Journal articles: 'Electron neutrinos; Solar Neutrino Observatory'

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KLEIN, JOSHUA R. "SOLAR NEUTRINO RESULTS FROM THE SUDBURY NEUTRINO OBSERVATORY." International Journal of Modern Physics A 17, no. 24 (September 30, 2002): 3378–92. http://dx.doi.org/10.1142/s0217751x0201279x.

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We describe here the measurement of the flux of neutrinos created by the decay of solar 8B by the Sudbury Neutrino Observatory (SNO). The neutrinos were detected via the charged current (CC) reaction on deuterium and by the elastic scattering (ES) of electrons. The CC reaction is sensitive exclusively to νe's, while the ES reaction also has a small sensitivity to νμ's and ντ's. The flux of νe's from 8B decay measured by the CC reaction rate is [Formula: see text]. Assuming no flavor transformation, the flux inferred from the ES reaction rate is [Formula: see text]. Comparison of ϕ CC (νe) to the Super-Kamiokande Collaboration's precision value of ϕ ES (νx) yields a 3.3σ difference, assuming the systematic uncertainties are normally distributed, providing evidence that there is non-electron flavor active neutrino component in the solar flux. The total flux of active 8B neutrinos is thus determined to be 5.44 ± 0.99 × 106 cm- 2s- 1, in close agreement with the predictions of solar models.

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Miramonti, Lino. "Neutrino Physics and Astrophysics with the JUNO Detector." Universe 4, no. 11 (November 16, 2018): 126. http://dx.doi.org/10.3390/universe4110126.

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The Jiangmen Underground Neutrino Observatory (JUNO) is a 20 kton liquid scintillator multi-purpose underground detector, under construction near the Chinese city of Jiangmen, with data collection expected to start in 2021. The main goal of the experiment is the neutrino mass hierarchy determination, with more than three sigma significance, and the high-precision neutrino oscillation parameter measurements, detecting electron anti-neutrinos emitted from two nearby (baseline of about 53 km) nuclear power plants. Besides, the unprecedented liquid scintillator-type detector performance in target mass, energy resolution, energy calibration precision, and low-energy threshold features a rich physics program for the detection of low-energy astrophysical neutrinos, such as galactic core-collapse supernova neutrinos, solar neutrinos, and geo-neutrinos.

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MAJUMDAR, DEBASISH, AMITAVA RAYCHAUDHURI, KAMALES KAR, ALAK RAY, and FIROZA K. SUTARIA. "OSCILLATION EFFECTS ON NEUTRINOS FROM THE EARLY PHASE OF A NEARBY SUPERNOVA." International Journal of Modern Physics A 15, no. 14 (June 10, 2000): 2105–20. http://dx.doi.org/10.1142/s0217751x00000872.

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Recent observations of atmospheric and solar neutrinos strongly support the phenomenon of neutrino oscillations — a manifestation of a nonzero and nondegenerate mass spectrum. Neutrinos emitted during stellar core collapse leading to a supernova are of the electron neutrino type at source — as for solar and reactor (anti-)neutrinos — and provide another useful tool in the search for flavor oscillations. Their propagation to an earth-bound detector involves length scales that can uniquely probe very small neutrino mass differences hitherto unobservable. Although the number of neutrinos emitted during the collapse phase is much smaller than that emitted in the post-bounce epoch (in which all flavors of neutrinos are emitted), a nearby supernova event may nevertheless register a substantial number of detections from the collapse phase at SuperKamiokande (SK) and the Sudbury Neutrino Observatory (SNO). The measurement of the fluence of these neutrinos at SNO and the distortion of the spectrum detected at SK can yield valuable information about neutrino mass difference and mixing which are illustrated here in terms of two- and three-flavor oscillation models. In particular, we find that R SNO , the ratio of the calorimetric detection of the neutrino fluence via the neutral current channel to the total energy integrated fluence observed via the charged current channel at SNO, is a sensitive probe for oscillations. We also find that αn, the ratio of the nth central moments of the distributions seen at SK and SNO (charged current), can be a useful tool (especially for n=3) to look for neutrino oscillations.

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DUNCAN, F. A. "RESULTS FROM THE PURE D2O PHASE OF THE SUDBURY NEUTRINO OBSERVATORY." International Journal of Modern Physics A 18, no. 22 (September 10, 2003): 3789–807. http://dx.doi.org/10.1142/s0217751x0301718x.

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The Sudbury Neutrino Observatory is a 1000 T D2O Cerenkov detector that is sensitive to 8 B and hep solar neutrinos. Both Charged Current and Neutral Current interaction rates on deuterons as well as the Elastic Scattering interaction rate on electrons can be measured simultaneously. Assuming an undistorted 8 B neutrino spectrum, the total flux measured with the NC reaction is [Formula: see text], which is consistent with solar models. The νe component of the 8 B solar flux is [Formula: see text] for a kinetic energy threshold of 5 MeV. The non-νe component is [Formula: see text], which is 5.3σ greater than zero, giving strong evidence for solar νe flavor transformation. The Day-Night Asymmetry for the Charged Current interaction is [Formula: see text]. If the total flux of active neutrinos is additionally constrained to have no asymmetry, the νe asymmetry is found to be [Formula: see text]. Combined with other solar neutrino data, a global MSW oscillation analysis strongly favors the Large Mixing Angle (LMA) solution.

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Vescovi, D., L. Piersanti, S. Cristallo, M. Busso, F. Vissani, S. Palmerini, S. Simonucci, and S. Taioli. "Effects of a revised 7Be e−-capture rate on solar neutrino fluxes." Astronomy & Astrophysics 623 (March 2019): A126. http://dx.doi.org/10.1051/0004-6361/201834993.

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Context. Electron-capture on 7Be is the main production channel for 7Li in several astrophysical environments. Theoretical evaluations have to account for not only the nuclear interaction, but also the processes in the plasma in which 7Be ions and electrons interact. In recent decades several estimates were presented, pointing out that the theoretical uncertainty in the rate is in general of a few percent. Aims. In the framework of fundamental solar physics, we consider a recent evaluation for the 7Be+e− rate, which has not been used up to now, in the estimate of neutrino fluxes. Methods. We analyzed the effects of the new assumptions on standard solar models (SSMs) and compared the results obtained by adopting the revised 7Be+e− rate to those obtained by that reported in a widely used compilation of reaction rates (ADE11). Results. We found that new SSMs yield a maximum difference in the efficiency of the 7Be channel of about −4% with respect to what is obtained with the previously adopted rate. This fact affects the production of neutrinos from 8B, increasing the relative flux up to a maximum of 2.7%. Negligible variations are found for the physical and chemical properties of the computed solar models. Conclusions. The agreement with the Sudbury Neutrino Observatory measurements of the neutral current component of the 8B neutrino flux is improved.

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Fargion, Daniele, Pietro Oliva, Pier Giorgio de Sanctis Lucentini, and Maxim Yu Khlopov. "Signals of HE atmospheric μ decay in flight around the Sun’s albedo versus astrophysical νμ and ντ traces in the Moon shadow." International Journal of Modern Physics D 27, no. 06 (April 2018): 1841002. http://dx.doi.org/10.1142/s021827181841002x.

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The Sun albedo of Cosmic Rays (CRs) at GeVs energy has been discovered recently by the FERMI satellite. They are traces of atmospheric CRs hitting solar atmosphere and reflecting skimming gamma photons. Even if relevant for astrophysics, as being a trace of atmospheric solar CR noises they cannot offer any signal of neutrino astronomy. On the contrary, the Moon with no atmosphere, may become soon a novel filtering calorimeter and an amplifier of energetic muon astronomical neutrinos (at TeV up to hundred TeVs energy); these lepton tracks leave an imprint in their beta decay while in flight to Earth. Their TeV electron air-shower are among the main signals. Also, a more energetic, but more rare, PeV up to EeV tau lunar neutrino events may be escaping as a tau lepton from the Moon: [Formula: see text] PeV secondaries, then, may be shining on Earth’s atmosphere in lunar shadows in a surprising way. One or a few gamma air-shower events inside the Moon shadows may occur each year in near future Cherenkov telescope array (CTA) or large high altitude air shower observatory (LHAASO) TeV gamma array detector, assuming a nonnegligible astrophysical TeV up to hundred TeV neutrino component (with respect to our terrestrial ruling atmospheric ones); these signals will open a new wonderful passe-partout keyhole for neutrino, been seen along the Moon. The lunar solid angle is small and the muon or tau expected rate is rare, but with the future largest tau radio array as the giant radio array for neutrino detection (GRAND), one might well discover such neutrino imprint.

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Miramonti, Lino, Matteo Agostini, Konrad Altenmueller, Simon Appel, Victor Atroshchenko, Zara Bagdasarian, Davide Basilico, et al. "Solar Neutrinos Spectroscopy with Borexino Phase-II." Universe 4, no. 11 (November 7, 2018): 118. http://dx.doi.org/10.3390/universe4110118.

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Solar neutrinos have played a central role in the discovery of the neutrino oscillation mechanism. They still are proving to be a unique tool to help investigate the fusion reactions that power stars and further probe basic neutrino properties. The Borexino neutrino observatory has been operationally acquiring data at Laboratori Nazionali del Gran Sasso in Italy since 2007. Its main goal is the real-time study of low energy neutrinos (solar or originated elsewhere, such as geo-neutrinos). The latest analysis of experimental data, taken during the so-called Borexino Phase-II (2011-present), will be showcased in this talk—yielding new high-precision, simultaneous wide band flux measurements of the four main solar neutrino components belonging to the “pp” fusion chain (pp, pep, 7 Be, 8 B), as well as upper limits on the remaining two solar neutrino fluxes (CNO and hep).

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Gavrin, V. N., A. I. Abazov, D. N. Abdurashitov, O. L. Anosov, O. V. Bychuk, S. N. Danshin, L. A. Eroshkina, et al. "The Baksan Gallium Solar Neutrino Experiment." International Astronomical Union Colloquium 121 (1990): 201–12. http://dx.doi.org/10.1017/s0252921100067956.

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AbstractA radiochemical 71Ga−71 Ge experiment to determine the integral flux of neutrinos from the sun has been constructed at the Baksan Neutrino Observatory in the USSR. Measurements have begun with 30 tonnes of gallium. The experiment is being expanded with the addition of another 30 tonnes. The motivation, experimental procedures, and present status of this experiment are presented.

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Miramonti, Lino. "Status and the perspectives of the Jiangmen Underground Neutrino Observatory (JUNO)." Modern Physics Letters A 35, no. 09 (March 13, 2020): 2030004. http://dx.doi.org/10.1142/s0217732320300049.

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One of the remaining undetermined fundamental aspects in neutrino physics is the determination of the neutrino mass hierarchy, i.e. discriminating between the two possible orderings of the mass eigenvalues, known as Normal and Inverted Hierarchies. The Jiangmen Underground Neutrino Observatory (JUNO), a 20 kt Liquid Scintillator Detector currently under construction in the South of China, can determine the neutrino mass hierarchy and improve the precision of three oscillation parameters by one order of magnitude. Moreover, thanks to its large liquid scintillator mass, JUNO will also contribute to study neutrinos from non-reactor sources such as solar neutrinos, atmospheric neutrinos, geoneutrinos, supernova burst and diffuse supernova neutrinos. Furthermore, JUNO will also contribute to nucleon decay studies. In this work, I will describe the status and the perspectives of the JUNO experiment.

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Hossain, K. M., D. N. Ghosh, K. Ghosh, and A. K. Bhattacharya. "Multifractality and singularity of 8B solar neutrino flux signals from Sudbury Neutrino Observatory." IET Signal Processing 5, no. 7 (2011): 690. http://dx.doi.org/10.1049/iet-spr.2010.0168.

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BETHE, H. A. "SOLAR NEUTRINOS." International Journal of Modern Physics D 01, no. 01 (January 1992): 1–12. http://dx.doi.org/10.1142/s0218271892000021.

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Solar neutrinos have been measured by a radioactive scheme involving 37 Cl , and by electron collisions at Kamiokande II. The former experiment gave 1/4, the latter 1/2 of the intensity expected from the standard solar model. Kamiokande showed that the central temperature from the standard model is at least approximately correct. Both experiments can be explained by the Mikheyev-Smirnov-Wolfenstein (MSW) theory, and they show the mass of the μ neutrino to be of order 10−3 eV . Preliminary results from an experiment using 71 Ga confirm the conclusions.

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Schever, M. "Status of the Jiangmen Underground Neutrino Observatory." Ukrainian Journal of Physics 64, no. 7 (September 17, 2019): 635. http://dx.doi.org/10.15407/ujpe64.7.635.

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The Jiangmen Underground Neutrino Observatory (JUNO) is a next generation multipurpose antineutrino detector currently under construction in Jiangmen, China. The central detector, containing 20 kton of a liquid scintillator, will be equipped with ∼18 000 20 inch and 25 600 3 inch photomultiplier tubes. Measuring the reactor antineutrinos of two powerplants at a baseline of 53 km with an unprecedented energy resolution of 3%/√︀E(MeV), the main physics goal is to determine the neutrino mass hierarchy within six years of run time with a significance of 3–4q. Additional physics goals are the measurement of solar neutrinos, geoneutrinos, supernova burst neutrinos, the diffuse supernova neutrino background, and the oscillation parameters sin2 O12, Δm212, and |Δm2ee| with a precision <1%, as well as the search for proton decays. The construction is expected to be completed in 2021.

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Rott, Carsten. "Progress in neutrino astronomy." Journal of the Korean Physical Society 78, no. 10 (March 19, 2021): 864–72. http://dx.doi.org/10.1007/s40042-021-00106-1.

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AbstractThe dream of observing our universe through neutrinos is rapidly becoming a reality. More than three decades after the first observation of neutrinos from beyond our solar system associated with Supernova SN1987A, neutrino astronomy is in the midst of a revolution. Extraterrestrial neutrinos are now routinely detected, following the discovery of a high-energy diffuse astrophysical neutrino flux in 2013. The detection of a high-energy neutrino in coincidence with a flaring blazar in 2017 has brought the field rapidly into the multi-messenger science era. The latest developments in the field of neutrino astronomy are reviewed and prospects with current and future detectors discussed. Particular emphasis is put on domestic programs in neutrino astronomy and the possibility to construct a large neutrino observatory in Korea.

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McDonald, Arthur B. "The Sudbury Neutrino Observatory: Observation of Flavor Change for Solar Neutrinos." International Journal of Modern Physics A 31, no. 27 (September 30, 2016): 1630048. http://dx.doi.org/10.1142/s0217751x16300489.

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McDonald, Arthur B. "The Sudbury Neutrino Observatory: Observation of flavor change for solar neutrinos." Annalen der Physik 528, no. 6 (March 17, 2016): 469–80. http://dx.doi.org/10.1002/andp.201600031.

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Heeger, Karsten M. "Resolving the solar neutrino problem: Evidence for massive neutrinos in the Sudbury Neutrino Observatory." Europhysics News 32, no. 5 (September 2001): 180–83. http://dx.doi.org/10.1051/epn:2001506.

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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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BELLERIVE, A. "REVIEW OF SOLAR NEUTRINO EXPERIMENTS." International Journal of Modern Physics A 19, no. 08 (March 30, 2004): 1167–79. http://dx.doi.org/10.1142/s0217751x04019093.

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This paper reviews the constraints on the solar neutrino mixing parameters with data collected by the Homestake, SAGE, GALLEX, Kamiokande, SuperKamiokande, and SNO experiments. An emphasis will be given to the global solar neutrino analyses in terms of matter-enhanced oscillation of two active flavors. The results to-date, including both solar model dependent and independent measurements, indicate that electron neutrinos are changing to other active types on route to the Earth from the Sun. The total flux of solar neutrinos is found to be in very good agreement with solar model calculations. Future measurements will focus on greater accuracy for mixing parameters and on better sensitivity to low neutrino energies.

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GOLDMAN, T., G. J. STEPHENSON, and B. H. J. McKELLAR. "IMPLICATIONS OF QUARK–LEPTON SYMMETRY FOR NEUTRINO MASSES AND OSCILLATIONS." Modern Physics Letters A 15, no. 06 (February 28, 2000): 439–43. http://dx.doi.org/10.1142/s0217732300000426.

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We identify a plausible scenario based on quark–lepton symmetry which correlates long baseline oscillations with maximal mixing to sterile neutrinos. The implication for the Sudbury Neutrino Observatory (SNO) is that the neutral current signal will be found to suffer the same suppression from the standard solar model prediction as obtains for the charged current signal. Flavor mixing among active neutrinos is expected to occur on shorter baselines with smaller mixing amplitudes.

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Bahcall, John N., Marc Kamionkowski, and Alberto Sirlin. "Solar neutrinos: Radiative corrections in neutrino-electron scattering experiments." Physical Review D 51, no. 11 (June 1, 1995): 6146–58. http://dx.doi.org/10.1103/physrevd.51.6146.

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Boyarkin, O. M., and I. O. Boyarkina. "Solar neutrinos as indicators of the Sun’s activity." International Journal of Modern Physics A 34, no. 33 (November 30, 2019): 1950227. http://dx.doi.org/10.1142/s0217751x19502270.

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Opportunity of the solar flares (SFs) prediction observing the solar neutrino fluxes is investigated. In three neutrino generations, the evolution of the neutrino flux traveling the coupled sunspots (CSs) which are the SF source is considered. It is assumed that the neutrinos possess both the dipole magnetic moment and the anapole moment while the magnetic field above the CSs may reach the values [Formula: see text] Gs, display the twisting nature and posses the nonpotential character. The possible resonance conversions of the solar neutrino flux are examined. Since the [Formula: see text] resonance takes place before the convective zone, its existence can in no way be connected with the SF. However, when the solar neutrino flux moves through the CSs in the preflare period, then it may undergo the additional resonance conversions and, as a result, depleting the electron neutrinos flux may be observed.

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RAJPOOT, SUBHASH. "A MODEL FOR SIMPSON’S 17 keV NEUTRINO." International Journal of Modern Physics A 07, no. 18 (July 20, 1992): 4441–48. http://dx.doi.org/10.1142/s0217751x92001988.

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Recent studies of β-decay spectra seem to confirm Simpson’s earlier findings that the electron neutrinos contain a small (1%) admixture of a 17 keV Dirac neutrino. An unconventional model with SU(2)L×SU(2)R×U(1)B−1 gauge interactions is presented in which all neutrinos are Dirac particles. Electron and muon neutrinos acquire seesaw Dirac masses of order 10−3eV for the MSW solution for the solar neutrino problem. The τ neutrino is identified as Simpson’s 17 keV neutrino. Constraints coming from cosmology and particle physics are shown to be satisfied.

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Minakata, H., and C. Peña-Garay. "Solar Neutrino Observables Sensitive to Matter Effects." Advances in High Energy Physics 2012 (2012): 1–15. http://dx.doi.org/10.1155/2012/349686.

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We discuss constraints on the coefficientAMSWwhich is introduced to simulate the effect of weaker or stronger matter potential for electron neutrinos with the current and future solar neutrino data. The currently available solar neutrino data leads to a boundAMSW=1.47+0.54−0.42(+1.88−0.82)at 1σ(3σ) CL, which is consistent with the Standard Model predictionAMSW=1. For weaker matter potential (AMSW<1), the constraint which comes from the flat8B neutrino spectrum is already very tight, indicating the evidence for matter effects. However for stronger matter potential (AMSW>1), the bound is milder and is dominated by the day-night asymmetry of8B neutrino flux recently observed by Super-Kamiokande. Among the list of observables of ongoing and future solar neutrino experiments, we find that (1) an improved precision of the day-night asymmetry of8B neutrinos, (2) precision measurements of the low-energy quasi-monoenergetic neutrinos, and (3) the detection of the upturn of the8B neutrino spectrum at low energies are the best choices to improve the bound onAMSW.

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Diwan, Milind, Rob Edgecock, Takuya Hasegawa, Thomas Patzak, Masato Shiozawa, and Jim Strait. "Future Long-Baseline Neutrino Facilities and Detectors." Advances in High Energy Physics 2013 (2013): 1–35. http://dx.doi.org/10.1155/2013/460123.

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We review the ongoing effort in the US, Japan, and Europe of the scientific community to study the location and the detector performance of the next-generation long-baseline neutrino facility. For many decades, research on the properties of neutrinos and the use of neutrinos to study the fundamental building blocks of matter has unveiled new, unexpected laws of nature. Results of neutrino experiments have triggered a tremendous amount of development in theory: theories beyond the standard model or at least extensions of it and development of the standard solar model and modeling of supernova explosions as well as the development of theories to explain the matter-antimatter asymmetry in the universe. Neutrino physics is one of the most dynamic and exciting fields of research in fundamental particle physics and astrophysics. The next-generation neutrino detector will address two aspects: fundamental properties of the neutrino like mass hierarchy, mixing angles, and the CP phase, and low-energy neutrino astronomy with solar, atmospheric, and supernova neutrinos. Such a new detector naturally allows for major improvements in the search for nucleon decay. A next-generation neutrino observatory needs a huge, megaton scale detector which in turn has to be installed in a new, international underground laboratory, capable of hosting such a huge detector.

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BOWLES, THOMAS J. "A NATIONAL UNDERGROUND SCIENCE AND ENGINEERING LABORATORY." International Journal of Modern Physics A 18, no. 22 (September 10, 2003): 4129–33. http://dx.doi.org/10.1142/s0217751x03017415.

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Dramatic progress has been made in the last several years in our understanding of the properties of neutrinos with evidence for neutrino flavor transformation coming from measurements of atmospheric neutrinos by SuperKamiokande, of solar neutrinos by the Sudbury Neutrino Observatory (SNO), and of reactor neutrinos by KamLAND. These results are a step in the ongoing program of science that is carried out in underground laboratories. The potential for additional significant discoveries with new capabilities in underground laboratories exists and should be exploited. Discoveries are likely to be made not only in nuclear and particle physics, but also in astrophysics, geophysics, and geobiology. A concerted effort is now underway in the United States to create a National Underground Science and Engineering Laboratory (NUSEL) that would provide the facilities and infrastructure necessary to capitalize on the opportunities presented by underground science.

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Bettini, A. "Experimental Highlights from Gran Sasso Laboratory." International Journal of Modern Physics A 18, supp01 (February 2003): 178–214. http://dx.doi.org/10.1142/s0217751x03016653.

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The Gran Sasso National Laboratory of the INFN has given important contributions to the discovery of the phenomenon of neutrino oscillations with experiments both on electron neutrinos from the Sun and muon neutrinos indirectly produced by cosmic rays interactions in the atmosphere. Other experiments in the laboratory give the best limits on electron neutrino effective Majorana mass with two different isotopes. We appear to have entered a new physics domain in which the study of neutrinos may lead us to discover new phenomena, corresponding to energy scales by much higher than those of the present accelerators. Underground laboratories are showing their relevance complementary to the colliders for the advance of basic physics. The physics program at the Gran Sasso Laboratory that we are defining will be focussed on neutrino physics with a complementary set of experiments on the muon neutrino beam from CERN (CNGS project), on solar neutrinos, on atmospheric neutrinos and on neutrinos from Supernova explosion. The relevant thermonuclear cross-sections will be measured. The Majorana vs. Dirac nature of electron neutrinos will be explored with the search for neutrino-less double beta decays in different isotopes.

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Yilmaz, Deniz. "Combined Effect of NSI and SFP on Solar Electron Neutrino Oscillation." Advances in High Energy Physics 2016 (2016): 1–6. http://dx.doi.org/10.1155/2016/1435191.

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The combined effect of spin-flavor precession (SFP) and the nonstandard neutrino interaction (NSI) on the survival probability of solar electron neutrinos (assumed to be Dirac particles) is examined for various values ofϵ11,ϵ12, andμB. It is found that the neutrino survival probability curves affected by SFP and NSI effects individually for some values of the parameters (ϵ11,ϵ12, andμB) get close to the standard MSW curve when both effects are combined. Therefore, the combined effect of SFP and NSI needs to be taken into account when the solar electron neutrino data obtained by low energy solar neutrino experiments is investigated.

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EJIRI, HIROYASU. "MAJORANA NEUTRINO MASSES BY SPECTROSCOPIC STUDIES OF DOUBLE BETA DECAYS AND MOON." Modern Physics Letters A 22, no. 18 (June 14, 2007): 1277–91. http://dx.doi.org/10.1142/s0217732307023778.

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This is a brief review of spectroscopic studies of neutrino-less double beta decays (0νββ) and the MOON (Mo Observatory Of Neutrinos) project. It aims at studying the Majorana nature of neutrinos and the mass spectrum by spectroscopic studies of 0νββ with ν-mass sensitivity of 〈mν〉 ≈ 30 meV . The solid scintillator option of the MOON detector is a super ensemble of multi-layer modules, each being composed by a scintillator plate and two tracking detector planes. Thin ββ source films are interleaved between the detector planes. High localization of the two β tracks enables one to select true signals and reject BG ones by spatial and time correlation analyses. MOON with detector ≠ ββ source is used for studying 0νββ decays from 100 Mo , 82 Se and other ββ isotopes with large nuclear sensitivity (large Qββ). Real-time exclusive measurements of low energy solar neutrinos can also be made by observing inverse β rays from solar-ν captures of 100 Mo in delayed coincidence with the subsequent β decay of 100 Tc .

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MA, ERNEST. "PATTERN OF THE APPROXIMATE MASS DEGENERACY OF MAJORANA NEUTRINOS." Modern Physics Letters A 17, no. 05 (February 20, 2002): 289–94. http://dx.doi.org/10.1142/s0217732302006412.

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In view of the recently reported evidence for a nonzero Majorana mass of the electron neutrino, together with the established phenomena of atmospheric and solar neutrino oscillations, the case of three nearly mass-degenerate Majorana neutrinos is now an interesting possibility. We show in this paper how a natural pattern of symmetry breaking in the recently proposed A4 model of Majorana neutrino masses can accommodate the data on neutrino oscillations, resulting in the predictions sin 2 2θ atm = 1 and sin 2 2θ sol = 2/3.

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Abe, K., Y. Chen, K. Hiraide, K. Ichimura, S. Imaizumi, N. Kato, K. Kobayashi, et al. "Search for exotic neutrino-electron interactions using solar neutrinos in XMASS-I." Physics Letters B 809 (October 2020): 135741. http://dx.doi.org/10.1016/j.physletb.2020.135741.

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ANEZIRIS, C., and J. SCHECHTER. "NEUTRINO “SPIN ROTATION” IN A TWISTING MAGNETIC FIELD." International Journal of Modern Physics A 06, no. 13 (May 30, 1991): 2375–86. http://dx.doi.org/10.1142/s0217751x91001179.

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We calculate in a simple model the reduction in probability for (say) an electron neutrino to rotate to another state in a transverse magnetic field when that field twists in the transverse plane. This may be of relevance to a “second generation” analysis of solar neutrinos. Connection with the Berry phase for this problem is also discussed.

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MINAKATA, HISAKAZU, HIROSHI NUNOKAWA, KIYOSHI SHIRAISHI, and HIROSHI SUZUKI. "NEUTRINOS FROM SUPERNOVA EXPLOSION AND THE MIKHEYEV-SMIRNOV-WOLFENSTEIN EFFECT." Modern Physics Letters A 02, no. 11 (November 1987): 827–34. http://dx.doi.org/10.1142/s0217732387001051.

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It is shown that by taking the effect of the Earth into account the possible observation of electron neutrinos from the supernova SN1987A at the Kamiokande II is compatible with the solution of the solar neutrino puzzle by the Mikheyev-Smirnov-Wolfenstein mechanism. Our scenario requires relatively large mixing angles sin 2 2θ ≳ 0.3 and, most probably, ∆m2 of the order of 10−6 ~ 10−5 (eV) 2. The implications of possible observation in other neutrino detectors are briefly discussed.

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Wang, Ling, and Mu-ming Poo. "Yifang Wang: high energy physics in China." National Science Review 3, no. 2 (June 1, 2016): 252–56. http://dx.doi.org/10.1093/nsr/nww033.

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Abstract On 8 March 2012, Yifang Wang, co-spokesperson of the Daya Bay Experiment and Director of Institute of High Energy Physics, Chinese Academy of Sciences, announced the discovery of a new type of neutrino oscillation with a surprisingly large mixing angle (θ13), signifying ‘a milestone in neutrino research’. Now his team is heading for a new goal—to determine the neutrino mass hierarchy and to precisely measure oscillation parameters using the Jiangmen Underground Neutrino Observatory, which is due for completion in 2020. Neutrinos are fundamental particles that play important roles in both microscopic particle physics and macroscopic universe evolution. The studies on neutrinos, for example, may answer the question why our universe consists of much more matter than antimatter. But this is not an easy task. Though they are one of the most numerous particles in the universe and zip through our planet and bodies all the time, these tiny particles are like ‘ghost’, difficult to be captured. There are three flavors of neutrinos, known as electron neutrino (νe), muon neutrino (νμ), and tau neutrino (ντ), and their flavors could change as they travel through space via quantum interference. This phenomenon is known as neutrino oscillation or neutrino mixing. To determine the absolute mass of each type of neutrino and find out how they mix is very challenging. In a recent interview with NSR in Beijing, Yifang Wang explained how the Daya Bay Experiment on neutrino oscillation not only addressed the frontier problem in particle physics, but also harnessed the talents and existing technology in Chinese physics community. This achievement, Wang reckons, will not be an exception in Chinese high energy physics, when appropriate funding and organization for big science projects could be efficiently realized in the future.

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Kharlanov, Oleg. "Reception of Modulated Neutrino Day-Night Effect Signal by Neutrino Detectors." EPJ Web of Conferences 201 (2019): 09005. http://dx.doi.org/10.1051/epjconf/201920109005.

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The regeneration effect of solar neutrinos in the Earth leading to the so-called day-night effect strongly depends on the neutrino energy, the time of day, and the season. Classical neutrino experiments, such as Super-Kamiokande, typically observe this effect cumulatively, i.e., virtually integrate it over the year. We discuss various day-night effects that could become potentially observable if time-weighted data processing is applied to neutrino events. The procedure is similar to reception of radio-frequency modulated signals and ‘demodulation’ of the neutrino signal, for example, is able to reveal interesting signatures in the high-energy tail of the electron recoil energy spectrum

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Andringa, S., E. Arushanova, S. Asahi, M. Askins, D. J. Auty, A. R. Back, Z. Barnard, et al. "Current Status and Future Prospects of the SNO+ Experiment." Advances in High Energy Physics 2016 (2016): 1–21. http://dx.doi.org/10.1155/2016/6194250.

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SNO+ is a large liquid scintillator-based experiment located 2 km underground at SNOLAB, Sudbury, Canada. It reuses the Sudbury Neutrino Observatory detector, consisting of a 12 m diameter acrylic vessel which will be filled with about 780 tonnes of ultra-pure liquid scintillator. Designed as a multipurpose neutrino experiment, the primary goal of SNO+ is a search for the neutrinoless double-beta decay (0νββ) of130Te. In Phase I, the detector will be loaded with 0.3% natural tellurium, corresponding to nearly 800 kg of130Te, with an expected effective Majorana neutrino mass sensitivity in the region of 55–133 meV, just above the inverted mass hierarchy. Recently, the possibility of deploying up to ten times more natural tellurium has been investigated, which would enable SNO+ to achieve sensitivity deep into the parameter space for the inverted neutrino mass hierarchy in the future. Additionally, SNO+ aims to measure reactor antineutrino oscillations, low energy solar neutrinos, and geoneutrinos, to be sensitive to supernova neutrinos, and to search for exotic physics. A first phase with the detector filled with water will begin soon, with the scintillator phase expected to start after a few months of water data taking. The0νββPhase I is foreseen for 2017.

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Smith, Peter F. "Further studies of the OMNIS supernova neutrino observatory: optimisation of detector configuration and possible extension to solar neutrinos." Astroparticle Physics 16, no. 1 (October 2001): 75–96. http://dx.doi.org/10.1016/s0927-6505(01)00104-9.

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Cox, Arthur N. "Solar Opacities Constrained by Solar Neutrinos and Solar Oscillations." International Astronomical Union Colloquium 121 (1990): 61–80. http://dx.doi.org/10.1017/s0252921100067828.

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AbstractThis review discusses the current situation for opacities at the solar center, the solar surface, and for the few million kelvin temperatures that occur below the convection zone. The solar center conditions are important because they are crucial for the neutrino production, which continues to be predicted about 4 times that observed. The main extinction effects there are free-free photon absorption in the electric fields of the hydrogen, helium and the CNO atoms, free electron scattering of photons, and the bound-free and bound-bound absorption of photons by iron atoms with two electrons in the 1s bound level. An assumption that the iron is condensed-out below the convection zone, and the opacity in the central regions is thereby reduced, results in about a 25 percent reduction in the central opacity but only a 5 percent reduction at the base of the convection zone. Furthermore, the p-mode solar oscillations are changed with this assumption, and do not fit the observed ones as well as for standard models. A discussion of the large effective opacity reduction by weakly interacting massive particles (WIMPs or Cosmions) also results in poor agreement with observed p-mode oscillation frequencies. The much larger opacities for the solar surface layers from the Los Alamos Astrophysical Opacity Library instead of the widely used Cox and Tabor values show small improvements in oscillation frequency predictions, but the largest effect is in the discussion of p-mode stability. Solar oscillation frequencies can serve as an opacity experiment for the temperatures and densities, respectively, of a few million kelvin and between 0.1 and 10 g/cm3. Current oscillation frequency calculations indicate that possibly the Opacity Library values need an increase of typically 15 percent just at the bottom of the convection zone at 3×106K. Opacities have uncertainties at the photosphere and deeper than the convection zone ranging from 10 to 25 percent. The equation of state that supplies data for the opacity calculations fortunately has pressure uncertainties of only about 1 percent, but opacity uncertainties will always be much larger. A discussion is given about opacity experiments that the stars provide. Opacities in the envelopes of the Hyades G stars, the Cepheids, δ Scuti variables, and the β Cephei variables indicate that significantly larger opacities, possibly caused by iron lines, seem to be required.

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Bednarek, Włodek. "Gamma-rays and neutrinos from accreating neutron stars." Proceedings of the International Astronomical Union 6, S275 (September 2010): 305–6. http://dx.doi.org/10.1017/s1743921310016224.

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AbstractDense wind of a massive star can be partially captured by a companion neutron star (NS) creating a very turbulent and magnetized transition region at some distance from the NS surface. We consider the consequences of electron and hadron acceleration at such a transition region. Electrons lose energy on the synchrotron process and the inverse Compton (IC) scattering of thermal radiation from the NS surface and/or the massive star. We calculate the synchrotron spectra (from X-rays to soft γ-rays) and IC spectra in the case of sources accreting the matter under the accretor and propeller scenarios. It is argued that a population of accreting massive binaries, recently discovered by the INTEGRAL observatory, can be detectable by the Fermi LAT telescope. On the other hand, TeV γ-ray emission from other class of massive binaries can be interpreted in terms of a magnetar accreting matter in the propeller scenario. We also calculate the expected neutrino event rates in a km2 detector produced by relativistic hadrons accelerated in such scenario.

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Porcelli, A., M. Agostini, K. Altenmüller, S. Appel, V. Atroshchenko, Z. Bagdasarian, D. Basilico, et al. "Recent Borexino results and perspectives of the SOX measurement." EPJ Web of Conferences 182 (2018): 02099. http://dx.doi.org/10.1051/epjconf/201818202099.

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Borexino is a liquid scintillator detector sited underground in the Laboratori Nazionali del Gran Sasso (Italy). Its physics program, until the end of this year, is focussed on the study of solar neutrinos, in particular from the Beryllium, pp, pep and CNO fusion reactions. Knowing the reaction chains in the sun provides insights towards physics disciplines such as astrophysics (star physics, star formation, etc.), astroparticle and particle physics. Phase II started in 2011 and its aim is to improve the phase I results, in particular the measurements of the neutrino fluxes from the pep and CNO processes. By the end of this year, data taking from the sun will be over and a new project is scheduled to launch: Short distance Oscillation with boreXino (SOX), which uses a Cerium source for neutrinos (100÷150 kCi of activity) and aims to confirm or rule out the presence of sterile neutrinos. This particle is hypothesised to justify the reactor, Gallium and LSND anomalies found and can reject extensions to the standard model. The work presented is a summary of the solar neutrino results achieved so far, which lead not only to a precise study of the processes in the sun, but also to more Standard Model oriented measurements (such as the stability of the charge, i.e. the life time of the electron). Furthermore, the perspectives of the SOX program are discussed showing the experiment sensitivity to a fourth neutrino state covering almost entirely 3σ of the preferred region of the anomalous neutrino experiments, and additional applications of the detector such as the study of geo-neutrinos.

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CLINE, DAVID B., and WOOPYO HONG. "A LIQUID ARGON OR XENON DETECTOR TO OBSERVE A NEUTRINO MAGNETIC MOMENT OF μν~10−11μB." International Journal of Modern Physics A 07, no. 17 (July 10, 1992): 4167–73. http://dx.doi.org/10.1142/s0217751x92001861.

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We describe the current situation in the search for a finite magnetic moment. Solar neutrino experiments can be interpreted in terms of a neutrino magnetic moment of ~10−10−10−11μB. Other astrophysical constraints are very model-dependent. We then describe a technique to detect a magnetic moment using neutrinos from a reactor or low energy neutrino facility and a cryogenic electron drift detector with a mass in the range of 1–5 tons. Background estimates are also given for an experimental search. We estimate that a neutrino magnetic moment down to 4×10−11μB can be searched for with this technique. We consider both argon and xeuon to be suitable detector components.

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Grimus, W., and T. Schwetz. "Elastic neutrino–electron scattering of solar neutrinos and potential effects of magnetic and electric dipole moments." Nuclear Physics B 587, no. 1-3 (October 2000): 45–66. http://dx.doi.org/10.1016/s0550-3213(00)00451-x.

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HOROWITZ, C. J. "MULTI-MESSENGER OBSERVATIONS OF NEUTRON-RICH MATTER." International Journal of Modern Physics E 20, no. 10 (October 2011): 2077–100. http://dx.doi.org/10.1142/s0218301311020332.

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At very high densities, electrons react with protons to form neutron-rich matter. This material is central to many fundamental questions in nuclear physics and astrophysics. Moreover, neutron-rich matter is being studied with an extraordinary variety of new tools such as Facility for Rare Isotope Beams (FRIB) and the Laser Interferometer Gravitational Wave Observatory (LIGO). We describe the Lead Radius Experiment (PREX) that uses parity violating electron scattering to measure the neutron radius in 208Pb. This has important implications for neutron stars and their crusts. We discuss X-ray observations of neutron star radii. These also have important implications for neutron-rich matter. Gravitational waves (GW) open a new window on neutron-rich matter. They come from sources such as neutron star mergers, rotating neutron star mountains, and collective r-mode oscillations. Using large scale molecular dynamics simulations, we find neutron star crust to be very strong. It can support mountains on rotating neutron stars large enough to generate detectable gravitational waves. Finally, neutrinos from core collapse supernovae (SN) provide another, qualitatively different probe of neutron-rich matter. Neutrinos escape from the surface of last scattering known as the neutrino-sphere. This is a low density warm gas of neutron-rich matter. Neutrino-sphere conditions can be simulated in the laboratory with heavy ion collisions. Observations of neutrinos can probe nucleosyntheses in SN. Simulations of SN depend on the equation of state (EOS) of neutron-rich matter. We discuss a new EOS based on virial and relativistic mean field calculations. We believe that combing astronomical observations using photons, GW, and neutrinos, with laboratory experiments on nuclei, heavy ion collisions, and radioactive beams will fundamentally advance our knowledge of compact objects in the heavens, the dense phases of QCD, the origin of the elements, and of neutron-rich matter.

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Farine, J. "Measurement of the rate of ν e+d → p+p+e − interactions produced by 8B solar neutrinos at the Sudbury Neutrino Observatory." Physics of Atomic Nuclei 65, no. 12 (December 2002): 2147–55. http://dx.doi.org/10.1134/1.1530292.

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44

Slad, L. M. "Existing and expected manifestations of a new fundamental interaction." International Journal of Modern Physics E 30, no. 06 (June 2021): 2150052. http://dx.doi.org/10.1142/s021830132150052x.

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In this paper, a number of characteristics of the new fundamental interaction are described. The interaction is carried by a massless pseudoscalar boson and extends to at least the electron neutrino, proton and neutron. A substantiation of the existence of such an interaction is supported by an good agreement between the theoretical and experimental rates of all the five observed processes with solar neutrinos. A bright manifestation of the new interaction is expected in the observation that its contribution to the rate of splitting of a number of light stable nuclei by reactor antineutrinos is approximately six orders of magnitude greater than the contribution of electroweak interaction.

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Saruwatari, Motoaki, Masa-aki Hashimoto, Ryohei Fukuda, and Shin-ichiro Fujimoto. "R-Process Nucleosynthesis in MHD Jet Explosions of Core-Collapse Supernovae." Journal of Astrophysics 2013 (October 22, 2013): 1–13. http://dx.doi.org/10.1155/2013/506146.

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We investigate the r-process nucleosynthesis during the magnetohydrodynamical (MHD) explosion of a supernova in a helium star of 3.3 M⊙, where effects of neutrinos are taken into account using the leakage scheme in the two-dimensional (2D) hydrodynamic code. Jet-like explosion due to the combined effects of differential rotation and magnetic field is able to erode the lower electron fraction matter from the inner layers. We find that the ejected material of low electron fraction responsible for the r-process comes out from just outside the neutrino sphere deep inside the Fe-core. It is found that heavy element nucleosynthesis depends on the initial conditions of rotational and magnetic fields. In particular, the third peak of the distribution is significantly overproduced relative to the solar system abundances, which would indicate a possible r-process site owing to MHD jets in supernovae.

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46

Klapdor-Kleingrothaus, H. V. "Perspectives of double beta and dark matter search as windows to new physics." HNPS Proceedings 9 (February 11, 2020): 130. http://dx.doi.org/10.12681/hnps.2779.

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Nuclear double beta decay provides an extraordinarily broad potential to search for beyond Standard Model physics, probing already now the TeV scale, on which new physics should manifest itself. These possibilities are reviewed here. First, the results of present generation experiments are presented. The most sensitive one of them - the Heidelberg-Moscow experiment in the Gran Sasso - probes the electron mass now in the sub eV region and has reached recently a limit of ~ 0.1 eV. This limit has striking influence on presently discussed neutrino mass scenarios. Basing to a large extent on the theoretical work of the Heidelberg Double Beta Group in the last two years, results are obtained also for SUSY models (R-parity breaking, sneutrino mass), leptoquarks (leptoquark-Higgs coupling), compositeness, right-handed W boson mass, test of special relativity and equivalence principle in the neutrino sector and others. These results are comfortably competitive to corresponding results from high-energy accelerators like TEVATRON, HERA, etc. One of the enriched 7Ge detectors also yields the most stringent limits for cold dark matter (WIMPs) to date by using raw data. Second, future perspectives of ßß research are discussed. A new Heidelberg experimental proposal (GENIUS) will allow to increase the sensitivity for Majorana neutrino masses from the present level of at best 0.1 eV down to 0.01 or even 0.001 eV. Its physical potential would be a breakthrough into the multi-TeV range for many beyond standard models. Its sensitivity for neutrino oscillation parameters would be larger than of all present terrestrial neutrino oscillation experiments and of those planned for the future. It could probe directly the large angle, and for almost degenerate neutrino mass scenarios even the small angle solution of the solar neutrino problem. It would further, already in a first step using only 100 kg of natural Ge detectors, cover almost the full MSSM parameter space for prediction of neutralinos as cold dark matter, making the experiment competitive to LHC in the search for supersymmetry. Finally GENIUS could be used as the first real time detector of solar pp neutrinos.

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Dai, Yang, Alex B. Borisov, James W. Longworth, Keith Boyer, and Charles K. Rhodes. "Cryptographic Unification of Mass and Space Links Neutrino Flavor (νe/νμ) Transformations with the Cosmological Constant Λ." International Journal of Modern Physics A 18, no. 23 (September 20, 2003): 4257–83. http://dx.doi.org/10.1142/s0217751x03016392.

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The universe exhibits two striking manifestations, (a) immense complexity and (b) an astonishingly high scale-free precision. Since a cryptographic system based on the modular arithmetic of a finite field can provide a mathematical structure matching these two cardinal characteristics, it is natural to evaluate the theoretical possibilities of a cryptographic analysis of physical phenomena. The organization of the particle mass scale provides a particularly suitable test of this idea, since the cryptographic approach also has the inherent feature that divergences are fully barred, thereby eliminating the need for ad hoc procedures of renormalization. This article (1) shows how such a cryptographic concept can be implemented and (2) demonstrates its surprising ability to synthesize the description of a broad range of phenomena through the development of an interlocking set of quantitative findings. It is found that a cryptographic theoretical framework based solely on two physically anchored parameters, a modulus Pα and a corresponding primitive root gα, can simultaneously achieve six goals. Specifically, it (α) unites the concepts of mass and space, (β) organizes the physical mass scale in a group structure, (γ) produces a quantitative concordance of findings linking the cosmic and micro-scales that includes values for the fine structure constant α and the unified strong-electroweak coupling constant α*, (δ) respectively gives prospective magnitudes of 0.808 meV and 27.68 meV for the rest masses mνe and mνμ of the electron (νe) and muon (νμ) neutrinos, (∊) specifies a symmetry condition that yields an exact predicted value for the Higgs particle mass that lies above 1018 GeV, and (ζ) enables the formulation of a direct physical connection between the anomalous flavor (νe/νμ) transforming propagation of solar neutrinos and the existence of a positive cosmological constant Λ. These results are uniformly in agreement with all corresponding observational data.

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Aalbers, J., F. Agostini, S. E. M. Ahmed Maouloud, M. Alfonsi, L. Althueser, F. D. Amaro, J. Angevaare, et al. "Solar neutrino detection sensitivity in DARWIN via electron scattering." European Physical Journal C 80, no. 12 (December 2020). http://dx.doi.org/10.1140/epjc/s10052-020-08602-7.

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AbstractWe detail the sensitivity of the proposed liquid xenon DARWIN observatory to solar neutrinos via elastic electron scattering. We find that DARWIN will have the potential to measure the fluxes of five solar neutrino components: pp, $$^7$$ 7 Be, $$^{13}$$ 13 N, $$^{15}$$ 15 O and pep. The precision of the $$^{13}$$ 13 N, $$^{15}$$ 15 O and pep components is hindered by the double-beta decay of $$^{136}$$ 136 Xe and, thus, would benefit from a depleted target. A high-statistics observation of pp neutrinos would allow us to infer the values of the electroweak mixing angle, $$\sin ^2\theta _w$$ sin 2 θ w , and the electron-type neutrino survival probability, $$P_{ee}$$ P ee , in the electron recoil energy region from a few keV up to 200 keV for the first time, with relative precision of 5% and 4%, respectively, with 10 live years of data and a 30 tonne fiducial volume. An observation of pp and $$^7$$ 7 Be neutrinos would constrain the neutrino-inferred solar luminosity down to 0.2%. A combination of all flux measurements would distinguish between the high- (GS98) and low-metallicity (AGS09) solar models with 2.1–2.5$$\sigma $$ σ significance, independent of external measurements from other experiments or a measurement of $$^8$$ 8 B neutrinos through coherent elastic neutrino-nucleus scattering in DARWIN. Finally, we demonstrate that with a depleted target DARWIN may be sensitive to the neutrino capture process of $$^{131}$$ 131 Xe.

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Aharmim, B., S. N. Ahmed, A. E. Anthony, E. W. Beier, A. Bellerive, M. Bergevin, S. D. Biller, et al. "Electron energy spectra, fluxes, and day-night asymmetries of8B solar neutrinos from measurements with NaCl dissolved in the heavy-water detector at the Sudbury Neutrino Observatory." Physical Review C 72, no. 5 (November 30, 2005). http://dx.doi.org/10.1103/physrevc.72.055502.

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de Salas, P. F., D. V. Forero, S. Gariazzo, P. Martínez-Miravé, O. Mena, C. A. Ternes, M. Tórtola, and J. W. F. Valle. "2020 global reassessment of the neutrino oscillation picture." Journal of High Energy Physics 2021, no. 2 (February 2021). http://dx.doi.org/10.1007/jhep02(2021)071.

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Abstract We present an updated global fit of neutrino oscillation data in the simplest three-neutrino framework. In the present study we include up-to-date analyses from a number of experiments. Concerning the atmospheric and solar sectors, besides the data considered previously, we give updated analyses of IceCube DeepCore and Sudbury Neutrino Observatory data, respectively. We have also included the latest electron antineutrino data collected by the Daya Bay and RENO reactor experiments, and the long-baseline T2K and NOνA measurements, as reported in the Neutrino 2020 conference. All in all, these new analyses result in more accurate measurements of θ13, θ12, $$ \Delta {m}_{21}^2 $$ Δ m 21 2 and $$ \left|\Delta {m}_{31}^2\right| $$ Δ m 31 2 . The best fit value for the atmospheric angle θ23 lies in the second octant, but first octant solutions remain allowed at ∼ 2.4σ. Regarding CP violation measurements, the preferred value of δ we obtain is 1.08π (1.58π) for normal (inverted) neutrino mass ordering. The global analysis still prefers normal neutrino mass ordering with 2.5σ statistical significance. This preference is milder than the one found in previous global analyses. These new results should be regarded as robust due to the agreement found between our Bayesian and frequentist approaches. Taking into account only oscillation data, there is a weak/moderate preference for the normal neutrino mass ordering of 2.00σ. While adding neutrinoless double beta decay from the latest Gerda, CUORE and KamLAND-Zen results barely modifies this picture, cosmological measurements raise the preference to 2.68σ within a conservative approach. A more aggressive data set combination of cosmological observations leads to a similar preference for normal with respect to inverted mass ordering, namely 2.70σ. This very same cosmological data set provides 2σ upper limits on the total neutrino mass corresponding to Σmν< 0.12 (0.15) eV in the normal (inverted) neutrino mass ordering scenario. The bounds on the neutrino mixing parameters and masses presented in this up-to-date global fit analysis include all currently available neutrino physics inputs.

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Journal articles on the topic 'Electron neutrinos; Solar Neutrino Observatory'

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