Готові списки джерел за темами / High energy neutrino conversion

Добірка наукової літератури з теми "High energy neutrino conversion"

Автор: Grafiati
Опубліковано: 14 березня 2023

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Статті в журналах з теми "High energy neutrino conversion"

1

CHIU, S. H. "RESONANT FLAVOR CONVERSION OF SUPERNOVA NEUTRINOS AND NEUTRINO PARAMETERS." Modern Physics Letters A 24, no. 34 (November 10, 2009): 2741–59. http://dx.doi.org/10.1142/s0217732309031855.

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Анотація:
The unknown neutrino parameters may leave detectable signatures in the supernova (SN) neutrino flux. However, even the contribution from the MSW flavor transition alone could cause ambiguity in the interpretation to the neutrino signals because of the uncertain local density profile of the SN matter and the model-dependent SN neutrino spectral parameters. A specific parametrization to the unknown local density profile is proposed in this work, and the contribution from the standard MSW effect is investigated through a multi-detector analysis of the SN neutrinos. In establishing the model-independent scheme, results based on the existing spectral models are included. The limitation of the analysis is also discussed.
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2

IBRAHIM, UNGKU FERWANI SALWA UNGKU, NOR SOFIAH AHMAD, NORHASLIZA YUSOF, and HASAN ABU KASSIM. "NEUTRINO ENERGY LOSS AT MATTER-RADIATION DECOUPLING PHASE." Modern Physics Letters A 24, no. 11n13 (April 30, 2009): 1051–54. http://dx.doi.org/10.1142/s0217732309000577.

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Neutrinos are produced copiously in the early universe. Neutrinos and antineutrinos ceased to be in equilibrium with radiation when the weak interaction rate becomes slower than the rate expansion of the universe. The ratio of the temperature of the photon to the temperature of the neutrino at this stage is Tγ/Tν = (11/4)1/3. We investigate the neutrino energy loss due to the oscillation of the electron neutrino into a different flavor in the charged-current interaction of νe-e- based on the work of Sulaksono and Simanjuntak. The energy loss from the neutrinos ΔEν during the decoupling of the neutrinos with the rest of the matter would be a gain in the energy of the electrons and can be obtained from the integration of stopping power equation ΔEν = (dEν/dT-1)dT-1 where Eν and T are the energy of the neutrinos and the temperature respectively. When the universe expands and matter-radiation decouples, an extra energy will be transferred to the photons via the annihilation of the electron-positron pairs, e++e-→γ+γ. This consequently will increase the temperature of the photons. The net effect to the lowest order is an increase in the ratio of the photon temperature to the neutrino temperature. The magnitude of energy loss of the neutrino is ∼10-4-10-5 MeV for the probability of conversion of νe → νi (i = μ,τ) between 0 to 1.0.
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3

Peres, O. L. G., and A. Yu Smirnov. "Testing the solar neutrino conversion with atmospheric neutrinos." Physics Letters B 456, no. 2-4 (June 1999): 204–13. http://dx.doi.org/10.1016/s0370-2693(99)00487-6.

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4

Blennow, Mattias, and Alexei Yu Smirnov. "Neutrino Propagation in Matter." Advances in High Energy Physics 2013 (2013): 1–33. http://dx.doi.org/10.1155/2013/972485.

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Анотація:
We describe the effects of neutrino propagation in the matter of the Earth relevant to experiments with atmospheric and accelerator neutrinos and aimed at the determination of the neutrino mass hierarchy and CP violation. These include (i) the resonance enhancement of neutrino oscillations in matter with constant or nearly constant density, (ii) adiabatic conversion in matter with slowly changing density, (iii) parametric enhancement of oscillations in a multilayer medium, and (iv) oscillations in thin layers of matter. We present the results of semianalytic descriptions of flavor transitions for the cases of small density perturbations, in the limit of large densities and for small density widths. Neutrino oscillograms of the Earth and their structure after determination of the 1–3 mixing are described. A possibility to identify the neutrino mass hierarchy with the atmospheric neutrinos and multimegaton scale detectors having low energy thresholds is explored. The potential of future accelerator experiments to establish the hierarchy is outlined.
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5

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

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Анотація:
The detection of galactic supernova (SN) neutrinos represents one of the future frontiers of low energy neutrino physics and astrophysics. The neutron coherence of neutral currents (NCs) allows quite large cross-sections in the case of neutron rich targets, which can be exploited in detecting earth and sky neutrinos by measuring nuclear recoils. They are relatively cheap and easy to maintain. These (NC) cross-sections are not dependent on flavor conversions and, thus, their measurement will provide useful information about the neutrino source. In particular, they will yield information about the primary neutrino fluxes and perhaps about the spectrum after flavor conversions in neutrino sphere. They might also provide some clues about the neutrino mass hierarchy. The advantages of large gaseous low threshold and high resolution time projection counters (TPC) detectors are discussed.
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6

BERNARDINI, A. E., and M. M. GUZZO. "INFLUENCE OF SECOND-ORDER CORRECTIONS TO THE ENERGY-DEPENDENCE OF NEUTRINO FLAVOR CONVERSION FORMULAS." Modern Physics Letters A 23, no. 23 (July 30, 2008): 1949–60. http://dx.doi.org/10.1142/s0217732308026066.

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We discuss the intermediate wave-packet formalism for analytically quantifying the energy dependence of the two-flavor conversion formula that is usually considered for analyzing neutrino oscillations and adjusting the focusing horn, target position and/or detector location of some flavor conversion experiments. Following a sequence of analytical approximations where we consider the second-order corrections in a power series expansion of the energy, we point out a residual time-dependent phase which, in addition to some well-known wave-packet effects, can subtly modify the oscillation parameters and limits. In the present precision era of neutrino oscillation experiments where higher precision measurements are required, we quantify some small corrections in neutrino flavor conversion formulas which lead to a modified energy-dependence for νμ ↔ νe oscillations.
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7

Zoller, V. R. "Coherent neutrino magnetic conversion in crystals." Physics Letters B 416, no. 3-4 (January 1998): 447–51. http://dx.doi.org/10.1016/s0370-2693(97)01177-5.

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8

TOTANI, TOMONORI, and KATSUHIKO SATO. "EFFECTS OF NEUTRINO OSCILLATION ON THE SUPERNOVA RELIC NEUTRINO BACKGROUND." International Journal of Modern Physics D 05, no. 05 (October 1996): 519–27. http://dx.doi.org/10.1142/s0218271896000321.

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We investigate to what extent the oscillation or conversion of neutrinos enhances the expected event rate of the supernova relic neutrino background (SRN) at the SuperKamiokande detector (SK). The SRN [Formula: see text] can be almost completely exchanged with vμ-like neutrinos by the MSW oscillation under the inverse mass hierarchy with Δm2~ 10−8–105[eV2], or by the magnetic moment of Majorana neutrinos with μv≳10−12μB and Δm2~10−4–10° [eV2]. In the standard calculation of the SRN flux, the event rate of the SRN [Formula: see text] at the SK in the observable energy range of 15–40 MeV can be enhanced from 1.2 yr−1 to 2.4 yr−1 if all [Formula: see text] are exchanged with vμ-like neutrinos. The enhancement is prominent especially in the high energy range (≳ 25 MeV). In the astrophysically optimistic calculation, the event rate becomes as high as 9.4 yr−1. Because the theoretical upper bound of the SRN events without oscillation is about 5 yr−1 taking into account the various astrophysical uncertainties, we might have to resort to the neutrino oscillation if more than 5 events in a year, as well as a significantly harder spectrum, were observed in the SK.
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9

Delepine, David, Vannia González Macías, Shaaban Khalil, and Gabriel López Castro. "Probing Majorana neutrino CP phases and masses in neutrino–antineutrino conversion." Physics Letters B 693, no. 4 (October 2010): 438–42. http://dx.doi.org/10.1016/j.physletb.2010.08.068.

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10

DVORNIKOV, MAXIM. "NEUTRINO SPIN RELAXATION IN MEDIUM WITH STOCHASTIC CHARACTERISTICS." International Journal of Modern Physics A 21, no. 11 (April 30, 2006): 2403–13. http://dx.doi.org/10.1142/s0217751x06028497.

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The helicity evolution of a neutrino propagating in randomly moving and polarized matter is studied. The type of the neutrino interaction with background fermions is arbitrary. We derive the equation for the description of the averaged neutrino helicity evolution. In the particular case of a τ-neutrino interacting with ultrarelativistic electron–positron plasma, we obtain the expression for the neutrino helicity relaxation rate in the explicit form. We study the neutrino spin relaxation in the relativistic primordial plasma. Supposing that the conversion of left-handed neutrinos into right-handed ones is suppressed at the early stages of the Universe evolution, we get the upper limit on the τ-neutrino mass.
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Дисертації з теми "High energy neutrino conversion"

1

Lunardini, Cecilia. "Matter Effects on Conversion of Neutrinos from Supernovae and Cosmological Sources." Doctoral thesis, SISSA, 2001. http://hdl.handle.net/20.500.11767/4324.

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This thesis collects in a unitary presentation the results of a series of papers [25, 54, 55, 56] in which we studied the effects of matter on oscillations of cosmic neutrinos from various sources. After a first introductory chapter, in chapter 2 we consider the conditions for significant matter effect; in particular we show that a minimum width of medium is required, independently of the neutrino oscillation parameters and energy, and of the matter density profile. In chapter 3 this condition is applied to high-energy neutrinos propagating across the universe: -vve find that substantial effect is produced by the relic neutrino background provided that it has a large CF-asymmetry and the neutrino source is at cosmological distance. The effect and its observability are discussed in detail. The chapters 4-6 are devoted to supernova neutrinos and their regeneration in the matter of the Earth. A detailed description of the Earth matter effect is presented in chapter 4, and in chapter 5 we give an application to the neutrino signal from SN1987 A. vVe find that the Earth effect could reconcile the difference in the energy spectra of the Kamiokande and IMB data. In chapter 6 we consider future supernova neutrino detections: we show that the Earth matter effect is observable and has important implications on the reconstruction of the neutrino mixing scheme and mass spectrum. The discussion is completed by three appendices.
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2

Nielsen, Adam Derek. "Monte Carlo calculation of fluence-to-ambient dose equivalent conversion coefficients for high-energy neutrons." Thesis, Georgia Institute of Technology, 1998. http://hdl.handle.net/1853/16424.

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3

Allport, P. P. "High energy neutrino scattering at low Q'2." Thesis, University of Oxford, 1986. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.376865.

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4

Guillaud, Mathilde. "Neutrino oscillations at very high energy/matter density." Thesis, KTH, Fysik, 2020. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-292510.

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Анотація:
Neutrino oscillations in matter can be studied in different regimes, depending on the energy of the incoming neutrinos and the matter density of the medium. In this thesis we investigate neutrino oscillations in dense matter at very high energy (TeV-PeV range), taking into account the absorption that the neutrinos may undergo in such dense media. This absorption phenomenon is relevant for neutrino telescope measurements of astrophysical neutrinos. We begin with a brief reminder on neutrino oscillations in vacuum and the construction of the PMNS matrix. Then, we proceed with calculations for dense matter. We then explore the accuracy of the resulting effective 2-neutrino mixing formulas. They present a good accuracy for Earth-like densities in our range of energies. We develop the calculations for oscillation probabilities in dense matter with absorption through charged-current inelastic scattering for both the two-neutrino and three-neutrino case. We find that in dense media, astrophysical neutrinos indeed undergoabsorption, which reduces signicantly the fluxes for each flavor, with a resonant absorption of electron-anti-neutrinos around E_{res}\simeq 6.3PeV. We discuss the impact of neutrino absorption in the Earth for neutrino telescopes measurements. We find that solar and lunar shadowing is not problematic for current telescopes but could be a good angular resolution indicator for new telescopes to come.
Neutrinooscillationer i materia kan studeras i olika regimer beroende på inkommande neutrinernas energi och densiteten hos det bakomliggande mediet. I detta examensarbete undersöker vi neutrinooscillationer i gränsen av tät materia och mycket hög energi (TeV-PeV-intervall), och tar hänsyn till den absorption av neutriner som då kan inträffa i sådant materia. Detta absorptionsfenomen är relevant för neutrino-teleskopmätningar av astrofysiska neutriner. Vi börjar med att kort påminna oss om neutrinooscillationer i vakuum och konstruktionen av PMNS-matrisen. Vi försätter sedan med beräkningar av neutrinooscillationer i tät materia. Vi undersöker noggrannheten i resulterande effektiva 2-neutrino-blandningsformlerna. De uppvisar en god noggrannhet i jordlika materieprofiler i vårt intervall av energier. Vi utvecklar beräkningarna av oscillationssannolikheterna i tät materia inklusive absorption genom laddad ström oelastisk spridning i båda två- och tresmaksfallen. Vi finner att astrofysiska neutriner i tät materia absorberas, vilket minskar betydligt flödena för varje smak, med en resonansabsorption av elektron-antineutrino omkring E_res\simeq 6.3PeV. Vi diskuterar sedan effekterna av neutrinoabsorption på jorden för neutrino-teleskopmätningar. Vi finner att sol- och månskuggning är inte problematisk för nuvarande teleskop och kunde vara en bra vinkelupplösningsindikator för kommande teeskop.
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5

Li, Xiaoyue. "A Joint Analysis of T2K Beam Neutrino and Super-Kamiokande Sub-GeV Atmospheric Neutrino Data." Thesis, State University of New York at Stony Brook, 2018. http://pqdtopen.proquest.com/#viewpdf?dispub=10844911.

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Neutrino oscillation is a phenomenon in which neutrinos produced from charged current weak interactions can change flavor as they propagate. The mixing between the three flavor eigenstates and mass eigenstates can be measured through neutrino oscillations as the oscillation probabilities depend on the mixing angles and neutrino mass squared differences.

T2K is a long baseline neutrino experiment, in which a nearly pure muon neutrino or muon antineutrino beam is produced at J-PARC on the east coast of Japan and travels 295 km through the Earth’s crust towards the far detector, Super-Kamiokande (Super-K), a 50 kiloton water Cherenkov detector, in the west of Japan. The neutrino fluxes in the absence of oscillation are measured by the near detectors 280 meters away from the target, and again with oscillation effects at Super-K. Aside from the beam neutrino from J-PARC, Super-K also measures neutrino oscillations independently through the neutrinos produced in the Earth's atmosphere.

This thesis presents the first analysis in which both the T2K beam neutrino data and the sub-GeV atmospheric neutrino data at Super-K are used in a unified framework to measure neutrino oscillation parameters. The beam neutrino samples are selected for optimal sensitivity to sin2&thetas;23 and δCP. A Bayesian analysis using a Markov Chain Monte Carlo method is performed. Using T2K Runs 1–8 data which amounts to 14.7 × 1020 protons on target (POT) in neutrino-mode and 7.6 × 1020 POT in antineutrino-mode, and 2520 days of Super-K data, the oscillation parameters are measured to be sin2&thetas; 23 = 0.528+0.032–0.028, |Δ m232| = 2.46+0.084 –0.060(10–3eV2), sin 2&thetas;13 = 0.0270+0.0065–0.0047 ; and the 90% credible interval of δCP is [–π, –0.18]&[2.33, π]. When the data is also combined with the constraint on sin2 2&thetas;13 = 0.0857 ± 0.046 from reactor neutrino experiments, the oscillation parameters are measured to be sin2&thetas;23 = 0.543+0.026 –0.023, |Δm2 32| = 2.49 +0.042–0.090(10–3eV2 ), sin2&thetas;13 = 0.0223+0.0012 –0.0013; the 90% credible interval of δ CP is [–π, –0.628], and the CP-conserving value δ CP = 0 is excluded at 2σ.

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6

Michaud, Denis 1970. "Neutrino propagation through matter." Thesis, McGill University, 1994. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=55513.

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In this thesis, we examine the evolution of a quantum system through background matter in order to determine the conditions of validity required for a description in terms of an effective Hamiltonian. General scattering rate equations are obtained for coherent diffuse scattering. We find, as expected, that the diffuse scattering rate is small compared to the coherent scattering rate in a medium with low fluctuations allowing an effective Hamiltonian description. However, for a more turbulent background, it is still possible to have more significant contributions to the diffuse scattering which may affect the existing theory of neutrino flavor conversion (MSW effect).
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7

Gamsizkan, Halil. "A Qcd Analysis Of High Energy Neutrino-nucleon Interactions." Master's thesis, METU, 2003. http://etd.lib.metu.edu.tr/upload/1006428/index.pdf.

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In this thesis, a leading-order QCD analysis of structure functions in neutrinonucleon interactions is performed. From the CCFR nucleon structure function data, the QCD parameter Lambda has been extracted. This measurement also corresponds to a measurement of the strong coupling constant. Two fits to the data have been performed, the nonsinglet-only fit and the singlet-nonsinglet combined fit. The result for Lambda was found to be 289 +62 ¡
59 §
76 MeV, where the errors are statistical and systematical, respectively. This result is compared to the world-wide measurements of this quantity. In order to verify the agreement, also the logarithmic slopes of the QCD model and the structure function data are calculated and compared.
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8

Olivo, Martino. "Neutrino emission from high-energy component gamma-ray bursts." Licentiate thesis, Uppsala universitet, Högenergifysik, 2010. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-132961.

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Gamma-ray bursts (GRBs) are brief and sudden explosions radiating most of their energy in the soft γ-ray band ( 100 keV). In the context of multimessenger astroparticle physics recent observations of GRBs provide an excellent benchmark for testing theoretical models of high energy emission mechanisms. Acceleration of hadrons in the engine is expected to produce high energy neutrinos and gamma-rays simultaneously via π±/π0 decays, thus reinforcing the motivation for coincident searches in km3 neutrino telescopes. The Waxman-Bachall spectra and the corresponding expected neutrino rates in IceCube are derived here for GRB090510 amd GRB090902B recently detected by the Fermi Large Area Telescope. The implications of the significant detection of deviations from the Band function fit in photon spectra and a model that explains these extra-components in terms of π0-decay photons are presented here and the relevance to neutrino astronomy is shown.
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9

Hill, Gary Colin. "Experimental and theoretical aspects of high energy neutrino astrophysics /." Title page, table of contents and summary only, 1996. http://web4.library.adelaide.edu.au/thesis/09PH/09phh6461.pdf.

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10

O'Rourke, Brogan Roisín. "AGN Candidates for High Energy Neutrino Emission in IceCube." Thesis, Uppsala universitet, Högenergifysik, 2020. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-409739.

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Since the construction of the IceCube Neutrino Observatory was completed in 2010, many amazing discoveries have been made in the field of neutrino physics. Recently a neutrino event has been linked to an blazar-type active galactic nucleus source, bringing us one step closer to understanding the production of high-energy extragalactic neutrinos and ushering in a new era of multimessenger astronomy. This was found by linking the neutrino event to one of the Fermi Collaboration’s gamma ray sources which had a blazar counterpart. The quest to link other neutrino events to AGN (active galactic nuclei) sources through collaboration with the Fermi Large Area Telescope has turned up some interesting candidates. The fact that some of these potential sources are not blazars is curious and, although unconfirmed as neutrino sources, these objects merit further investigation due to their unusual nature.
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Книги з теми "High energy neutrino conversion"

1

Halzen, F. Icecube and the discovery of high-energy cosmic neutrinos. Firenze: Leo S. Olschki, 2018.

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2

Shi, Yixiang, Ningsheng Cai, Tianyu Cao, and Jiujun Zhang. High-Temperature Electrochemical Energy Conversion and Storage. Boca Raton : CRC Press, Taylor & Francis Group, 2018. | Series: Electrochemical energy store & conversion: CRC Press, 2017. http://dx.doi.org/10.1201/b22506.

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3

Workshop on High Energy Neutrino Astrophysics (1992 Honolulu, Hawaii). Proceedings of the Workshop on High Energy Neutrino Astrophysics, Honolulu, Hawaii, 23-26 March 1992. Edited by Stenger Victor J. 1935-. Singapore: World Scientific, 1992.

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4

1938-, Barger V., and Cline D. 1933-, eds. Neutrino mass and low energy weak interactions, Telemark, 1984. Singapore: World Scientific, 1985.

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5

United States. High Energy Physics Advisory Panel. Subpanel on Accelerator-Based Neutrino Oscillation Experiments. High Energy Physics Advisory Panel, Subpanel on Accelerator-Based Neutrino Oscillation Experiments. Washington, D.C: U.S. Dept. of Energy, Office of Energy Research, Division of High Energy Physics, 1995.

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6

United States. Dept. of Energy. Office of Energy Research, ed. Report of the HEPAP Subpanel on High Energy Gamma Ray and Neutrino Astronomy. Washington, D.C: U.S. Dept. of Energy, Office of Energy Research, 1988.

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7

Gaisser, Thomas K. High energy neutrino absorption and its effect on stars in close X-ray binaries. Greenbelt, Md: National Aeronautics and Space Administration, Goddard Space Flight Center, 1986.

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8

Goetzberger, A., Vesselinka Petrova-Koch, and Rudolf Hezel. High-efficient low-cost photovoltaics: Recent developments. Edited by SpringerLink (Online service). Berlin: Springer, 2009.

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9

Shin Enerugī Sangyō Gijutsu Sōgō Kaihatsu Kikō (Japan), ed. Baiomasu enerugī kōkōritsu tenkan gijutsu kaihatsu (tenkan yōso gijutsu kaihatsu): Shin enerugī gijitsu kenkyū kaihatsu = High efficiency bioenergy conversion project (development of elemental technologies for bioenergy conversion) : new energy technology development. Kawasaki-shi: Shin Enerugi ̄ Sangyō Gijutsu Sōgō Kaihatsu Kikō, 2008.

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10

Chubb, Donald L. High efficiency thermal to electric energy conversion using selective emitters and spectrally tuned solar cells. [Washington, DC]: National Aeronautics and Space Administration, 1992.

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Частини книг з теми "High energy neutrino conversion"

1

Horvath, Jorge Ernesto. "Neutrino Astrophysics." In High-Energy Astrophysics, 187–202. Cham: Springer International Publishing, 2022. http://dx.doi.org/10.1007/978-3-030-92159-0_9.

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2

Lee, T. D. "High-energy neutrino experiments." In Selected Papers, 75–90. Boston, MA: Birkhäuser Boston, 1986. http://dx.doi.org/10.1007/978-1-4612-5397-6_14.

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3

Lee, T. D. "High-energy neutrino experiments." In Selected Papers, 91–102. Boston, MA: Birkhäuser Boston, 1986. http://dx.doi.org/10.1007/978-1-4612-5397-6_15.

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4

Lee, T. D. "High-energy neutrino experiments." In Selected Papers, 103–16. Boston, MA: Birkhäuser Boston, 1986. http://dx.doi.org/10.1007/978-1-4612-5397-6_16.

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5

Resvanis, L. K. "High Energy Neutrino Telescopes." In TeV Gamma-Ray Astrophysics, 213–34. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_17.

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6

Spurio, Maurizio. "High-Energy Neutrino Astrophysics." In Astronomy and Astrophysics Library, 321–57. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-08051-2_10.

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7

Spurio, Maurizio. "High-Energy Neutrino Astrophysics." In Astronomy and Astrophysics Library, 355–99. Cham: Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96854-4_10.

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Mintz, S. L., G. M. Gerstner, M. A. Barnett, and M. Pourkaviani. "Neutrino and Anti-Neutrino Reactions in Nuclei." In High-Energy Physics and Cosmology, 35–55. Boston, MA: Springer US, 1997. http://dx.doi.org/10.1007/978-1-4615-5397-7_4.

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9

Sen, Manibrata. "Supernova Neutrinos: Fast Flavor Conversions Near the Core." In XXII DAE High Energy Physics Symposium, 533–37. Cham: Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-73171-1_125.

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10

Vannucci, F. "Neutrino Oscillations at Accelerators." In High-Energy Physics and Cosmology, 21–26. Boston, MA: Springer US, 1997. http://dx.doi.org/10.1007/978-1-4615-5397-7_2.

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Тези доповідей конференцій з теми "High energy neutrino conversion"

1

Bhattacharyya, Soumya. "Fast Neutrino Flavor Conversion at Late Time." In 40th International Conference on High Energy physics. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.390.0196.

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2

Batkin, I. S., and M. K. Sundaresan. "Coherent conversion of neutrino flavor by collisions with relic neutrino gas." In High energy physics at the millennium: MRST (Montreal-Rochester-Syracuse-Ontario)’99 "The sundarfest". American Institute of Physics, 1999. http://dx.doi.org/10.1063/1.1301297.

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3

Yanli, Xiong, Qiu Xiaopeng, Liu Shuhuan, Li Zhuoqi, Liu Shuangying, Ma Yong, Song Ci, and Han Ning. "Simulation and Analysis of 4H-SiC-Based PiN Fast Neutron Detector With Polyethylene Converter Using Geant4." In 2022 29th International Conference on Nuclear Engineering. American Society of Mechanical Engineers, 2022. http://dx.doi.org/10.1115/icone29-92268.

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Анотація:
Abstract When detecting fast neutrons, generally select materials with high hydrogen content, such as polyethylene and lithium hydride. It’s known that polyethylene is widely used and has high detect efficiency. Therefore, this paper uses Geant4 software to simulate 4H-SiC-based PiN fast neutron detector with polyethylene converter of varies thickness. With the increase of converter thickness, the conversion efficiency of 1–14MeV monoenergetic fast neutron will first increase and then decrease. By analysing the trend of conversion efficiency, the thickness is determined as 1000um. Then, the 1MeV, 2MeV, 4MeV and 8MeV monoenergetic neutrons and typical fats neutron source: Am-Be neutron source are simulated under the thickness of 1000um convertor, the particle types and energy distribution to the sensitive volume and the energy deposition of particles in the sensitive region are also obtained. Through the analysis of recoil proton energy spectrum, the relationship between incident neutron energy and recoil proton energy are studied. Also, through the analysis of PKA (primary knocked-out atoms) energy spectrum, we found that the main reactions in epi-layer are 28Si(n,n’) 28Si, 12C(n,n’) 12C, 28Si(n,α) 25Mg, 28Si(n,p) 28Al, etc. It is found that heavy ions such as C and Si produced by neutrons in sensitive volume account for a large proportion. The above research finally helps to investigate the deposit energy in the epi-layer.
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4

Takeishi, Taichi, Satoshi Takeda, and Takanori Kitada. "Improvement of Conversion Ratio of Thorium Fuel in LWR by Adding Neutron Absorber." In 2021 28th International Conference on Nuclear Engineering. American Society of Mechanical Engineers, 2021. http://dx.doi.org/10.1115/icone28-65683.

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Abstract The reproduction factor of Th232 is high in the thermal energy range and there is a possibility to achieve the breeding in LWRs. However, it is necessary to improve the conversion ratio since the breeding is difficult in LWRs. The conversion ratio can be improved by suppressing capture rate of Pa233 and by promoting capture rate of Th232. In addition, these capture rates can be modified by adding neutron absorber. Therefore, the neutron absorber is focused for improving the conversion ratio in this study. The high resonance peaks of Pa233 capture cross section exist around 1∼100 eV. The resonance peaks of Th232 are higher than 10 eV. Thus, when the 1∼10 eV neutrons are suppressed in the fuel, the Pa233 resonance capture reaction is suppressed and the Th232 resonance capture reaction is promoted by neutron spectrum hardening. Therefore, six neutron absorbers that have high capture cross section peaks at 1∼10 eV were selected. The PWR pin cell calculations were carried out by Monte Carlo code MVP. The fuels are composed of a base material and an absorber. The base material is an oxidized fuel composed of U233(10 wt%), Th232(89.95 wt%), and Pa233(0.05 wt%). The amount of neutron absorber was adjusted so that the infinite multiplication factor becomes 1.33. The impact of adding neutron absorber on the reaction rate was evaluated. As the result, the hardening of the neutron spectrum leads increase of the capture rate of Pa233, and the capture rate of Th232 in the epithermal energy range is increased. The change of capture rate of Th232 is greater than that of Pa232. Therefore, the conversion ratio is found to be improved by adding neutron absorber.
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5

STANEV, TODOR. "HIGH ENERGY NEUTRINO ASTRONOMY." In Proceedings of the 13th Course of the International School of Cosmic Ray Astrophysics. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702968_0030.

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6

HALZEN, FRANCIS. "HIGH-ENERGY NEUTRINO ASTRONOMY." In Proceedings of the International Conference. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702999_0020.

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7

Halzen, Francis. "High-Energy Neutrino Astronomy." In THE NEW COSMOLOGY: Conference on Strings and Cosmology; The Mitchell Symposium on Observational Cosmology. AIP, 2004. http://dx.doi.org/10.1063/1.1848331.

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MIGNECO, E. "HIGH ENERGY NEUTRINO ASTRONOMY." In Proceedings of the International Symposium EXOCT07. WORLD SCIENTIFIC, 2008. http://dx.doi.org/10.1142/9789812797049_0033.

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Halzen, Francis. "High-Energy Neutrino Astronomy." In Proceedings of Nobel Symposium 129. WORLD SCIENTIFIC, 2006. http://dx.doi.org/10.1142/9789812773906_0015.

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Stenger, V. J., J. G. Learned, S. Pakvasa, and X. Tata. "High Energy Neutrino Astrophysics." In Proceedings of the Workshop. WORLD SCIENTIFIC, 1992. http://dx.doi.org/10.1142/9789814537353.

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Звіти організацій з теми "High energy neutrino conversion"

1

Abbasabadi, A., A. Devoto, D. A. Dicus, and W. W. Repko. High energy photon-neutrino interactions. Office of Scientific and Technical Information (OSTI), July 1998. http://dx.doi.org/10.2172/639760.

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2

Coan, Thomas. High Energy Neutrino Physics with NOvA. Office of Scientific and Technical Information (OSTI), September 2016. http://dx.doi.org/10.2172/1323468.

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3

Oltman, Edward. Nucleon Structure Functions from High-Energy Neutrino and Anti-Neutrino Interactions in Iron. Office of Scientific and Technical Information (OSTI), January 1989. http://dx.doi.org/10.2172/1427781.

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4

Iocco, F. High Energy Neutrino Signals from the Epoch of Reionization. Office of Scientific and Technical Information (OSTI), July 2007. http://dx.doi.org/10.2172/909542.

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5

Crotty, Patrick R. High-energy neutrino fluxes from the supermassive dark matter. Office of Scientific and Technical Information (OSTI), January 2002. http://dx.doi.org/10.2172/1420932.

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Strongin, Boris. Opposite Sign Dimuon Production in High-Energy Neutrino - Nucleon Interactions. Office of Scientific and Technical Information (OSTI), January 1989. http://dx.doi.org/10.2172/1427776.

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7

Vaitaitis, Arturas Genrikas. Search for neutral heavy leptons in a high-energy neutrino beam. Office of Scientific and Technical Information (OSTI), January 2000. http://dx.doi.org/10.2172/1421441.

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Lang, Karol. An Experimental Study of Dimuons Produced in High-Energy Neutrino Interactions. Office of Scientific and Technical Information (OSTI), January 1985. http://dx.doi.org/10.2172/1433242.

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9

Kirchstetter, Thomas. High-temperature thermal energy storage with thermophotovoltaic energy conversion (Final Report). Office of Scientific and Technical Information (OSTI), December 2020. http://dx.doi.org/10.2172/1881904.

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10

Mekhiche, Mike, Hiz Dufera, and Deb Montagna. Advanced, High Power, Next Scale, Wave Energy Conversion Device. Office of Scientific and Technical Information (OSTI), October 2012. http://dx.doi.org/10.2172/1097434.

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