafonova, Natalia, Walter Fulgione, Alexey Malgin, Konstantin Manukovskiy, Olga Ryazhskaya, Stanley Yen, and Andrey Yudin. "Possible explanation of the neutrino signal from SN1987A detected with the LSD." EPJ Web of Conferences 191 (2018): 03004. http://dx.doi.org/10.1051/epjconf/201819103004.

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On February 23 1987 in 2:52 UT the neutrino telescope LSD under Mont Blanc detected neutrino signal, which could not be explained within the framework of the standard collapse model. We show that the LSD signal could be a consequence of the detection of gamma-quanta emitted from neutron-capture reactions on by iron nuclei contained in the composition of the experimental setup. Neutrons are produced in neutrino-nuclei reactions in the surrounding granite rock and steel structures of the detector.

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Matsui, Riki, Shigeo S. Kimura, Kenji Toma, and Kohta Murase. "High-energy Neutrino Emission Associated with Gravitational-wave Signals: Effects of Cocoon Photons and Constraints on Late-time Emission." Astrophysical Journal 950, no. 2 (June 1, 2023): 190. http://dx.doi.org/10.3847/1538-4357/acd004.

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Abstract We investigate prospects for the detection of high-energy neutrinos produced in the prolonged jets of short gamma-ray bursts (sGRBs). The X-ray light curves of sGRBs show extended emission components lasting for 100–1000 s, which are considered to be produced by prolonged engine activity. Jets produced by such activity should interact with photons in the cocoon formed by the propagation of the jet inside the ejecta of neutron star mergers. We calculate neutrino emission from jets produced by prolonged engine activity, taking account of the interaction between photons provided from the cocoon and cosmic rays accelerated in the jets. We find that IceCube-Gen2, a future neutrino telescope, with second-generation gravitational-wave detectors will probably be able to observe neutrino signals associated with gravitational waves with around 10 years of operation, regardless of the assumed value of the Lorentz factor of the jets. Neutrino observations may enable us to constrain the dissipation region of the jets. We apply this model to GRB 211211A, a peculiar long GRB whose origin may be a binary neutron star merger. Our model predicts that IceCube is unlikely to detect any associated neutrinos, but a few similar events will be able to put a meaningful constraint on the physical quantities of the prolonged engine activities.

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Argüelles, Carlos A., and Jordi Salvado. "Sterile Neutrinos with Neutrino Telescopes." Universe 7, no. 11 (November 9, 2021): 426. http://dx.doi.org/10.3390/universe7110426.

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Searches for light sterile neutrinos are motivated by the unexpected observation of an electron neutrino appearance in short-baseline experiments, such as the Liquid Scintillator Neutrino Detector (LSND) and the Mini Booster Neutrino Experiment (MiniBooNE). In light of these unexpected results, a campaign using natural and anthropogenic sources to find the light (mass-squared-difference around 1 eV2) sterile neutrinos is underway. Among the natural sources, atmospheric neutrinos provide a unique gateway to search for sterile neutrinos due to the broad range of baseline-to-energy ratios, L/E, and the presence of significant matter effects. Since the atmospheric neutrino flux rapidly falls with energy, studying its highest energy component requires gigaton-scale neutrino detectors. These detectors—often known as neutrino telescopes since they are designed to observe tiny astrophysical neutrino fluxes—have been used to perform searches for light sterile neutrinos, and researchers have found no significant signal to date. This brief review summarizes the current status of searches for light sterile neutrinos with neutrino telescopes deployed in solid and liquid water.

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Campion, S., J. D. Uribe-Suárez, J. D. Melon Fuksman, and J. A. Rueda. "MeV, GeV and TeV Neutrinos from Binary-Driven Hypernovae." Symmetry 15, no. 2 (February 3, 2023): 412. http://dx.doi.org/10.3390/sym15020412.

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We analyze neutrino emission channels in energetic (≳1052 erg) long gamma-ray bursts within the binary-driven hypernova model. The binary-driven hypernova progenitor is a binary system composed of a carbon-oxygen star and a neutron star (NS) companion. The gravitational collapse leads to a type Ic supernova (SN) explosion and triggers an accretion process onto the NS. For orbital periods of a few minutes, the NS reaches the critical mass and forms a black hole (BH). Two physical situations produce MeV neutrinos. First, during the accretion, the NS surface emits neutrino–antineutrino pairs by thermal production. We calculate the properties of such a neutrino emission, including flavor evolution. Second, if the angular momentum of the SN ejecta is high enough, an accretion disk might form around the BH. The disk’s high density and temperature are ideal for MeV-neutrino production. We estimate the flavor evolution of electron and non-electron neutrinos and find that neutrino oscillation inside the disk leads to flavor equipartition. This effect reduces (compared to assuming frozen flavor content) the energy deposition rate of neutrino–antineutrino annihilation into electron–positron (e+e−) pairs in the BH vicinity. We then analyze the production of GeV-TeV neutrinos around the newborn black hole. The magnetic field surrounding the BH interacts with the BH gravitomagnetic field producing an electric field that leads to spontaneous e+e− pairs by vacuum breakdown. The e+e− plasma self-accelerates due to its internal pressure and engulfs protons during the expansion. The hadronic interaction of the protons in the expanding plasma with the ambient protons leads to neutrino emission via the decay chain of π-meson and μ-lepton, around and far from the black hole, along different directions. These neutrinos have energies in the GeV-TeV regime, and we calculate their spectrum and luminosity. We also outline the detection probability by some current and future neutrino detectors.

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Abbasi, R., M. Ackermann, J. Adams, N. Aggarwal, J. A. Aguilar, M. Ahlers, M. Ahrens, et al. "IceCube Search for Neutrinos Coincident with Gravitational Wave Events from LIGO/Virgo Run O3." Astrophysical Journal 944, no. 1 (February 1, 2023): 80. http://dx.doi.org/10.3847/1538-4357/aca5fc.

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Abstract Using data from the IceCube Neutrino Observatory, we searched for high-energy neutrino emission from the gravitational-wave events detected by the advanced LIGO and Virgo detectors during their third observing run. We did a low-latency follow-up on the public candidate events released during the detectors’ third observing run and an archival search on the 80 confident events reported in the GWTC-2.1 and GWTC-3 catalogs. An extended search was also conducted for neutrino emission on longer timescales from neutron star containing mergers. Follow-up searches on the candidate optical counterpart of GW190521 were also conducted. We used two methods; an unbinned maximum likelihood analysis and a Bayesian analysis using astrophysical priors, both of which were previously used to search for high-energy neutrino emission from gravitational-wave events. No significant neutrino emission was observed by any analysis, and upper limits were placed on the time-integrated neutrino flux as well as the total isotropic equivalent energy emitted in high-energy neutrinos.

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MALLICK, RITAM, ABHIJIT BHATTACHARYYA, SANJAY K. GHOSH, and SIBAJI RAHA. "GENERAL RELATIVISTIC EFFECT ON THE ENERGY DEPOSITION RATE FOR NEUTRINO PAIR ANNIHILATION ABOVE THE EQUATORIAL PLANE ALONG THE SYMMETRY AXIS NEAR A ROTATING NEUTRON STAR." International Journal of Modern Physics E 22, no. 02 (February 2013): 1350008. http://dx.doi.org/10.1142/s0218301313500080.

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The estimate of the energy deposition rate (EDR) for neutrino pair annihilation has been carried out. The EDR for the neutrinos coming from the equatorial plane of a rotating neutron star is calculated along the rotation axis using the Cook–Shapiro–Teukolsky metric. The neutrino trajectories and hence the neutrinos emitted from the disk are affected by the redshift due to disk rotation and gravitation. The EDR is very sensitive to the value of the temperature and its variation along the disk. The rotation of the star has a negative effect on the EDR; it decreases with increase in rotational velocity.

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37

Balantekin, A. Baha, and Boris Kayser. "On the Properties of Neutrinos." Annual Review of Nuclear and Particle Science 68, no. 1 (October 19, 2018): 313–38. http://dx.doi.org/10.1146/annurev-nucl-101916-123044.

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This article reviews our present understanding of neutrino properties with a particular emphasis on observable differences between Majorana and Dirac neutrinos. We summarize current and future experimental efforts toward measuring neutrino properties and describe consequences of the Majorana versus Dirac nature of neutrinos on neutrino masses, neutrino decays, and neutrino electromagnetic properties.

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Abe, Seisho. "Nuclear de-excitation associated with neutrino-carbon interactions." Journal of Physics: Conference Series 2156, no. 1 (December 1, 2021): 012189. http://dx.doi.org/10.1088/1742-6596/2156/1/012189.

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Abstract Neutrino interactions in low energy regions below 30 MeV, where the experimental searches for supernova relic neutrino are conducted, have a large uncertainty due to complicated nuclear effects such as the Pauli blocking effect and de-excitation of a residual nucleus. Understanding the effect of nuclear de-excitation is especially critical since neutrons measured by liquid scintillator detectors can be emitted via de-excitation. We build a systematic method to predict nuclear de-excitation associated with neutrino-carbon interaction using TALYS and Geant4. This prediction is combined with the results of neutrino event generators, and we find a large increase in neutron multiplicity.

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Luo, Qinghuan. "Neutrinos from Relativistic Outflows of Fast Spinning Magnetars." Publications of the Astronomical Society of Australia 22, no. 2 (2005): 157–61. http://dx.doi.org/10.1071/as04069.

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AbstractPulsars may be born with a short rotation period of milliseconds with the magnetic field amplified through dynamo processes up to ∼1015–1016 G. Such millisecond magnetars spin down rapidly, emitting bursts of high-energy neutrinos and gamma rays. Specifically, acceleration of ions in both the polar gap (as in a normal pulsar) and the relativistic magnetar wind is considered. In both cases ions can be accelerated to ultra-high energies and these energetic ions can lead to production of high-energy neutrinos and gamma rays through interaction with thermal radiation from the hot neutron star or the heated inner boundary region of the stellar envelope as the result of the deposition of energy by the magnetar wind. The detectability of the neutrino flux by a kilometre-scale neutrino detector such as the planned IceCube neutrino observatory is discussed.

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SCHWIENHORST, REINHARD. "COLLIDING NEUTRINO BEAMS." Modern Physics Letters A 23, no. 32 (October 20, 2008): 2751–61. http://dx.doi.org/10.1142/s0217732308028193.

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From several neutrino oscillation experiments, we understand now that neutrinos have mass. However, we really do not know what mechanism is responsible for producing this neutrino mass. Current or planned neutrino experiments utilize neutrino beams and long-baseline detectors to explore flavor mixing but do not address the question of the origin of neutrino mass. In order to begin answering that question, neutrino interactions need to be explored at much higher energies. This paper outlines a program to explore neutrinos and their interactions with various particles through a series of experiments involving colliding neutrino beams.

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41

Sridhar, Navin, Brian D. Metzger, and Ke Fang. "High-energy Neutrinos from Gamma-Ray-faint Accretion-powered Hypernebulae." Astrophysical Journal 960, no. 1 (December 27, 2023): 74. http://dx.doi.org/10.3847/1538-4357/ad03e8.

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Abstract Hypernebulae are inflated by accretion-powered winds accompanying hyper-Eddington mass transfer from an evolved post-main-sequence star onto a black hole or neutron star companion. The ions accelerated at the termination shock—where the collimated fast disk winds and/or jet collide with the slower, wide-angled wind-fed shell—can generate high-energy neutrinos via hadronic proton–proton reactions, and photohadronic (p γ) interactions with the disk thermal and Comptonized nonthermal background photons. It has been suggested that some fast radio bursts (FRBs) may be powered by such short-lived jetted hyper-accreting engines. Although neutrino emission associated with the millisecond duration bursts themselves is challenging to detect, the persistent radio counterparts of some FRB sources—if associated with hypernebulae—could contribute to the high-energy neutrino diffuse background flux. If the hypernebula birth rate follows that of stellar-merger transients and common envelope events, we find that their volume-integrated neutrino emission—depending on the population-averaged mass-transfer rates—could explain up to ∼25% of the high-energy diffuse neutrino flux observed by the IceCube Observatory and the Baikal Gigaton Volume Detector Telescope. The time-averaged neutrino spectrum from hypernebula—depending on the population parameters—can also reproduce the observed diffuse neutrino spectrum. The neutrino emission could in some cases furthermore extend to >100 PeV, detectable by future ultra-high-energy neutrino observatories. The large optical depth through the nebula to Breit–Wheeler (γ γ) interaction attenuates the escape of GeV–PeV gamma rays coproduced with the neutrinos, rendering these gamma-ray-faint neutrino sources, consistent with the Fermi observations of the isotropic gamma-ray background.

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42

Bondar, Aleksandr, Alexey Buzulutskov, Aleksandr Burdakov, Evgeny Grishnyaev, Aleksandr Dolgov, Aleksandr Makarov, Sergey Polosatkin, Andrey Sokolov, Sergey Taskaev, and Lev Shekhtman. "Proposal for Neutron Scattering Systems for Calibration of Dark Matter Search and Low-Energy Neutrino Detectors." Siberian Journal of Physics 8, no. 3 (October 1, 2013): 27–38. http://dx.doi.org/10.54362/1818-7919-2013-8-3-27-38.

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The proposal of two neutron scattering systems for calibration of two-phase cryogenic avalanche detectors with high sensitivity being developed at Budker INP is presented. This kind of detectors is designed for the search of dark matter and low energy neutrino detection, in particular, coherent neutrino scattering on nuclei. Detector calibration is made with a measurement of ionization yield and scintillation quenching factor for low energy recoiling nuclei (in 0.5 to 100 keV range) originating from elastic scattering of neutrons. To provide wide range of recoiling nuclei energies two systems of neutron scattering are proposed. The first one is based on small-sized DD generator of fast (2.45 MeV) monoenergetic neutrons operating on sealed neutron tube. The second one is based on tandem proton accelerator and lithium target and capable of generation of monoenergetic epithermal neutrons with energy up to 100 keV

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43

Saez, Maria Manuela. "Exploring Neutrino Mass Orderings through Supernova Neutrino Detection." Universe 9, no. 11 (October 28, 2023): 464. http://dx.doi.org/10.3390/universe9110464.

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Core-collapse supernovae (SNs) are one of the most powerful cosmic sources of neutrinos, with energies of several MeV. The emission of neutrinos and antineutrinos of all flavors carries away the gravitational binding energy of the compact remnant and drives its evolution from the hot initial to the cold final states. Detecting these neutrinos from Earth and analyzing the emitted signals present a unique opportunity to explore the neutrino mass ordering problem. This research outlines the detection of neutrinos from SNs and their relevance in understanding the neutrino mass ordering. The focus is on developing a model-independent analysis strategy, achieved by comparing distinct detection channels in large underground detectors. The objective is to identify potential indicators of mass ordering within the neutrino sector. Additionally, a thorough statistical analysis is performed on the anticipated neutrino signals for both mass orderings. Despite uncertainties in supernova explosion parameters, an exploration of the parameter space reveals an extensive array of models with significant sensitivity to differentiate between mass orderings. The assessment of various observables and their combinations underscores the potential of forthcoming supernova observations in addressing the neutrino mass ordering problem.

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Warren, Mackenzie L., Grant J. Mathews, Matthew Meixner, Jun Hidaka, and Toshitaka Kajino. "Impact of sterile neutrino dark matter on core-collapse supernovae." International Journal of Modern Physics A 31, no. 25 (September 8, 2016): 1650137. http://dx.doi.org/10.1142/s0217751x16501372.

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We summarize the impact of sterile neutrino dark matter on core-collapse supernova explosions. We explore various oscillations between electron neutrinos or mixed [Formula: see text] neutrinos and right-handed sterile neutrinos that may occur within a core-collapse supernova. In particular, we consider sterile neutrino masses and mixing angles that are consistent with sterile neutrino dark matter candidates as indicated by recent X-ray flux measurements. We find that the interpretation of the observed 3.5 keV X-ray excess as due to a decaying 7 keV sterile neutrino that comprises 100% of the dark matter would have almost no observable effect on supernova explosions. However, in the more realistic case in which the decaying sterile neutrino comprises only a small fraction of the total dark matter density due to the presence of other sterile neutrino flavors, WIMPs, etc. a larger mixing angle is allowed. In this case a 7 keV sterile neutrino could have a significant impact on core-collapse supernovae. We also consider mixing between [Formula: see text] neutrinos and sterile neutrinos. We find, however, that this mixing does not significantly alter the explosion and has no observable effect on the neutrino luminosities at early times.

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45

Petcov, S. T. "The Nature of Massive Neutrinos." Advances in High Energy Physics 2013 (2013): 1–20. http://dx.doi.org/10.1155/2013/852987.

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The compelling experimental evidences for oscillations of solar, reactor, atmospheric, and accelerator neutrinos imply the existence of 3-neutrino mixing in the weak charged lepton current. The current data on the 3-neutrino mixing parameters are summarised and the phenomenology of 3-νmixing is reviewed. The properties of massive Majorana neutrinos and of their various possible couplings are discussed in detail. Two models of neutrino mass generation with massive Majorana neutrinos—the type I see-saw and the Higgs triplet model—are briefly reviewed. The problem of determining the nature, Dirac or Majorana, of massive neutrinos is considered. The predictions for the effective Majorana mass|〈m〉|in neutrinoless double-beta-((ββ)0ν-) decay in the case of 3-neutrino mixing and massive Majorana neutrinos are summarised. The physics potential of the experiments, searching for(ββ)0ν-decay for providing information on the type of the neutrino mass spectrum, on the absolute scale of neutrino masses, and on the Majorana CP-violation phases in the PMNS neutrino mixing matrix, is also briefly discussed. The opened questions and the main goals of future research in the field of neutrino physics are outlined.

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Consolati, Giovanni, D. Franco, and D. Trezzi. "Positronium Formation and Decay in Organic Scintillators for Neutrino Detection." Materials Science Forum 733 (November 2012): 306–9. http://dx.doi.org/10.4028/www.scientific.net/msf.733.306.

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The detection of electron anti-neutrinos is generally carried out by searching for the coincidence of the reaction products, neutron and positron, in liquid scintillators. However, in these last a positron may form positronium (Ps) with an electron of the medium; efficiency of the process may be high. Furthermore, the triplet ground state sublevel (o-Ps) has lifetimes of a few ns. These features introduce distortions in the time distribution of the emitted photons, which is essential for position reconstruction and pulse shape discrimination algorithms in anti-neutrino experiments. This drawback can be favorably exploited by using o-Ps as a probe to detect anti-neutrinos in the scintillator. We report results of positron annihilation lifetime measurements in some organic liquid scintillators used for neutrino experiments. The o-Ps induced distortion of the scintillation photon emission time distribution may enhance the anti-neutrino detection.

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An, Rui, Vera Gluscevic, Ethan O. Nadler, and Yue Zhang. "Can Neutrino Self-interactions Save Sterile Neutrino Dark Matter?" Astrophysical Journal Letters 954, no. 1 (August 31, 2023): L18. http://dx.doi.org/10.3847/2041-8213/acf049.

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Abstract Sterile neutrinos only interact with the standard model through the neutrino sector, and thus represent a simple dark matter (DM) candidate with many potential astrophysical and cosmological signatures. Recently, sterile neutrinos produced through self-interactions of active neutrinos have received attention as a particle candidate that can yield the entire observed DM relic abundance without violating the most stringent constraints from X-ray observations. We examine consistency of this production mechanism with the abundance of small-scale structure in the universe, as captured by the population of ultrafaint dwarf galaxies orbiting the Milky Way, and derive a lower bound on the sterile-neutrino particle mass of 37 keV. Combining these results with previous collider and X-ray limits excludes 100% sterile-neutrino DM produced by strong neutrino self-coupling, mediated by a heavy (≳1 GeV) scalar; however, data permits sterile-neutrino DM production via a light mediator.

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JONES, J., I. MOCIOIU, I. SARCEVIC, and M. H. RENO. "TRACING VERY HIGH ENERGY TAU NEUTRINOS FROM COSMOLOGICAL SOURCES IN ICE." International Journal of Modern Physics A 20, no. 06 (March 10, 2005): 1204–11. http://dx.doi.org/10.1142/s0217751x05024092.

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Astrophysical sources of ultrahigh energy neutrinos yield tau neutrino fluxes due to neutrino oscillations. We study in detail the contribution of tau neutrinos with energies above 106 GeV relative to the contribution of the other flavors. We consider several different initial neutrino fluxes and include tau neutrino regeneration in transit through the Earth and energy loss of charged leptons. We discuss signals of tau neutrinos in detectors such as IceCube, RICE and ANITA.

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Khatun, Amina, and Fedor Šimkovic. "Effective Majorana Neutrino Mass for ΔL = 2 Neutrino Oscillations." Symmetry 14, no. 7 (July 5, 2022): 1383. http://dx.doi.org/10.3390/sym14071383.

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It is well known that the observations of neutrinoless double-beta decay prove the Majorana nature of the neutrino. However, with specific values of Majorana phases, the effective Majorana neutrino mass to be estimated from the observation of neutrinoless double-beta decay experiments is strongly suppressed if the neutrino mass pattern adheres to a normal ordering. In this case, double-beta decay might not be observed even though the neutrino is Majorana in nature. We show if neutrinos oscillate to antineutrinos in their propagation; then, the observation of this oscillation proves that neutrinos are Majorana and will provide a measurement of neutrino masses and Majorana phases.

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Lombardo, C. "Supernova’s neutrino detection at the Jiangmen Underground Neutrino Observatory." Journal of Physics: Conference Series 2429, no. 1 (February 1, 2023): 012029. http://dx.doi.org/10.1088/1742-6596/2429/1/012029.

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Abstract The Jiangmen Underground Neutrino Observatory (JUNO) will be the largest ever built liquid scintillator detector for neutrino physics. JUNO is a 20 kton liquid scintillator detector, equipped with 20012 large PMTs and 25600 small PMTs. It will be sensitive to various neutrino sources and will give a unique contribution to the observation of the all-flavor neutrino flux from a Galactic core collapse supernova (CCSN). JUNO can detects neutrinos emitted by the next CCSN neutrinos through several interactions, among which inverse beta decay, elastic scattering on electron and proton can providing information of energy spectra of all flavors. Furthermore, JUNO will be able to provide an alert during the pre-SN phase. In this manuscript, the observatory detectors and its capability to detect CCSN neutrinos will be presented.

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Journal articles on the topic 'Neutrino'

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