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1
Hargrove, C. K., and D. J. Paterson. "Solar-neutrino neutral-current detection methods in the Sudbury neutrino observatory." Canadian Journal of Physics 69, no. 11 (November 1, 1991): 1309–16. http://dx.doi.org/10.1139/p91-196.
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The Sudbury Neutrino Observatory will study the solar-neutrino problem through the detection of charged-current (CC), neutral-current (NC), and elastic-scattering (ES) interactions of solar neutrinos with heavy water. The measurement of the NC rate relative to the CC rate provides a nearly model-independent method of observing neutrino oscillations. The NC interaction breaks up the deuteron producing a neutron and a proton. The interaction rate in the original design is measured by observing Čerenkov light from showers produced by neutron-capture γ rays from the capture of the NC neutrons by a selected additive to the heavy water. These signals overlap the CC and ES signals, so that the measurement of the NC rate requires the subtraction of two signals obtained at different times. This paper describes our investigation of an alternate detection method in which the thermalized neutrons are captured by (n, α) or (n, p) reactions on light nuclei. The resulting charged-particle products are uniquely detected by scintillators or proportional counters, completely separating this NC signal from the CC and ES Čerenkov signals, thus simplifying its measurement, improving its significance, and allowing observation of otherwise unobservable short-term NC fluctuations. Although background rates for the new techniques have not yet been determined, the experimental advantages justify further development work.
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Caravaca, J. "SNO: Recent new results." International Journal of Modern Physics A 35, no. 34n35 (December 15, 2020): 2044012. http://dx.doi.org/10.1142/s0217751x20440121.
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The Sudbury Neutrino Observatory (SNO), whose main purpose was to study the neutrinos produced in the Sun, demonstrated that neutrinos can change flavor and, thus, they are massive particles. SNO detected and recorded neutrino and cosmic ray interactions from 1999 to 2006 and several analyses have been completed in the past year using legacy data. We present the results of the most recent ones: the measurements of neutron production in atmospheric neutrino interactions and neutron production by cosmic muons, a search for Lorentz symmetry violation in neutrino oscillations and a search for neutrino decay. A few other analyses are ongoing and we comment about their goal and status.
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Abe, Seisho. "Nuclear de-excitation associated with neutrino-carbon interactions." Journal of Physics: Conference Series 2156, no. 1 (December 1, 2021): 012189. http://dx.doi.org/10.1088/1742-6596/2156/1/012189.
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Abstract Neutrino interactions in low energy regions below 30 MeV, where the experimental searches for supernova relic neutrino are conducted, have a large uncertainty due to complicated nuclear effects such as the Pauli blocking effect and de-excitation of a residual nucleus. Understanding the effect of nuclear de-excitation is especially critical since neutrons measured by liquid scintillator detectors can be emitted via de-excitation. We build a systematic method to predict nuclear de-excitation associated with neutrino-carbon interaction using TALYS and Geant4. This prediction is combined with the results of neutrino event generators, and we find a large increase in neutron multiplicity.
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Balantekin, A. Baha, Michael J. Cervia, Amol V. Patwardhan, Rebecca Surman, and Xilu Wang 王夕露. "Collective Neutrino Oscillations and Heavy-element Nucleosynthesis in Supernovae: Exploring Potential Effects of Many-body Neutrino Correlations." Astrophysical Journal 967, no. 2 (May 28, 2024): 146. http://dx.doi.org/10.3847/1538-4357/ad393d.
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Abstract In high-energy astrophysical processes involving compact objects, such as core-collapse supernovae or binary neutron star mergers, neutrinos play an important role in the synthesis of nuclides. Neutrinos in these environments can experience collective flavor oscillations driven by neutrino–neutrino interactions, including coherent forward scattering and incoherent (collisional) effects. Recently, there has been interest in exploring potential novel behaviors in collective oscillations of neutrinos by going beyond the one-particle effective or “mean-field” treatments. Here, we seek to explore implications of collective neutrino oscillations, in the mean-field treatment and beyond, for the nucleosynthesis yields in supernova environments with different astrophysical conditions and neutrino inputs. We find that collective oscillations can impact the operation of the ν p-process and r-process nucleosynthesis in supernovae. The potential impact is particularly strong in high-entropy, proton-rich conditions, where we find that neutrino interactions can nudge an initial ν p-process neutron-rich, resulting in a unique combination of proton-rich low-mass nuclei as well as neutron-rich high-mass nuclei. We describe this neutrino-induced neutron-capture process as the “ν i-process.” In addition, nontrivial quantum correlations among neutrinos, if present significantly, could lead to different nuclide yields compared to the corresponding mean-field oscillation treatments, by virtue of modifying the evolution of the relevant one-body neutrino observables.
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Nakarmi, Prabandha, and Jeevan Jyoti Nakarmi. "Significance of neutrino-neutrino interaction in neutrino oscillation in core-collapse supernova." BIBECHANA 12 (December 17, 2014): 89–95. http://dx.doi.org/10.3126/bibechana.v12i0.11780.
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We study the possibility of neutrino-neutrino interaction inside the neutrino core of supernova (ρ ≥ 1010 g/cc) and outside the neutrinosphere. The angular dependence of the neutrino-neutrino interaction Hamiltonian causes multi-angle effects that can lead either to oscillation or free streaming of neutrinos. If the angle between interactions is π/2, the neutrinos are trapped inside neutrino core and chances of oscillation increases due to interaction. As the angle gradually changes, the chance of oscillation decreases and free streaming of neutrino can be observed out of core of supernova as shock waves.DOI: http://dx.doi.org/10.3126/bibechana.v12i0.11780 BIBECHANA 12 (2015) 89-95
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Esteban, Ivan, Sujata Pandey, Vedran Brdar, and John F. Beacom. "Astrophysical neutrino self-interactions in the high-statistics era." Journal of Physics: Conference Series 2156, no. 1 (December 1, 2021): 012103. http://dx.doi.org/10.1088/1742-6596/2156/1/012103.
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Abstract Do neutrinos have sizable self-interactions? They might. Laboratory constraints are weak, so strong effects are possible in astrophysical environments and the early universe. Observations with neutrino telescopes can provide an independent probe of neutrino self (“secret”) interactions, as the sources are distant and the cosmic neutrino background intervenes. We define a roadmap for making decisive progress on testing these interactions. This progress will be enabled by IceCube-Gen2 observations of high-energy astrophysical neutrinos. Critical to this is our comprehensive treatment of the theory, taking into account previously neglected or overly approximated effects, as well as including realistic detection physics. We show that IceCube-Gen2 can realize the full potential of neutrino astronomy for testing neutrino self-interactions, being sensitive to cosmologically relevant interaction models.
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An, Rui, Vera Gluscevic, Ethan O. Nadler, and Yue Zhang. "Can Neutrino Self-interactions Save Sterile Neutrino Dark Matter?" Astrophysical Journal Letters 954, no. 1 (August 31, 2023): L18. http://dx.doi.org/10.3847/2041-8213/acf049.
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Abstract Sterile neutrinos only interact with the standard model through the neutrino sector, and thus represent a simple dark matter (DM) candidate with many potential astrophysical and cosmological signatures. Recently, sterile neutrinos produced through self-interactions of active neutrinos have received attention as a particle candidate that can yield the entire observed DM relic abundance without violating the most stringent constraints from X-ray observations. We examine consistency of this production mechanism with the abundance of small-scale structure in the universe, as captured by the population of ultrafaint dwarf galaxies orbiting the Milky Way, and derive a lower bound on the sterile-neutrino particle mass of 37 keV. Combining these results with previous collider and X-ray limits excludes 100% sterile-neutrino DM produced by strong neutrino self-coupling, mediated by a heavy (≳1 GeV) scalar; however, data permits sterile-neutrino DM production via a light mediator.
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Carpio, Jose Alonso, and Kohta Murase. "Simulating neutrino echoes induced by secret neutrino interactions." Journal of Cosmology and Astroparticle Physics 2023, no. 02 (February 1, 2023): 042. http://dx.doi.org/10.1088/1475-7516/2023/02/042.
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Abstract New neutrino interactions beyond the Standard Model (BSM) have been of much interest in not only particle physics but also cosmology and astroparticle physics. We numerically investigate the time delay distribution of astrophysical neutrinos that interact with the cosmic neutrino background. Using the Monte Carlo method, we develop a framework that enables us to simulate the time-dependent energy spectra of high-energy neutrinos that experience even multiple scatterings en route and to handle the sharp increase in the cross section at the resonance energy. As an example, we focus on the case of secret neutrino interactions with a scalar mediator. While we find the excellent agreement between analytical and simulation results for small optical depths, our simulations enable us to study optically thick cases that are not described by the simplest analytic estimates. Our simulations are used to understand effects of cosmological redshifts, neutrino spectra and flavors. The developments will be useful for probing BSM neutrino interactions with not only current neutrino detectors such as IceCube and Super-Kamiokande but also future neutrino detectors such as IceCube-Gen2 and Hyper-Kamiokande.
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Mazumdar, Arindam, Subhendra Mohanty, and Priyank Parashari. "Flavour specific neutrino self-interaction: H 0 tension and IceCube." Journal of Cosmology and Astroparticle Physics 2022, no. 10 (October 1, 2022): 011. http://dx.doi.org/10.1088/1475-7516/2022/10/011.
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Abstract Self-interaction in the active neutrinos is studied in the literature to alleviate the H_0 tension. Similar self-interaction can also explain the observed dips in the flux of the neutrinos coming from the distant astro-physical sources in IceCube detectors. In contrast to the flavour universal neutrino interaction considered for solving the H 0 tension, which is ruled out from particle physics experiments, we consider flavour specific neutrino interactions. We show that the values of self-interaction coupling constant and mediator mass required for explaining the IceCube dips are inconsistent with the strong neutrino self-interactions preferred by the combination of BAO, HST and Planck data. However, the required amount of self-interaction between tau neutrinos (ντ ) in inverted hierarchy for explaining IceCube dips is consistent with the moderate self-interaction region of cosmological bounds at 1-σ level. For the case of other interactions and hierarchies, the IceCube preferred amount of self-interaction is consistent with moderate self-interaction region of cosmological bounds at 2-σ level only.
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Kolbe, E., and T. S. Kosmas. "Recent highlights on neutrino-nucleus interactions." HNPS Proceedings 9 (February 11, 2020): 63. http://dx.doi.org/10.12681/hnps.2776.
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The recent developments on neutrino-nucleus interactions at low and intermediate energies are reviewed and discussed in conjunction with the recent data of atmospheric, solar, and accelerator neutrino experiments. The theoretical nuclear physics approaches used to interpret and predict phenomena for which neutrinos play a crucial role are also investigated. We emphasize on the implications of neutrino reactions and properties into the astrophysical phenomena and atmospheric neutrino problems.
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Papoulias, D. K., and T. S. Kosmas. "Nuclear study of the exotic neutrino interactions." HNPS Proceedings 22 (March 8, 2019): 79. http://dx.doi.org/10.12681/hnps.1934.
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Open neutrino physics issues require precision studies, both theoretical and experimental ones, and towards this aim coherent neutral current neutrino-nucleus scattering events are expected to be observed soon. In this work, we explore ν -nucleus processes from a nuclear theory point of view and obtain results with high confidence level based on accurate nuclear structure cross sections calculations. The present study explores the differential event rates as well as the total number of events expected to be measured by nuclear detectors, indicating measurable rates. We concentrate on the possibility of detecting supernova neutrinos by using massive detectors like those of the GERDA and SuperCDMS dark matter experiments and at spallation neutron source facilities (at Oak Ridge National Lab) by the COHERENT experiment.
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Mathews, G. J., L. Boccioli, J. Hidaka, and T. Kajino. "Review of uncertainties in the cosmic supernova relic neutrino background." Modern Physics Letters A 35, no. 25 (July 15, 2020): 2030011. http://dx.doi.org/10.1142/s0217732320300116.
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We review the computation of and associated uncertainties in the current understanding of the relic neutrino background due to core-collapse supernovae, black hole formation and neutron star merger events. We consider the current status of uncertainties due to the nuclear equation of state (EoS), the progenitor masses, the source supernova neutrino spectrum, the cosmological star formation rate, the stellar initial mass function, neutrino oscillations, and neutrino self-interactions. We summarize the current viability of future neutrino detectors to distinguish the nuclear EoS and the temperature of supernova neutrinos via the detected relic supernova neutrino spectrum.
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Roy Choudhury, Shouvik, Steen Hannestad, and Thomas Tram. "Massive neutrino self-interactions and inflation." Journal of Cosmology and Astroparticle Physics 2022, no. 10 (October 1, 2022): 018. http://dx.doi.org/10.1088/1475-7516/2022/10/018.
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Abstract Certain inflationary models like Natural inflation (NI) and Coleman-Weinberg inflation (CWI) are disfavoured by cosmological data in the standard ΛCDM+r model (where r is the scalar-to-tensor ratio), as these inflationary models predict the regions in the ns -r parameter space that are excluded by the cosmological data at more than 2σ (here ns is the scalar spectral index). The same is true for single field inflationary models with an inflection point that can account for all or majority of dark matter in the form of PBHs (primordial black holes). Cosmological models incorporating strongly self-interacting neutrinos (with a heavy mediator) are, however, known to prefer lower ns values compared to the ΛCDM model. Considering such neutrino self-interactions can, thus, open up the parameter space to accommodate the above inflationary models. In this work, we implement the massive neutrino self-interactions with a heavy mediator in two different ways: flavour-universal (among all three neutrinos), and flavour-specific (involving only one neutrino species). We implement the new interaction in both scalar and tensor perturbation equations of neutrinos. Interestingly, we find that the current cosmological data can support the aforementioned inflationary models at 2σ in the presence of such neutrino self-interactions.
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SCHWIENHORST, REINHARD. "COLLIDING NEUTRINO BEAMS." Modern Physics Letters A 23, no. 32 (October 20, 2008): 2751–61. http://dx.doi.org/10.1142/s0217732308028193.
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From several neutrino oscillation experiments, we understand now that neutrinos have mass. However, we really do not know what mechanism is responsible for producing this neutrino mass. Current or planned neutrino experiments utilize neutrino beams and long-baseline detectors to explore flavor mixing but do not address the question of the origin of neutrino mass. In order to begin answering that question, neutrino interactions need to be explored at much higher energies. This paper outlines a program to explore neutrinos and their interactions with various particles through a series of experiments involving colliding neutrino beams.
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Ascencio-Sosa, M., Z. Bagdasarian, J. F. Beacom, M. Bergevin, M. Breisch, G. Caceres Vera, S. Dazeley, et al. "Deployment of Water-based Liquid Scintillator in the Accelerator Neutrino Neutron Interaction Experiment." Journal of Instrumentation 19, no. 05 (May 1, 2024): P05070. http://dx.doi.org/10.1088/1748-0221/19/05/p05070.
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Abstract The Accelerator Neutrino Neutron Interaction Experiment (ANNIE) is a 26-ton water Cherenkov neutrino detector installed on the Booster Neutrino Beam (BNB) at Fermilab. Its main physics goals are to perform a measurement of the neutron yield from neutrino-nucleus interactions, as well as a measurement of the charged-current cross section of muon neutrinos. An equally important focus is the research and development of new detector technologies and target media. Specifically, water-based liquid scintillator (WbLS) is of interest as a novel detector medium, as it allows for the simultaneous detection of Cherenkov light and scintillation. This paper presents the deployment of a 366 L WbLS vessel in ANNIE in March 2023 and the subsequent detection of both Cherenkov light and scintillation from the WbLS. This proof-of-concept allows for the future development of reconstruction and particle identification algorithms in ANNIE, as well as dedicated analyses within the WbLS volume, such as the search for neutral-current events and the hadronic scintillation component.
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Choudhury, Shouvik Roy, Steen Hannestad, and Thomas Tram. "Massive neutrino self-interactions and the Hubble tension." Journal of Physics: Conference Series 2156, no. 1 (December 1, 2021): 012016. http://dx.doi.org/10.1088/1742-6596/2156/1/012016.
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Abstract We consider flavour independent neutrino self-interactions among massive neutrinos mediated by a heavy scalar against cosmological data. Such a model had previously shown to have potential in completely resolving the Hubble tension for the very strong interaction case with coupling strength ∼ 109 times the Fermi constant, by delaying the onset of neutrino free-streaming until matter-radiation equality. Our cosmological model consists of a total nine parameters which includes the six ACDM parameters and three parameters related to neutrinos: sum of neutrino masses (Σmν ), neutrino energy density (Neff ), and the effective coupling strength, log10 [GeffMeV2]. With the latest CMB data from the Planck 2018 data release as well as auxiliary data, we find that the region in parameter space with such strong interactions is still present in the posterior distribution. However, high-l polarisation data from the Planck 2018 release disfavours this strongly interacting mode even though it cannot yet be excluded. Our resuts show that the neutrino mass bounds obtained from cosmological data remain robust against when considering neutrino self-interactions. We also find that the high-l polarisation data also does not allow for high values of H 0 that can solve the current Hubble discrepancy, i.e. this model is not a viable solution to the same.
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Keränen, Petteri. "Testing exotic neutrino-neutrino interactions with AGN neutrinos." Physics Letters B 417, no. 3-4 (January 1998): 320–25. http://dx.doi.org/10.1016/s0370-2693(97)01405-6.
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Park, Jong-Chul, and Gaurav Tomar. "Probing non-standard neutrino interactions with interference: insights from dark matter and neutrino experiments." Journal of Cosmology and Astroparticle Physics 2023, no. 08 (August 1, 2023): 025. http://dx.doi.org/10.1088/1475-7516/2023/08/025.
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Abstract Neutrino-electron scattering experiments play a crucial role in investigating the non-standard interactions of neutrinos. In certain models, these interactions can include interference terms that may affect measurements. Next-generation direct detection experiments, designed primarily for dark-matter searches, are also getting sensitive to probe the neutrino properties. We utilise the data from XENONnT, a direct detection experiment, and Borexino, a low-energy solar neutrino experiment, to investigate the impact of interference on non-standard interactions. Our study considers models with an additional U(1) B-L , including U(1), U(1) L e - L µ , and U(1) L e - L τ , to investigate the impact of interference on non-standard neutrino interactions. We demonstrate that this interference can lead to a transition between the considered non-standard interaction models in the energy range relevant to both the XENONnT and Borexino experiments. This transition can be used to distinguish among the considered models if any signals are observed at direct detection or neutrino experiments. Our findings underscore the importance of accounting for the interference and incorporating both direct detection and solar neutrino experiments to gain a better understanding of neutrino interactions and properties.
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Katori, Teppei, Juan Pablo Yanez, and Tianlu Yuan. "Neutrino interaction physics in neutrino telescopes." European Physical Journal Special Topics 230, no. 24 (December 2021): 4293–308. http://dx.doi.org/10.1140/epjs/s11734-021-00292-w.
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AbstractNeutrino telescopes can observe neutrino interactions starting at GeV energies by sampling a small fraction of the Cherenkov radiation produced by charged secondary particles. These experiments instrument volumes massive enough to collect substantial samples of neutrinos up to the TeV scale as well as small samples at the PeV scale. This unique ability of neutrino telescopes has been exploited to study the properties of neutrino interactions across energies that cannot be accessed with man-made beams. Here, we present the methods and results obtained by IceCube, the most mature neutrino telescope in operation, and offer a glimpse of what the future holds in this field.
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Colombi, María Paula, Osvaldo Civitarese, and Ana V. Penacchioni. "Neutrino-pair interactions in astrophysical systems." International Journal of Modern Physics E 29, no. 09 (September 2020): 2050080. http://dx.doi.org/10.1142/s0218301320500809.
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We study the effects produced by interactions among neutrinos upon extra-galactic neutrino-fluxes. We have assumed a separable type of pair interactions and performed a transformation to a quasi-particle mean field followed by a Tamm–Damcoff diagonalization. In doing so, we have adopted techniques originated in the quantum many-body problem, and adapted them to this specific case. The solutions of the associated eigenvalue problem provide us with energies and amplitudes which are then used to construct the neutrino response functions at finite density and temperature. The formalism is applied to the description of neutrinos produced in a SN environment.
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Volpe, Maria Cristina. "Neutrinos : from the r-process to the diffuse supernova neutrino background." Journal of Physics: Conference Series 2156, no. 1 (December 1, 2021): 012126. http://dx.doi.org/10.1088/1742-6596/2156/1/012126.
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Abstract Neutrinos from dense environments are connected to the longstanding open questions of how massive stars explode and what are the sites where r-process elements are made. Flavor evolution and neutrino properties can influence nucleosynthetic abundances. GW170817 has given indirect evidence for r-process elements in binary neutron star mergers. We discuss the impact of non-standard interactions in such sites. Nearby compact objects, strong gravitational fields are present. We discuss their influence upon neutrino decoherence in a wave packet treatment of neutrino propagation. We conclude by mentioning the upcoming measurement of the diffuse supernova neutrino background.
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Hayato, Yoshinari, and Luke Pickering. "The NEUT neutrino interaction simulation program library." European Physical Journal Special Topics 230, no. 24 (October 11, 2021): 4469–81. http://dx.doi.org/10.1140/epjs/s11734-021-00287-7.
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Abstract is a neutrino–nucleus interaction simulation program library. It can be used to simulate interactions for neutrinos with between 100 MeV and a few TeV of energy. is also capable of simulating hadron interactions within a nucleus and is used to model nucleon decay and hadron–nucleus interactions for particle propagation in detector simulations. This article describes the range of interactions modelled and how each is implemented.
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Kisslinger, Leonard S. "Neutrino mass creation via quintessence field interaction." Modern Physics Letters A 34, no. 39 (December 19, 2019): 1950327. http://dx.doi.org/10.1142/s0217732319503279.
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Neutrino matter and the quintessence field interacting with a fermion field are added to a MSSM EW Lagrangian previously used to calculate the magnetic field created during the Electroweak Phase Transition (EWPT). Flavor neutrinos are linear combinations of neutrinos with a definite mass. We estimate the mass of neutrinos using the value of the quintessence field during the EWPT with a modification of parameters used in a previous work on Dark Matter–Dark Energy interactions for a weak neutrino interaction. The possibility that sterile neutrinos might be Dark Matter is briefly reviewed.
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Carpio, Jose Alonso, Ali Kheirandish, and Kohta Murase. "Time-delayed neutrino emission from supernovae as a probe of dark matter-neutrino interactions." Journal of Cosmology and Astroparticle Physics 2023, no. 04 (April 1, 2023): 019. http://dx.doi.org/10.1088/1475-7516/2023/04/019.
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Abstract Thermal MeV neutrino emission from core-collapse supernovae offers a unique opportunity to probe physics beyond the Standard Model in the neutrino sector. The next generation of neutrino experiments, such as DUNE and Hyper-Kamiokande, can detect 𝒪(103) and 𝒪(104) neutrinos in the event of a Galactic supernova, respectively. As supernova neutrinos propagate to Earth, they may interact with the local dark matter via hidden mediators and may be delayed with respect to the initial neutrino signal. We show that for sub-MeV dark matter, the presence of dark matter-neutrino interactions may lead to neutrino echoes with significant time delays. The absence or presence of this feature in the light curve of MeV neutrinos from a supernova allows us to probe parameter space that has not been explored by dark matter direct detection experiments.
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Miloi, Mădălina Mihaela. "The DsTau Experiment: A Study for Tau-Neutrino Production." Particles 3, no. 1 (March 1, 2020): 164–68. http://dx.doi.org/10.3390/particles3010013.
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For clarifying the validity of the Lepton Universality hypothesis, one of the fundamental statements of the Standard Model, the interaction cross section for all three flavors of leptons have to be known with high precision. In neutrino sector, for electron and muon neutrinos, the interaction cross section is known fairly well, but for tau neutrino only poor estimations exist. In particular, the most direct measurement by the DONuT experiment was performed with rather poor accuracy due to low statistics and an uncertainty of the tau neutrino flux. The DsTau experiment proposes to study tau-neutrino production process and thus to improve significantly the accuracy of calculations of tau neutrino flux for neutrino accelerator experiments. To study reactions providing most of tau neutrinos, the experiment uses a setup based on high resolution nuclear emulsions, capable to register short lived particle decays created in proton-nucleus interactions. The present report is an overview of the DsTau experiment together with some of the preliminary results from the pilot run.
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Banerjee, Indra Kumar, Ujjal Kumar Dey, Newton Nath, and Saadat Salman Shariff. "PTOLEMY's test of generalized neutrino interactions: unveiling challenges and constraints." Journal of Cosmology and Astroparticle Physics 2024, no. 04 (April 1, 2024): 002. http://dx.doi.org/10.1088/1475-7516/2024/04/002.
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Abstract Unanswered questions surrounding neutrinos have motivated investigations into physics beyond the standard model (SM) of particle physics. In particular, generalized neutrino interactions (GNI) provide a broader framework for studying these effects compared to the commonly studied non-standard neutrino interactions. These interactions are described by higher dimensional operators while maintaining the gauge symmetries of the SM. Furthermore, the cosmic neutrino background, a predicted component of the SM and standard cosmology, has yet to be directly detected. To shed light on this elusive phenomenon, we conduct a comprehensive analysis of the relevant GNI, specifically focusing on their implications for the proposed cosmic neutrino detector PTOLEMY. We make an attempt to see the capabilities and the limitations of PTOLEMY in sensing GNI while remaining optimistic regarding PTOLEMY's experimental resolution. These interactions play a significant role in modifying the electron spectrum resulting from the capture of cosmic neutrinos on radioactive tritium. This work also explores how the presence of these interactions influences the differential electron spectrum, taking into account factors such as finite experimental resolution, the mass of the lightest neutrino eigenstate, the strength of the interactions, and the ordering of neutrino mass.
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STAŚTO, ANNA M. "ULTRAHIGH ENERGY NEUTRINO PHYSICS." International Journal of Modern Physics A 19, no. 03 (January 30, 2004): 317–40. http://dx.doi.org/10.1142/s0217751x04017082.
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Ultrahigh energy neutrinos can provide important information about the distant astronomical objects and the origin of the Universe. Precise knowledge about neutrino interactions and production rates is essential for estimating background, expected fluxes and detection probabilities. In this paper we review the applications of the high energy QCD to the calculations of the interaction cross-sections of the neutrinos. We also study the production of the ultrahigh energy neutrinos in the atmosphere due to the charm and beauty decays.
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Akita, Kensuke, and Masahide Yamaguchi. "A Review of Neutrino Decoupling from the Early Universe to the Current Universe." Universe 8, no. 11 (October 25, 2022): 552. http://dx.doi.org/10.3390/universe8110552.
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We review the distortions of spectra of relic neutrinos due to the interactions with electrons, positrons, and neutrinos in the early universe. We solve integro-differential kinetic equations for the neutrino density matrix, including vacuum three-flavor neutrino oscillations, oscillations in electron and positron background, a collision term and finite temperature corrections to electron mass and electromagnetic plasma up to the next-to-leading order O(e3). After that, we estimate the effects of the spectral distortions in neutrino decoupling on the number density and energy density of the Cosmic Neutrino Background (CνB) in the current universe, and discuss the implications of these effects on the capture rates in direct detection of the CνB on tritium, with emphasis on the PTOLEMY-type experiment. In addition, we find a precise value of the effective number of neutrinos, Neff=3.044. However, QED corrections to weak interaction rates at order O(e2GF2) and forward scattering of neutrinos via their self-interactions have not been precisely taken into account in the whole literature so far. Recent studies suggest that these neglections might induce uncertainties of ±(10−3−10−4) in Neff.
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Pia, V. "Reconstruction of neutrino interactions in SAND with an innovative liquid Argon imaging detector." Journal of Instrumentation 19, no. 02 (February 1, 2024): C02073. http://dx.doi.org/10.1088/1748-0221/19/02/c02073.
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Abstract The Deep Underground Neutrino Experiment will be a next-generation neutrino oscillation long-baseline accelerator experiment with the aim of determining the still unknown neutrino oscillation parameters, observing proton decay and detecting supernova neutrinos exploiting a Liquid Argon Time Projection Chambers (LArTPC) of unprecedented size. However, despite their successful application in neutrino and DM experiments, the performances of LArTPCs are limited in high intensity environments, such as in near-site detectors on neutrino beams, due to the long drift time needed to collect the ionisation charge. The design of SAND at the DUNE Near Detector complex includes a 1-ton LAr target -GRAIN (Granular Argon for Interaction of Neutrinos)- designed to overcome such limitation by imaging the scintillation light produced in neutrino interactions. By capturing “pictures” of the LAr (or LXe), GRAIN will allow to reconstruct the event topologies and energy deposition. Using this information, and that provided by the SAND electromagnetic calorimeter and target tracker system, SAND will allow on-axis beam monitoring, the control of systematics uncertainties for the oscillation analysis, precision measurements of neutrino cross-sections, and beyond Standard Model searches.
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ATHAR, H., C. S. KIM, and JAKE LEE. "INTRINSIC AND OSCILLATED ASTROPHYSICAL NEUTRINO FLAVOR RATIOS REVISITED." Modern Physics Letters A 21, no. 13 (April 30, 2006): 1049–65. http://dx.doi.org/10.1142/s021773230602038x.
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The pp interactions taking place in the cosmos around us are a source of the astrophysical neutrinos of all the three flavors. In these interactions, the electron and the muon neutrinos mainly come from the production and the decay of the π± mesons, whereas the tau neutrinos mainly come from the production and the decay of the [Formula: see text] mesons. We estimate the three intrinsic neutrino flavor ratios for 1 GeV ≤E≤1012 GeV in the pp interactions and found them to be 1:2:3×10-5. We study the effects of neutrino oscillations on these intrinsic ratios. We point out that the three ratios become 1:1:1 if L (pc)/E(GeV) ≥10-10 in the presence of neutrino oscillations, where L is the distance to the astrophysical neutrino source in units of parsecs.
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Ogawa, Hiroshi. "Search for exotic neutrino-electron interactions using solar neutrinos in XMASS-I." Journal of Physics: Conference Series 2156, no. 1 (December 1, 2021): 012136. http://dx.doi.org/10.1088/1742-6596/2156/1/012136.
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Abstract In recent years, the larger size and lower background of dark matter search detectors have opened up a new frontier of searching for new physics other than dark matter using these detectors. One of them is the search for new properties of neutrinos by observing the interaction of neutrinos at low energy. XMASS is a multi-purpose experiment using xenon exclusively in ites liquid xenon (LXe) and is located at the Kamioka Observatory in Japan. We searched for exotic neutrino-electron interactions that could be produced by either a neutrino millicharge, a neutrino magnetic moment, or by dark photons, which might affect the intearction cross section of solar neutrinos in XMASS. We analyzed data taken between November 2013 and March 2016 amounting to 711 live days. No significant signal has been found above the predicted background level in detector. We obtained an upper limit for neutrino millicharge of 5.4 × 10–11e for all flavors of neutrino. We also set individual flavors limits for υμ and ν τ, which are the best limits obtained by direct detection. We also obtain an upper limit for the neutrino magnetic moment of 1.8× 10–10μ B . In addition, we obtain upper limits for the coupling constant of dark photons in the U(1) B–L model. This result almost excludes the possibility to understand the muon g — 2 anomaly by dark photons.
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Sridhar, Navin, Brian D. Metzger, and Ke Fang. "High-energy Neutrinos from Gamma-Ray-faint Accretion-powered Hypernebulae." Astrophysical Journal 960, no. 1 (December 27, 2023): 74. http://dx.doi.org/10.3847/1538-4357/ad03e8.
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Abstract Hypernebulae are inflated by accretion-powered winds accompanying hyper-Eddington mass transfer from an evolved post-main-sequence star onto a black hole or neutron star companion. The ions accelerated at the termination shock—where the collimated fast disk winds and/or jet collide with the slower, wide-angled wind-fed shell—can generate high-energy neutrinos via hadronic proton–proton reactions, and photohadronic (p γ) interactions with the disk thermal and Comptonized nonthermal background photons. It has been suggested that some fast radio bursts (FRBs) may be powered by such short-lived jetted hyper-accreting engines. Although neutrino emission associated with the millisecond duration bursts themselves is challenging to detect, the persistent radio counterparts of some FRB sources—if associated with hypernebulae—could contribute to the high-energy neutrino diffuse background flux. If the hypernebula birth rate follows that of stellar-merger transients and common envelope events, we find that their volume-integrated neutrino emission—depending on the population-averaged mass-transfer rates—could explain up to ∼25% of the high-energy diffuse neutrino flux observed by the IceCube Observatory and the Baikal Gigaton Volume Detector Telescope. The time-averaged neutrino spectrum from hypernebula—depending on the population parameters—can also reproduce the observed diffuse neutrino spectrum. The neutrino emission could in some cases furthermore extend to >100 PeV, detectable by future ultra-high-energy neutrino observatories. The large optical depth through the nebula to Breit–Wheeler (γ γ) interaction attenuates the escape of GeV–PeV gamma rays coproduced with the neutrinos, rendering these gamma-ray-faint neutrino sources, consistent with the Fermi observations of the isotropic gamma-ray background.
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GUPTA, NAYANTARA, and D. P. BHATTACHARYYA. "INVESTIGATION ON THE NEUTRINO INDUCED MUONS FROM ACTIVE GALACTIC NUCLEI." Modern Physics Letters A 15, no. 25 (August 20, 2000): 1567–76. http://dx.doi.org/10.1142/s0217732300001742.
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The fluxes of neutrino induced muons at different zenith angles have been calculated using the high energy diffused neutrino spectra emitted from blazars. We have used the standard formulation developed by Gaisser based on charge-current interactions in rock and the QED-based energy loss formulation to estimate the spectra of neutrino induced muons. The energy spectra of neutrino flux generated from blazars has been taken from the model calculations of Protheroe. The latest charge-current and total interaction cross-sections at ultrahigh energies from Kwiecinski et al. have been used to find the probability of muon generation from neutrinos and the loss of neutrinos during propagation through the Earth. We find that our derived horizontal neutrino induced muon energy spectra expected from blazar model of Protheroe is comparable with the upper limits as predicted by SOUDAN 2 experiment.
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Garg, Diksha, Sameer Patel, Mary Hall Reno, Alexander Reustle, Yosui Akaike, Luis A. Anchordoqui, Douglas R. Bergman, et al. "Neutrino propagation in the Earth and emerging charged leptons with nuPyProp." Journal of Cosmology and Astroparticle Physics 2023, no. 01 (January 1, 2023): 041. http://dx.doi.org/10.1088/1475-7516/2023/01/041.
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Abstract Ultra-high-energy neutrinos serve as messengers of some of the highest energy astrophysical environments. Given that neutrinos are neutral and only interact via weak interactions, neutrinos can emerge from sources, traverse astronomical distances, and point back to their origins. Their weak interactions require large target volumes for neutrino detection. Using the Earth as a neutrino converter, terrestrial, sub-orbital, and satellite-based instruments are able to detect signals of neutrino-induced extensive air showers. In this paper, we describe the software code nuPyProp that simulates tau neutrino and muon neutrino interactions in the Earth and predicts the spectrum of the τ-leptons and muons that emerge. The nuPyProp outputs are lookup tables of charged lepton exit probabilities and energies that can be used directly or as inputs to the nuSpaceSim code designed to simulate optical and radio signals from extensive air showers induced by the emerging charged leptons. We describe the inputs to the code, demonstrate its flexibility and show selected results for τ-lepton and muon exit probabilities and energy distributions. The nuPyProp code is open source, available on github.
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Chauhan, Bhavesh, Basudeb Dasgupta, and Vivek Datar. "A deuterated liquid scintillator for supernova neutrino detection." Journal of Cosmology and Astroparticle Physics 2021, no. 11 (November 1, 2021): 005. http://dx.doi.org/10.1088/1475-7516/2021/11/005.
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Abstract For the next galactic supernova, operational neutrino telescopes will measure the neutrino flux several hours before their optical counterparts. Existing detectors, relying mostly on charged current interactions, are mostly sensitive to ν̅e and to a lesser extent to νe . In order to measure the flux of other flavors (νμ ,ν̅μ ,ντ ,and ν̅τ ), we need to observe their neutral current interactions with the detector. Such a measurement is not only crucial for overall normalization of the supernova neutrino flux but also for understanding the intricate neutrino oscillation physics. A deuterium based detector will be sensitive to all neutrino flavors. In this paper, we propose a 1 kton deuterated liquid scintillator (DLS) based detector that will see about 435 neutral current events and 170 (108) charged current νe (ν̅e ) events from a fiducial supernova at a distance of 10 kpc from Earth. We explore the possibility of extracting spectral information from the neutral current channel by measuring the quenched kinetic energy of the proton in the final state, where the neutron in the final state is tagged and used to reduce backgrounds. We also discuss the secondary interactions of the recoil neutrons in the detector.
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BINGHAM, R., L. O. SILVA, J. T. MENDONCA, P. K. SHUKLA, W. B. MORI, and A. SERBETO. "PLASMA WAKES DRIVEN BY NEUTRINOS, PHOTONS AND ELECTRON BEAMS." International Journal of Modern Physics B 21, no. 03n04 (February 10, 2007): 343–50. http://dx.doi.org/10.1142/s0217979207042112.
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There is considerable interest in the propagation dynamics of intense electron and photon neutrino beams in a background dispersive medium such as dense plasmas, particularly in the search for a mechanism to explain the dynamics of type II supernovae. Neutrino interactions with matter are usually considered as single particle interactions. All the single particle mechanisms describing the dynamical properties of neutrino's in matter are analogous with the processes involving single electron interactions with a medium such as Compton scattering, and Cerenkov radiation etc. However, it is well known that beams of electrons moving through a plasma give rise to a new class of processes known as collective interactions such as two stream instabilities which result in either the absorption or generation of plasma waves. Intense photon beams also drive collective interactions such as modulational type instabilities. In both cases relativistic electron beams of electrons and photon beams can drive plasma wakefields in plasmas. Employing the relativistic kinetic equations for neutrinos interacting with dense plasmas via the weak force we explore collective plasma streaming instabilities driven by Neutrino electron and photon beams and demonstrate that all three types of particles can drive wakefields.
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Jean-Jacques, Kendra, Anna Roland, Christelle Billan, and Preet Sharma. "A Review on Neutrino Oscillation Probabilities and Sterile Neutrinos." Emerging Science Journal 6, no. 2 (March 9, 2022): 418–28. http://dx.doi.org/10.28991/esj-2022-06-02-015.
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In the past decades, there have been many groundbreaking discoveries and advancements in the field of particle physics. One of the important elementary breakthroughs is the phenomenology of neutrino oscillations. This includes the properties of neutrinos in the Standard Model (SM) and how neutrino oscillations and their properties have been so important in strengthening the SM. Neutrino oscillations also play a vital role in understanding the current nature of our Universe and the way it behaves. There is also a great interest in neutrino oscillations and their connection with dark matter. In this review, we start with the introduction and discuss the theoretical background of neutrino oscillations and some experiments, which are working to detect the properties of neutrinos. Then the fundamentals of neutrino oscillations and their interactions were described. Since there are multiple sources of neutrinos, we have described the three sectors through which we can expect neutrinos to be produced. These are the atmospheric, solar, and reactor sectors. A brief section on the important milestones in neutrino oscillations is included because of the experiments and what they use to detect neutrino properties. Finally, we also include a section on sterile neutrinos since they have been under study for a long time and there is a possibility of them being connected to dark matter interactions. Doi: 10.28991/ESJ-2022-06-02-015 Full Text: PDF
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Chichiri, Carlos, Graciela B. Gelmini, Philip Lu, and Volodymyr Takhistov. "Cosmological dependence of sterile neutrino dark matter with self-interacting neutrinos." Journal of Cosmology and Astroparticle Physics 2022, no. 09 (September 1, 2022): 036. http://dx.doi.org/10.1088/1475-7516/2022/09/036.
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Abstract Unexplored interactions of neutrinos could be the key to understanding the nature of the dark matter (DM). In particular, active neutrinos with new self-interactions can produce keV-mass sterile neutrinos that account for the whole of the DM through the Dodelson-Widrow mechanism for a large range of active-sterile mixing values. This production typically occurs before Big-Bang Nucleosynthesis (BBN) in a yet uncharted era of the Universe. We assess how the mixing range for keV-mass sterile neutrino DM is affected by the uncertainty in the early Universe pre-BBN cosmology. This is particularly relevant for identifying the viable parameter space of sterile neutrino searches allowed by all astrophysical limits, as well as for cosmology, since the detection of a sterile neutrino could constitute the first observation of a particle providing information about the pre-BBN epoch. We find that the combined uncertainties in the early Universe cosmology and neutrino interactions significantly expand the allowed parameter space for sterile neutrinos that can constitute the whole of the DM.
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Klein, Spencer. "High-energy neutrino interaction physics with IceCube." EPJ Web of Conferences 208 (2019): 09001. http://dx.doi.org/10.1051/epjconf/201920809001.
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Although they are best known for studying astrophysical neutrinos, neutrino telescopes like IceCube can study neutrino interactions, at energies far above those that are accessible at accelerators. In this writeup, I present two IceCube analyses of neutrino interactions at energies far above 1 TeV. The first measures neutrino absorption in the Earth, and, from that determines the neutrino-nucleon cross-section at energies between 6.3 and 980 TeV. We find that the cross-sections are 1.30 +0.21 -0.19 (stat.) +0.39 -0.43 (syst.) times the Standard Model crosssection. We also present a measurement of neutrino inelasticity, using νμ charged-current interactions that occur within IceCube. We have measured the average inelasticity at energies from 1 TeV to above 100 TeV, and found that it is in agreement with the Standard Model expectations. We have also performed a series of fits to this track sample and a matching cascade sample, to probe aspects of the astrophysical neutrino flux, particularly the flavor ratio.
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Sato, Toshiki, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, and Brian J. Williams. "Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova." Astrophysical Journal 954, no. 2 (August 28, 2023): 112. http://dx.doi.org/10.3847/1538-4357/ace7c1.
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Abstract Neutrino interactions with stellar material are widely believed to be fundamental to the explosion of massive stars. However, this important process has remained difficult to confirm observationally. We propose a new method to verify it using X-ray observations of the supernova remnant Cassiopeia A. The elemental composition in its Fe-rich ejecta that could have been produced at the innermost region of the supernova, where neutrinos are expected to interact, allows us to examine the presence of neutrino interactions. Here we demonstrate that the amount of Mn produced without neutrino nucleosynthesis processes (i.e., the ν- and νp-processes) is too small to explain the Mn/Fe mass ratio we measure (0.14%–0.67%). This result supports the operation of significant neutrino interactions in the Cassiopeia A supernova. If the observed Mn/Fe mass ratio purely reflects the production at the innermost region of the supernova, this would be the first robust confirmation of neutrino–matter interactions in an individual supernova. We further show that the Mn/Fe mass ratio has the potential to constrain supernova neutrino parameters (i.e., total neutrino luminosity, neutrino temperature). Future spatially resolved, high-resolution X-ray spectroscopy will allow us to investigate the details of neutrino–supernova astrophysics through its signatures in elemental composition not only in Cassiopeia A but also in other remnants.
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Morales, G., and N. Fraija. "Neutrino propagation in winds around the central engine of sGRB." Monthly Notices of the Royal Astronomical Society 505, no. 4 (May 31, 2021): 4968–80. http://dx.doi.org/10.1093/mnras/stab1577.
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ABSTRACT Since neutrinos can escape from dense regions without being deflected, they are promising candidates to study the new physics at the sources that produce them. With the increasing development of more sensitive detectors in the coming years, we will infer several intrinsic properties from incident neutrinos. In particular, we centralize our study in those produced by thermal processes in short gamma-ray bursts (sGRBs) and their interactions within the central engine’s anisotropic medium. On the one hand, we consider baryonic winds produced with a strong magnetic contribution, and on the other hand, we treat only neutrino-driven winds. First, we obtain the effective neutrino potential considering both baryonic density profiles around the central engine. Then, we get the three-flavour oscillation probabilities in this medium to finally calculate the expected neutrino ratios. We find a stronger angular dependence on the expected neutrino ratios, which, incidentally, contrast from the expected theoretical ratios without considering the winds’ additional contribution. The joint analysis of this observable, together with the sGRB ejected jet angle, might lead to an effective mechanism to discriminate between the involved merger progenitors (black hole-neutron star (BH-NS) or neutron-star neutron-star(NS-NS)), acting as an additional detection channel to gravitational waves.
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Sen, Manibrata. "Sterile neutrino dark matter, neutrino secret self-interactions and extra radiation." Journal of Physics: Conference Series 2156, no. 1 (December 1, 2021): 012018. http://dx.doi.org/10.1088/1742-6596/2156/1/012018.
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Abstract keV scale sterile neutrinos are excellent warm dark matter candidates. In the early Universe, these can be produced from oscillations and scatterings of active neutrinos. However, in the absence of any new physics, this mechanism is in severe tension with observations from X-ray searches. In this work, we show that secret self-interactions of active neutrinos, mediated by a scalar, can efficiently produce these sterile neutrinos without being ruled out by X-ray observations. These neutrino self-interactions are also testable: for a mediator mass greater than a few MeV, these self-interactions can give signatures in laboratory based experiments, while for lighter mediators, there will be observable consequences for upcoming cosmology probes.1
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McFarland, K. S. "Neutrino Interactions." Nuclear Physics B - Proceedings Supplements 235-236 (February 2013): 143–48. http://dx.doi.org/10.1016/j.nuclphysbps.2013.04.004.
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Panman, J. "Neutrino interactions." Nuclear Physics B - Proceedings Supplements 3 (March 1988): 553–80. http://dx.doi.org/10.1016/0920-5632(88)90202-2.
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RAJPOOT, SUBHASH. "A MODEL FOR SIMPSON’S 17 keV NEUTRINO." International Journal of Modern Physics A 07, no. 18 (July 20, 1992): 4441–48. http://dx.doi.org/10.1142/s0217751x92001988.
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Recent studies of β-decay spectra seem to confirm Simpson’s earlier findings that the electron neutrinos contain a small (1%) admixture of a 17 keV Dirac neutrino. An unconventional model with SU(2)L×SU(2)R×U(1)B−1 gauge interactions is presented in which all neutrinos are Dirac particles. Electron and muon neutrinos acquire seesaw Dirac masses of order 10−3eV for the MSW solution for the solar neutrino problem. The τ neutrino is identified as Simpson’s 17 keV neutrino. Constraints coming from cosmology and particle physics are shown to be satisfied.
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Domi, Alba, Simon Bourret, and Liam Quinn. "Particle Physics with ORCA." EPJ Web of Conferences 207 (2019): 04003. http://dx.doi.org/10.1051/epjconf/201920704003.
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KM3NeT is a Megaton-scale neutrino telescope currently under construction at the bottom of the Mediterranean Sea. When completed, it will consist of two separate detectors: ARCA (Astroparticle Research with Cosmics in the Abyss), optimised for high-energy neutrino astronomy, and ORCA (Oscillation Research with Cosmics in the Abyss) for neutrino oscillation studies of atmospheric neutrinos. The main goal of ORCA is the determination of the neutrino mass ordering (NMO). Nevertheless it is possible to exploit ORCA’s configuration to make other important measurements, such as sterile neutrinos, non standard interactions, tau-neutrino appearance, neutrinos from Supernovae, Dark Matter and Earth Tomography studies. Part of these analyses are summarized here.
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Farnese, Christian. "Atmospheric Neutrino Search in the ICARUS T600 Detector." Universe 5, no. 1 (January 9, 2019): 17. http://dx.doi.org/10.3390/universe5010017.
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The 760-ton liquid argon ICARUS T600 detector performed a successful three-year physics run at the underground LNGS laboratories, studying in particular neutrino oscillations with the CNGS neutrino beam from CERN. This detector has been moved in 2017 to Fermilab after a significant overhauling and will be exposed soon to the Booster Neutrino Beam acting as the far station to search for sterile neutrinos within the SBN program. The contribution addresses the developed methods and the results of an analysis to identify and reconstruct atmospheric neutrino interactions collected by ICARUS T600 in the underground run at LNGS. Despite the limited statistics, this search demonstrates the excellent quality of the detector reconstruction and the feasibility of an automatic search for the electron neutrino CC interactions in the sub-GeV range, as required for the study of the BNB neutrinos at FNAL.
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CURRAT, CHARLES A. "Measuring Cosmic Ray and Atmospheric Neutrinos in the Sudbury Neutrino Observatory." International Journal of Modern Physics A 20, no. 14 (June 10, 2005): 3106–9. http://dx.doi.org/10.1142/s0217751x05025863.
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High energy muons and neutrinos are produced by the interaction of primary cosmic rays in the Earth's upper atmosphere. These primary interactions produce mesons that decay into muons and neutrinos. SNO is in a unique position amongst underground experiments in the world. At the depth of over 6 km water equivalent, it is the deepest underground laboratory currently in operation. SNO can make a number of novel measurements using muons. First, SNO is sensitive to the downward muon rate coming from primary cosmic ray interactions. Second, SNO's great depth makes possible the detection of atmospheric neutrinos (via the detection of neutrino induced muons) from the nadir to inclinations as large as cos (θ zenith ) ≃ 0.4 above the horizon. Although SNO is a modest-size Cherenkov detector, SNO's unique niche allows it to make important model-independent checks of atmospheric neutrino oscillations.
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Aksenov, Alexey G. "A Multidimensional Multicomponent Gas Dynamic with the Neutrino Transfer in Gravitational Collapse." Universe 8, no. 7 (July 7, 2022): 372. http://dx.doi.org/10.3390/universe8070372.
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The self-consistent problem of gravitational collapse is solved using 2D gas dynamics with taking into account the neutrino transfer in the flux-limited diffusion approximation. Neutrino are described by spectral energy density, and weak interaction includes a simplified physical model of neutrino interactions with nucleons. I investigate convection on the stage of the collapse and then in the center of the core, where the unstable entropy profile was probably formed. It is shown that convection has large scale. Convection appears only in the semitransparent region near the neutrinosphere due to non-equilibrium nonreversible neutronization. Convection increases the energy of emitted neutrino up to 15÷18 MeV. The obtained neutrino spectrum is important for the registration of low-energy neutrinos from a supernova.
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Kumano, Shunzo. "High-energy neutrino-nucleus interactions." EPJ Web of Conferences 208 (2019): 07003. http://dx.doi.org/10.1051/epjconf/201920807003.
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High-energy neutrino-nucleus interactions are discussed by considering neutrino-oscillation experiments and ultra-high-energy cosmic neutrino interactions. The largest systematic error for the current neutrino oscillation measurements comes from the neutrino-nucleus interaction part, and its accurate understanding is essential for high-precision neutrino physics, namely for studying CP violation in the lepton sector. Depending on neutrino beam energies, quasi-elastic, resonance, Regge, or/and deep inelastic scattering (DIS) processes contribute to the neutrino cross section. It is desirable to have a code to calculate the neutrino-nucleus cross section in any kinematical range by combining various theoretical descriptions. On the other hand, the IceCube collaboration started obtaining cross section data up to the 1015 eV range, so that it became necessary to understand ultra-high-energy neutrino interactions beyond the artificial lepton-accelerator energy range. For future precise neutrino physics including the CP measurement, it is also necessary to understand accurate nuclear corrections. The current status is explained for nuclear corrections in DIS structure functions. The possibility is also discussed to find gravitational sources within nucleons and nuclei, namely matrix elements of quark-gluon energy-momentum tensor. They could be probed by neutrino interactions without replying on direct ultra-weak “gravitational interactions” with high-intensity neutrino beams, possibly at a future neutrino factory, by using techniques of hadron tomography.