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Relevant bibliographies by topics / Electron neutrinos; Solar Neutrino Observatory

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Academic literature on the topic 'Electron neutrinos; Solar Neutrino Observatory'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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

1

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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5

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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6

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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8

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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Dissertations / Theses on the topic "Electron neutrinos; Solar Neutrino Observatory"

1

Heron, Heidi. "Techniques to measure the NC background in the SNO experiment." Thesis, University of Oxford, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.244578.

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Orrell, John Laurence. "A search for an electron antineutrino signal in the Sudbury Neutrino Observatory /." Thesis, Connect to this title online; UW restricted, 2004. http://hdl.handle.net/1773/9794.

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Cox-Mobrand, Gary A. "Data integrity and electronic calibrations for the neutral current detector phase measurement of the 8B solar neutrino flux at the Sudbury Neutrino Observatory /." Thesis, Connect to this title online; UW restricted, 2008. http://hdl.handle.net/1773/9647.

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4

Smith, Miles Walter Eldon. "An investigation of matter enhanced neutrino oscillation with the Sudbury Neutrino Observatory /." Thesis, Connect to this title online; UW restricted, 2002. http://hdl.handle.net/1773/9701.

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Miknaitis, Kathryn Kelly Schaffer. "A search for matter enhanced neutrino oscillations through measurements of day and night solar neutrino fluxes at the Sudbury Neutrino Observatory /." Thesis, Connect to this title online; UW restricted, 2005. http://hdl.handle.net/1773/9636.

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6

Paterson, David John Carleton University Dissertation Physics. "Studies of a novel method for solar neutrino neutral current detection in the Sudbury neutrino observatory." Ottawa, 1989.

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7

Loach, James Chilton. "Measurement of the Flux of 8B Solar Neutrinos at the Sudbury Neutrino Observatory." Thesis, University of Oxford, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.490107.

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The Sudbury Neutrino Observatory (SNO) was a heavy water Cerenkov detector that had the unique ability to measure both the total il active flux of solar neutrino, using a neutral current (NC) interaction, and the flux of electron neutrinos, using a charged current (CC) interaction. The experiment has demonstrated that neutrinos 3 change flavour and that the total neutrino flux is consistent with the prediction of solar models.

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8

Laberge, Gaetan (Gaetan Joseph Henri) Carleton University Dissertation Physics. "212Pb assay for the determination of the neutral current background at the Sudbury Neutrino Observatory." Ottawa, 1995.

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9

Stonehill, Laura C. "Deployment and background characterization of the Sudbury Neutrino Observatory neutral current detectors /." Thesis, Connect to this title online; UW restricted, 2005. http://hdl.handle.net/1773/9665.

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O'Keeffe, Helen Mary. "Low energy background in the NCD phase of the Sudbury Neutrino Observatory." Thesis, University of Oxford, 2008. http://ora.ox.ac.uk/objects/uuid:b53c04b1-5dba-4cfb-98ec-c0d8b87fb58b.

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The Sudbury Neutrino Observatory (SNO) was a 1 kilotonne heavy water Č{C}erenkov detector. Evidence for flavour changing neutrino oscillations was found by comparing the rate of Charged Current interactions with that of Neutral Current (NC) interactions. This thesis is concerned with the accurate determination of the NC flux in the Neutral Current Detector (NCD) phase of SNO. The measurement and understanding of radioactive backgrounds arising from decays of naturally occurring $^{232}$Th and $^{238}$U chain nuclei is crucial. This is because their daughter nuclei can produce neutrons via photodisintegration of deuterium. These would be indistinguishable from those produced by NC neutrino interactions. As the probability of neutron production was dependent upon the nature and location of activity, each contribution had to be determined separately. Of particular concern were $^{232}$Th and $^{238}$U in the D$_2$O and Neutral Current Detectors (NCDs). A maximum likelihood method was developed that exploited differences in the event isotropy and radial profile of each event class. These results were in agreement with water assay results and pre-deployment radioassays of the NCDs. An independent measurement of the $^{232}$Th content in the D$_2$O and H$_2$O was made by regularly assaying the water using filters loaded with hydrous titanium oxide. The concentration of $^{232}$Th in the water was determined by coincidence counting of the final assay sample. A new counter system was designed and built and the calibration and use of this system are presented. Two areas of increased activity were discovered on two of the NCDs deployed in the detector which would have prevented an accurate measurement of the NC flux. A method was devised to determine the composition and activity of one of these hotspots. The results were in good agreement with two independent methods and the uncertainty on the NC flux was reduced from $>7$% to $<1$%. The total number of neutrons produced per day by photodisintegration for $^{232}$Th and $^{238}$U in the D$_2$O and NCDs was measured to be $0.66^{+0.08}_{-0.07}$. This was significantly less than the expected 12.6 NC neutrino interactions per day. In the third phase, two independent data streams existed: PMT and NCD. A Monte Carlo study was undertaken to determine whether an accurate measure of the NC flux could be obtained using only PMT data. Results showed that no improvement could be made upon results from previous phases and the best measurement of the NC flux in the final phase would be made using PMT and NCD data.

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Books on the topic "Electron neutrinos; Solar Neutrino Observatory"

1

Dragowsky, Michael Raymond. Sudbury Neutrino Observatory energy calibration using gamma-ray sources. 1999.

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Book chapters on the topic "Electron neutrinos; Solar Neutrino Observatory"

1

Ewan, G. T. "Sudbury Neutrino Observatory." In Solar Neutrinos, 133–35. CRC Press, 2018. http://dx.doi.org/10.1201/9780429502811-44.

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2

’t Hooft, G. "Prediction For Neutrino-Electron Cross-Sections In Weinberg’s Model Of Weak Interactions." In Solar Neutrinos, 27–28. CRC Press, 2018. http://dx.doi.org/10.1201/9780429502811-10.

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3

Bahcall, John N., Raymond Davis, Peter Parker, Alexei Smirnov, and Roger Ulrich. "Measurement of the Rate of ve + d→p + p + e- Interactions Produced by 8B Solar Neutrinos at the Sudbury Neutrino Observatory." In Solar Neutrinos, 451–56. CRC Press, 2018. http://dx.doi.org/10.1201/9780429502811-121.

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Conference papers on the topic "Electron neutrinos; Solar Neutrino Observatory"

1

EJIRI, H., T. ITAHASHI, T. SHIMA, R. HAZAMA, Y. IKEGAMI, K. MATSUOKA, H. NAKAMURA, et al. "MOON(MO OBSERVATORY OF NEUTRINOS) FOR NEUTRINO STUDIES BY DOUBLE BETA DECAYS AND LOW ENERGY SOLAR NEUTRINOS." In Proceedings of the Fourth International Workshop. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812703101_0038.

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2

De Wasseige, Gwenhaël. "First search for GeV neutrinos from bright gamma-ray solar flares using the IceCube Neutrino Observatory." In 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.1075.

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3

KLAPDOR-KLEINGROTHAUS, H. V. "NEW UNDERGROUND NEUTRINO OBSERVATORY — GENIUS— IN THE NEW MILLENIUM : FOR SOLAR NEUTRINOS, DARK MATTER AND DOUBLE BETA DECAY." In Proceedings of the 2nd International Workshop. WORLD SCIENTIFIC, 2002. http://dx.doi.org/10.1142/9789812778000_0013.

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Hazama, Ryuta, Hiroyasu Ejiri, Jonathan Engel, Plamen Krastev, Nobuyuki Kudomi, Masaharu Nomachi, and R. G. Hamish Robertson. "MOON (Mo Observatory Of Neutrinos) for neutrino studies in [sup 100]Mo by double beta decays and solar-ν capture reactions." In NUCLEAR PHYSICS IN THE 21st CENTURY:International Nuclear Physics Conference INPC 2001. AIP, 2002. http://dx.doi.org/10.1063/1.1470263.

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