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Journal articles on the topic 'Solar Neutrino Flux'

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Published: 3 June 2025
Last updated: 31 July 2025

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1

Gutiérrez, Miguel, Manuel Masip, and Sergio Muñoz. "The Solar Disk at High Energies." Astrophysical Journal 941, no. 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-LA
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2

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
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3

KLEIN, JOSHUA R. "SOLAR NEUTRINO RESULTS FROM THE SUDBURY NEUTRINO OBSERVATORY." International Journal of Modern Physics A 17, no. 24 (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 t
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4

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 (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] res
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5

DEV, S., and JYOTI DHAR SHARMA. "RESOLUTION OF THE Be/B SOLAR NEUTRINO FLUX ANOMALY IN THE RESONANT SPIN-FLAVOR PRECESSION SCENARIO WITH TWISTING SOLAR MAGNETIC FIELDS." Modern Physics Letters A 15, no. 05 (2000): 351–60. http://dx.doi.org/10.1142/s0217732300000335.

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The Be/B neutrino flux anomaly has been examined within the framework of the resonant spin-flavor precession scenario with twisting solar magnetic fields. It is found that the twist of the toroidal component of the solar magnetic field, leads naturally to a complete disappearance of 7 Be neutrinos emerging from one of the solar hemispheres. However, the 7 Be neutrino flux emerging from the other solar hemisphere with oppositely twisted magnetic field must survive completely. Thus, this scenario predicts seasonal variations of the 7 Be neutrino flux to be observed in the Borexino experiment.
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6

DEV, S., and SANJEEV KUMAR. "CONSTRAINTS ON WEAKLY MIXED STERILE NEUTRINOS IN THE LIGHT OF SNO SALT PHASE AND 766.3 Ty KamLAND DATA." Modern Physics Letters A 20, no. 38 (2005): 2957–67. http://dx.doi.org/10.1142/s0217732305018189.

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The possibility of flavor transitions into sterile neutrinos (accompanying the dominant LMA transitions) in the solar boron neutrino flux has been examined in a scenario proposed by Hollanda and Smirnov to overcome some generic problems of the pure LMA scenario. It is found that the most recent SNO salt phase solar neutrino data and the KamLAND 766.3 Ty spectral data, allow for a significant sterile presence in the solar boron neutrino flux reaching the earth.
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7

PAL, PALASH B. "PARTICLE PHYSICS CONFRONTS THE SOLAR NEUTRINO PROBLEM." International Journal of Modern Physics A 07, no. 22 (1992): 5387–459. http://dx.doi.org/10.1142/s0217751x92002465.

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This review has four parts. In Part I, we describe the reactions that produce neutrinos in the sun and the expected flux of those neutrinos on the earth. We then discuss the detection of these neutrinos, and how the results obtained differ from the theoretical expectations, leading to what is known as the solar neutrino problem. In Part II, we show how neutrino oscillations can provide a solution to the solar neutrino problem. This includes vacuum oscillations, as well as matter enhanced oscillations. In Part III, we discuss the possibility of time variation of the neutrino flux and how a magn
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8

KWONG, WAIKWOK, and S. P. ROSEN. "THE SOLAR NEUTRINO PROBLEM AND BOUNDS ON SOLAR NEUTRINO FLUXES." Modern Physics Letters A 10, no. 19 (1995): 1331–49. http://dx.doi.org/10.1142/s0217732395001460.

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We review the current status of the solar neutrino problem. A survey of the experiments and their results are given, and solar physics crucial to the understanding of these results are discussed. Semi-empirical methods are used to derive bounds on the fluxes of the three most important components (pp, 7Be and 8B) of the solar neutrino spectrum. The 8B neutrinos are directly measured to be about half of the theoretical prediction. Relative to their theoretical predictions, we find the 7Be neutrinos to be highly suppressed and the pp neutrinos not suppressed. We are also able to derive a lower b
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9

Khavroshkin, O. B., and V. V. Tsyplakov. "HENRI EFFECT: REGISTRATION PARAMETERS." Metafizika, no. 4 (December 15, 2020): 67–71. http://dx.doi.org/10.22363/2224-7580-2020-4-67-71.

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The detected anomalous neutrino radioisotope (ANRI) absorption or effect allows one to study the variety of interactions of neutrino fluxes with radioactive matter and its consequences. Thus, results were obtained on solar neutrinos v , seismicity and heat flow of the Earth. The study of the features of the mechanical manifestation of the neutrino flux as a mechanical effect of the solar flux v in space on the Pioneer-type spacecraft is promising for many reasons.
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10

RAYCHAUDHURI, PROBHAS. "TIME VARIATIONS IN KAMIOKANDE SOLAR NEUTRINO DATA." Modern Physics Letters A 06, no. 22 (1991): 2003–7. http://dx.doi.org/10.1142/s0217732391002165.

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Solar neutrino flux (Eν ≥ 7.5 MeV ) data from 1st January to April 1990 as measured in Kamiokande solar neutrino experiment have been analyzed statistically and have found that the solar neutrino data varies with the solar activity cycle with very high statistical significance (> 98% confidence level). Average solar neutrino flux data in the sunspot minimum range cannot be equal to twice the average solar neutrino flux data in the sunspot maximum range, which suggests that the neutrino flip through the magnetic field of the convection zone of the sun is not responsible for the solar neutrin
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11

Spiro, M., and D. Vignaud. "Solar Neutrino Projects." International Astronomical Union Colloquium 121 (1990): 157–69. http://dx.doi.org/10.1017/s0252921100067919.

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AbstractAn overview of the solar neutrino projects is given, with an emphasis on the complementarity of the different experiments (gallium, indium, heavy water,...) to solve the solar neutrino problem that was raised by the chlorine and the Kamiokande results. The separation of the different sources of neutrinos in the Sun would contribute significantly to the astrophysical understanding of the Sun. Some of the planned experiments could be able to pinpoint neutrino oscillations (within a wide range of parameters) almost independently of solar models. Projects which are particularly sensitive t
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12

RAYCHAUDHURI, PROBHAS. "ANALYSIS OF SOLAR NEUTRINO FLUX FROM THE EXISTING SOLAR NEUTRINO DETECTORS." International Journal of Modern Physics A 14, no. 08 (1999): 1205–23. http://dx.doi.org/10.1142/s0217751x99000622.

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It is suggested that the experimental data on the solar neutrino flux as measured in the existing solar neutrino detectors (e.g. Homestake, Kamiokande II and III, Gallex and Sage) vary with the solar activity cycle to a very high level of statistical significance. We have applied the run test and the change point test to the nine sets of solar neutrino flux that have been generated by the Monte-Carlo simulation with production rate and background parameters that are typical of those in the actual Homestake experiment. Homestake solar neutrino flux data show anticorrelation with sunspot numbers
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13

BELLERIVE, A. "REVIEW OF SOLAR NEUTRINO EXPERIMENTS." International Journal of Modern Physics A 19, no. 08 (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. F
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14

RAYCHAUDHURI, PROBHAS. "SOLAR NEUTRINO FLUX VARIATION IN KAMIOKANDE DETECTOR DURING SOLAR CYCLE 22." Modern Physics Letters A 13, no. 14 (1998): 1109–14. http://dx.doi.org/10.1142/s0217732398001182.

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The 8 B solar neutrino flux observed in Kamiokande detector (KAMIOKANDE II and III) from January 1987 to February 1995 has been analysed statistically and it has been found that solar neutrino flux data in Kamiokande detector varies with the solar activity cycle. It is also shown that solar neutrino flux data in Kamiokande detector also has five phases during the solar cycle 22 as observed in the Homestake solar neutrino flux data during the solar cycles 21 and 22 indicating that the solar activity cycle is due to the pulsating character of the nuclear energy generation inside the core of the
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15

Pavićević, M. K., F. Bosch, G. Amthauer, et al. "Status and New Data of the Geochemical Determination of the pp-Neutrino Flux by LOREX." Advances in High Energy Physics 2012 (2012): 1–15. http://dx.doi.org/10.1155/2012/274614.

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LOREX (LORandite EXperiment) addresses the determination of the solar (pp) neutrino flux during the last four million years by exploiting the reaction 205Tl+νe→ 205Pb+e-with an incomparably low-energy threshold of 50 keV for the capture of solar neutrinos. The ratio of205Pb/205Tl atoms in the Tl-bearing mineral lorandite provides, if corrected for the cosmic-ray induced background, the product of the flux of solar neutrinos and their capture probability by205Tl, averaged over the age of lorandite. To get the mean solar neutrino flux itself, four problems have to be addressed: (1) the geologica
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16

DUNCAN, F. A. "RESULTS FROM THE PURE D2O PHASE OF THE SUDBURY NEUTRINO OBSERVATORY." International Journal of Modern Physics A 18, no. 22 (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 5.3
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17

Miramonti, Lino, Matteo Agostini, Konrad Altenmueller, et al. "Solar Neutrinos Spectroscopy with Borexino Phase-II." Universe 4, no. 11 (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), wil
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18

RAYCHAUDHURI, PROBHAS. "TIME VARIATION OF SOLAR NEUTRINO FLUX." Modern Physics Letters A 08, no. 21 (1993): 1961–68. http://dx.doi.org/10.1142/s0217732393001677.

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Considering the solar neutrino data during the period from June, 1989 to April, 1992 within first sunspot maximum (it coincides with the maximum of the sunspot (Wolf numbers) and second sunspot maximum (usually appears 2–3 years after the first sunspot maximum) from the four solar neutrino experiments (37 Cl radiochemical, SAGE I & II, Gallex, Kamiokande II & III) we see that the average solar neutrino flux is much higher at the second sunspot maximum (May, 1991 to April, 1992) than at the first sunspot maximum (June, 1989 to April, 1991). This type of observation is already observed i
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19

Zhao, Jie, Baobiao Yue, Haoqi Lu, et al. "Model-independent Approach of the JUNO 8B Solar Neutrino Program." Astrophysical Journal 965, no. 2 (2024): 122. http://dx.doi.org/10.3847/1538-4357/ad2bfd.

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Abstract The physics potential of detecting 8B solar neutrinos will be exploited at the Jiangmen Underground Neutrino Observatory (JUNO), in a model-independent manner by using three distinct channels of the charged current (CC), neutral current (NC), and elastic scattering (ES) interactions. Due to the largest-ever mass of 13C nuclei in the liquid scintillator detectors and the expected low background level, 8B solar neutrinos are observable in the CC and NC interactions on 13C for the first time. By virtue of optimized event selections and muon veto strategies, backgrounds from the accidenta
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20

GAVRYUSEV, V., and E. GAVRYUSEVA. "Solar Neutrino Flux Variations." Annals of the New York Academy of Sciences 647, no. 1 Texas/ESO-Cer (1991): 483–94. http://dx.doi.org/10.1111/j.1749-6632.1991.tb32198.x.

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21

IGNATIEV, A. YU, and G. C. JOSHI. "THE CHARGED NEUTRINO: A NEW APPROACH TO THE SOLAR NEUTRINO PROBLEM." Modern Physics Letters A 09, no. 16 (1994): 1479–88. http://dx.doi.org/10.1142/s0217732394001313.

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We have considered the effect of the reduction of the solar neutrino flux on earth due to the deflection of the charged neutrino by the magnetic field of the solar convective zone. The antisymmetry of this magnetic field about the plane of the solar equator induces the anisotropy of the solar neutrino flux thus creating the deficit of the neutrino flux on the earth. The deficit has been estimated in terms of solar and neutrino parameters and the condition of a 50% deficit has been obtained: Qν grad H≥10−18 eG/cm where Qν is the neutrino electric charge, grad H is the gradient of the solar toro
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22

MORRISON, DOUGLAS R. O. "UPDATED REVIEW OF SOLAR MODELS AND SOLAR NEUTRINO EXPERIMENTS." International Journal of Modern Physics D 01, no. 02 (1992): 281–302. http://dx.doi.org/10.1142/s0218271892000148.

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The Conventional Wisdom that there is a Solar Neutrino Problem and that New Physics is required, is examined. The various solar evolutionary models, (or SSM), are described and in particular the four new 1992 papers. While the evolutionary models are generally robust, there are important assumptions and uncertainties (screening, nuclear reaction rates, etc.) which mean that the errors cannot be small. Diffusion in the Sun is expected to be significant but so far there is no calculation which includes all types of diffusion, especially turbulent diffusion. The new and important helioseismologic
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23

SMY, MICHAEL B. "CONSTRAINTS ON NEUTRINO OSCILLATION PARAMETERS FROM TIME/ENERGY DEPENDENCE OF SOLAR 8B NEUTRINO FLUX." International Journal of Modern Physics A 16, supp01b (2001): 718–20. http://dx.doi.org/10.1142/s0217751x01007881.

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A search for neutrino oscillation is presented using time variations and energy dependence of the observed reduction of the solar neutrino flux. No significant time variation or energy dependence has been found in 1117 days of solar neutrino data taken with the Super-Kamiokande experiment. This constrains the two-neutrino oscillation parameter space independently of the model dependence of the solar neutrino flux. The combination of Super-Kamiokande's data of the day-night variation, energy dependence and flux results in two allowed regions at 95% C.L.
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24

Albert, A., S. Alves, M. André, et al. "Search for solar atmospheric neutrinos with the ANTARES neutrino telescope." Journal of Cosmology and Astroparticle Physics 2022, no. 06 (2022): 018. http://dx.doi.org/10.1088/1475-7516/2022/06/018.

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Abstract Solar Atmospheric Neutrinos (SAνs) are produced by the interaction of cosmic rays with the solar medium. The detection of SAνs would provide useful information on the composition of primary cosmic rays as well as the solar density. These neutrinos represent an irreducible source of background for indirect searches for dark matter towards the Sun and the measurement of their flux would allow for a better assessment of the uncertainties related to these searches. In this paper we report on the analysis performed, based on an unbinned likelihood maximisation, to search for SAνs with the
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25

DEV, S., and JYOTI DHAR SHARMA. "THE STATUS OF THE SOLAR NEUTRINO PROBLEM IN THE RESONANT SPIN-FLAVOR PRECESSION SCENARIO WITH TWISTING SOLAR MAGNETIC FIELDS." Modern Physics Letters A 15, no. 22n23 (2000): 1445–60. http://dx.doi.org/10.1142/s0217732300001870.

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Resonant spin-flavor precession scenario with twisting solar magnetic fields has been confronted with the solar neutrino data from various ongoing experiments. In particular, the anticorrelation apparent in the Homestake solar neutrino data has been taken seriously to constrain the twisting profiles of the magnetic field in the convective zone of the Sun. The twisting profiles, thus derived, have been used to calculate the neutrino detection rates for the Homestake, Kamiokande (super-Kamiokande) and the gallium experiments. It is found that the presence of twisting reduces the degree of antico
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26

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 m
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27

IANNI, ALDO. "STATUS OF BOREXINO." International Journal of Modern Physics A 18, no. 22 (2003): 3895–907. http://dx.doi.org/10.1142/s0217751x03017245.

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Borexino is a real-time solar neutrino detector under commissioning at the Gran Sasso underground laboratories (Italy). The main goal of the experiment is the spectroscopy of sub-MeV solar neutrinos focusing on the measurement of the 7 Be neutrino flux on Earth. In order to achieve such a goal Borexino has developed a new technology for large-scale low-count rate experiments. This paper reviews the status of the experiment and the strategy adopted to reach a high level of radiopurity. Besides its primary task Borexino will also be able to search for SuperNova neutrinos, non-standard neutrinos
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INOUE, K. "REACTOR NEUTRINO EXPERIMENTS." International Journal of Modern Physics A 19, no. 08 (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 fo
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29

Gavrin, V. N., A. I. Abazov, D. N. Abdurashitov, 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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Jonathan Walg, Anatoly Rodnianski, and Itzhak Orion. "Solar flare detection method using Rn-222 radioactive source." GSC Advanced Research and Reviews 5, no. 2 (2020): 159–66. http://dx.doi.org/10.30574/gscarr.2020.5.2.0087.

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Solar neutrino detection is known to be a very challenging task, due to the minuscule absorption cross-section and mass of the neutrino. One research showed that relative large solar-flares affected the decay-rates of Mn-54 in December 2006. Since most the radiation emitted during a solar flare are blocked before reaching the earth surface, it should be assumed that such decay-rate changes could be due to neutrino flux increase from the sun, in which only neutrinos can penetrate the radionuclide. This study employs the Rn-222 radioactive source for the task of solar flare detection, based on t
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Jonathan, Walg, Rodnianski Anatoly, and Orion Itzhak. "Solar flare detection method using Rn-222 radioactive source." GSC Advanced Research and Reviews 5, no. 2 (2020): 159–66. https://doi.org/10.5281/zenodo.4319660.

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Solar neutrino detection is known to be a very challenging task, due to the minuscule absorption cross-section and mass of the neutrino. One research showed that relative large solar-flares affected the decay-rates of Mn-54 in December 2006. Since most the radiation emitted during a solar flare are blocked before reaching the earth surface, it should be assumed that such decay-rate changes could be due to neutrino flux increase from the sun, in which only neutrinos can penetrate the radionuclide. This study employs the Rn-222 radioactive source for the task of solar flare detection, based on t
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32

Abe, S., S. Asami, A. Gando, et al. "Limits on Astrophysical Antineutrinos with the KamLAND Experiment." Astrophysical Journal 925, no. 1 (2022): 14. http://dx.doi.org/10.3847/1538-4357/ac32c1.

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Abstract We report on a search for electron antineutrinos ( ν ¯ e ) from astrophysical sources in the neutrino energy range 8.3–30.8 MeV with the KamLAND detector. In an exposure of 6.72 kton-year of the liquid scintillator, we observe 18 candidate events via the inverse beta decay reaction. Although there is a large background uncertainty from neutral current atmospheric neutrino interactions, we find no significant excess over background model predictions. Assuming several supernova relic neutrino spectra, we give upper flux limits of 60–110 cm−2 s−1 (90% confidence level, CL) in the analysi
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33

RAYCHAUDHURI, PROBHAS. "SOLAR NEUTRINO FLUX VARIATION AND NEUTRINO MAGNETIC MOMENT." Modern Physics Letters A 04, no. 02 (1989): 111–14. http://dx.doi.org/10.1142/s0217732389000150.

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34

Rott, Carsten. "Progress in neutrino astronomy." Journal of the Korean Physical Society 78, no. 10 (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 f
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35

Basilico, D., S. Appel, Z. Bagdasarian, et al. "Recent results from Borexino on solar neutrinos." EPJ Web of Conferences 290 (2023): 04001. http://dx.doi.org/10.1051/epjconf/202329004001.

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Borexino has been a neutrino detector based on ultrapure liquid scintillator, located at the Laboratori Nazionali del Gran Sasso, Italy. Its main scientific goal was the real-time measurement of solar neutrino fluxes, which play an irreplaceable role for the comprehension of the mechanisms powering our star. Over the past two years, the Borexino collaboration has pursued the improvement of the CNO flux measurement, obtaining further indications about the solar metallicity. In a parallel way, Borexino has demonstrated for the first time the possibility of exploiting the directional Cherenkov in
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36

Grating, D. R., and O. L. G. Peres. "Effects of solar neutrinos scale on atmospheric neutrino flux." Brazilian Journal of Physics 37, no. 2b (2007): 626–29. http://dx.doi.org/10.1590/s0103-97332007000400027.

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37

Krastev, Plamen I., and Alexei Yu. Smirnov. "Boron neutrino flux and resonant conversion of solar neutrinos." Physics Letters B 338, no. 2-3 (1994): 282–89. http://dx.doi.org/10.1016/0370-2693(94)91379-x.

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38

Shtanov, Yu. "Cosmic neutrino from the decay of the scalaron dark matter." Bulletin of Taras Shevchenko National University of Kyiv. Astronomy, no. 66 (2022): 5–7. http://dx.doi.org/10.17721/btsnua.2022.66.5-7.

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The scalaron dark mater in F(R) gravity theory can decay into pairs of massive neutrino. We calculate the corresponding decay width and the current neutrino abundance and spectrum in the universe. The obtained neutrino flux turns out to be very small compared to the solar neutrino flux at Earth at similar energies.
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39

RAYCHAUDHURI, PROBHAS. "SOLAR NEUTRINO FLUX AND SUNSPOT DATA." Modern Physics Letters A 03, no. 14 (1988): 1319–22. http://dx.doi.org/10.1142/s0217732388001586.

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It is shown that the sunspot data and the solar neutrino data anticorrelates except for the period of three years after the sunspot maximum. This suggests that the solar activity cycle is due to the pulsating character of the nuclear energy generation inside the core of the sun.
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40

Buenker, Robert J. "The Fate of Solar Neutrinos." East African Scholars Journal of Engineering and Computer Sciences 5, no. 1 (2022): 1–3. http://dx.doi.org/10.36349/easjecs.2022.v05i01.001.

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The history of attempts to reconcile the amount of neutrino flux arriving at the earth’s surface from the sun with the profile of fusion reactions occurring on the sun is recounted. Less than half the expected number of neutrinos is actually found, which has raised questions about the reliability of the method of detection used. It is pointed out that there is a key theoretical assumption which may be incorrect, however, namely that every fusion reaction necessarily leads to the emission of a single neutrino. While this assumption is amply verified for reactions taking place under normal labor
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41

Obara, S., S. Ieki, K. Ishidoshiro, T. Mitsui, H. Watanabe, and M. P. Decowski. "Search for Supernova Relic Neutrinos at KamLAND." Journal of Physics: Conference Series 2156, no. 1 (2021): 012138. http://dx.doi.org/10.1088/1742-6596/2156/1/012138.

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Abstract We report a search for electron antineutrinos at KamLAND with an 8.3−30.8 MeV energy range via the inverse beta decay. In 6.72 kton-yr of KamLAND data, we found 18 neutrino candidates and no significant excess over estimated backgrounds. From data interpretation, with the assumption of some supernova relic neutrino spectrum predictions, we give upper flux limits of 60−110 cm−2 s−1 (90% CL) in the analysis range and present a model-independent flux. These upper limits are the most stringent for 8−13 MeV region. We also improve on the upper probability limit of 8B solar neutrinos conver
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42

AHLUWALIA, D. V. "ON RECONCILING ATMOSPHERIC, LSND, AND SOLAR NEUTRINO-OSCILLATION DATA." Modern Physics Letters A 13, no. 28 (1998): 2249–64. http://dx.doi.org/10.1142/s0217732398002400.

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The L/E-flatness of the e-like events observed in the recent atmospheric-neutrino data from super-Kamiokande (SuperK) is interpreted to reflect a new symmetry of the neutrino-oscillation mixing matrix. From that we obtain an analytical set of constraints yielding a class of mixing matrices of the property to simultaneously fit both the SuperK and the LSND data. The resulting mass squared difference relevant for the LSND experiment is found as 0.3 eV2. The discussed symmetry, e.g., carries the nature that expectation values of masses for νμ and ντ are identical. These considerations are purely
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43

Abusleme, Angel, Thomas Adam, Shakeel Ahmad, et al. "JUNO sensitivity to 7Be, pep, and CNO solar neutrinos." Journal of Cosmology and Astroparticle Physics 2023, no. 10 (2023): 022. http://dx.doi.org/10.1088/1475-7516/2023/10/022.

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Abstract The Jiangmen Underground Neutrino Observatory (JUNO), the first multi-kton liquid scintillator detector, which is under construction in China, will have a unique potential to perform a real-time measurement of solar neutrinos well below the few MeV threshold typical of Water Cherenkov detectors. JUNO's large target mass and excellent energy resolution are prerequisites for reaching unprecedented levels of precision. In this paper, we provide estimation of the JUNO sensitivity to 7Be, pep, and CNO solar neutrinos that can be obtained via a spectral analysis above the 0.45 MeV threshold
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44

Vitagliano, Edoardo, Javier Redondo, and Georg Raffelt. "Solar neutrino flux at keV energies." Journal of Cosmology and Astroparticle Physics 2017, no. 12 (2017): 010. http://dx.doi.org/10.1088/1475-7516/2017/12/010.

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45

Gnedin, Yu N., R. N. Ikhsanov, and E. V. Miletsky. "Variations of the solar neutrino flux." Proceedings of the International Astronomical Union 2004, IAUS223 (2004): 103–4. http://dx.doi.org/10.1017/s1743921304005253.

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46

Haxton, W. C. "Uncertainties in the solar neutrino flux." Nuclear Physics B - Proceedings Supplements 77, no. 1-3 (1999): 73–80. http://dx.doi.org/10.1016/s0920-5632(99)00400-4.

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47

ANICIN, I. V., V. PEJOVIĆ, M. K. PAVIĆEVIĆ, et al. "ON THE POSSIBILITY TO SIMULTANEOUSLY DETERMINE THE LONG-TERM AVERAGE FLUXES OF SOLAR pp-NEUTRINOS AND COSMIC RAY MUONS." Modern Physics Letters A 26, no. 17 (2011): 1267–71. http://dx.doi.org/10.1142/s0217732311035626.

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The Allchar mine in the southern FYR Macedonia contains the world's largest known concentration of thallium bearing minerals. LOREX (acronym for the geo-chemical LORandite EXperiment) is an international collaboration exploring the opportunity to use the rare mineral lorandite ( TlAsS 2) for the determination of the solar pp-neutrino flux, averaged over the 4.3 million year age of the deposit. Here we discuss the possibility to determine simultaneously both the solar neutrino and the cosmic ray muon flux, averaged over the same period of time. Cosmic-ray muons participate in the reaction 205 T
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48

Lim, C. S., M. Mori, Y. Oyama, and A. Suzuki. "Correlation between solar neutrino flux and solar magnetic activity for Majorana neutrinos." Physics Letters B 243, no. 4 (1990): 389–95. http://dx.doi.org/10.1016/0370-2693(90)91402-w.

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49

Sivaram, C. "Propagation and Oscillation of Neutrinos with Magnetic Moment inside the Sun." Symposium - International Astronomical Union 142 (1990): 63–64. http://dx.doi.org/10.1017/s0074180900087751.

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The VVO mechanism suggests that the existence of a neutrino magnetic moment would lead to variations of the observed solar neutrino flux with the magnetic activity of the Sun. The MSW mechansm suggests neutrino oscillations in the dense plasma solar interior. Assuming a non-vanishing neutrino magnetic moment and a magnetic field gradient increasing towards the solar core as required in some dynamo models, the combined effect of the oscillation and the flipping on neutrino propagation in the solar interior is studied. The effect of charge screening in scattering cross-section is also considered
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50

Davis, R., K. Lande, C. K. Lee, B. T. Cleveland, and J. Ullman. "Report on the Homestake Chlorine Solar Neutrino Experiment." International Astronomical Union Colloquium 121 (1990): 171–77. http://dx.doi.org/10.1017/s0252921100067920.

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AbstractA report on the results obtained from the chlorine radiochemical solar neutrino experiment in the Homestake mine, Lead, SD. Over the period 1970-1988 a neutrino capture rate of 2.3 ± 0.3 SNU was observed. This rate is discussed in relation: to the theoretical standard solar model, the results from the Kamiokande II experiment, and variations in the solar neutrino flux.
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