Relevant bibliographies by topics / Radiative Emission of Neutrino Pair

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Academic literature on the topic 'Radiative Emission of Neutrino Pair'

Author: Grafiati
Published: 14 March 2023

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Journal articles on the topic "Radiative Emission of Neutrino Pair"

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Jentschura, Ulrich D., and István Nándori. "Neutrino Pair Cerenkov Radiation for Tachyonic Neutrinos." Advances in High Energy Physics 2017 (2017): 1–8. http://dx.doi.org/10.1155/2017/9850312.

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The emission of a charged light lepton pair by a superluminal neutrino has been identified as a major factor in the energy loss of highly energetic neutrinos. The observation of PeV neutrinos by IceCube implies their stability against lepton pair Cerenkov radiation. Under the assumption of a Lorentz-violating dispersion relation for highly energetic superluminal neutrinos, one may thus constrain the Lorentz-violating parameters. A kinematically different situation arises when one assumes a Lorentz-covariant, space-like dispersion relation for hypothetical tachyonic neutrinos, as an alternative to Lorentz-violating theories. We here discuss a hitherto neglected decay process, where a highly energetic tachyonic neutrino may emit other (space-like, tachyonic) neutrino pairs. We find that the space-like dispersion relation implies the absence of a q2 threshold for the production of a tachyonic neutrino-antineutrino pair, thus leading to the dominant additional energy loss mechanism for an oncoming tachyonic neutrino in the medium-energy domain. Surprisingly, the small absolute values of the decay rate and energy loss rate in the tachyonic model imply that these models, in contrast to the Lorentz-violating theories, are not pressured by the cosmic PeV neutrinos registered by the IceCube collaboration.
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Yoshimura, M., N. Sasao, and M. Tanaka. "Radiative emission of neutrino pair free of quantum electrodynamic backgrounds." Progress of Theoretical and Experimental Physics 2015, no. 5 (May 19, 2015): 53B06–0. http://dx.doi.org/10.1093/ptep/ptv064.

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Yoshimura, M., A. Fukumi, N. Sasao, and T. Yamaguchi. "Parity Violating Observables in Radiative Neutrino Pair Emission from Metastable Atoms." Progress of Theoretical Physics 123, no. 3 (March 1, 2010): 523–32. http://dx.doi.org/10.1143/ptp.123.523.

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Dinh, D. N., and S. T. Petcov. "Radiative emission of neutrino pairs in atoms and light sterile neutrinos." Physics Letters B 742 (March 2015): 107–16. http://dx.doi.org/10.1016/j.physletb.2015.01.020.

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Jentschura, U. D., I. Nándori, and G. Somogyi. "Lorentz breaking and SU(2)L × U(1)Y gauge invariance for neutrinos." International Journal of Modern Physics E 28, no. 09 (September 2019): 1950072. http://dx.doi.org/10.1142/s0218301319500721.

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Conceivable Lorentz-violating effects in the neutrino sector remain a research area of great general interest, as they touch upon the very foundations on which the Standard Model and our general understanding of fundamental interactions are laid. Here, we investigate the relation of Lorentz violation in the neutrino sector in light of the fact that neutrinos and the corresponding left-handed charged leptons form [Formula: see text] doublets under the electroweak gauge group. Lorentz-violating effects thus cannot be fully separated from questions related to gauge invariance. The model dependence of the effective interaction Lagrangians used in various recent investigations is explored with a special emphasis on neutrino splitting, otherwise known as the neutrino-pair Cerenkov radiation and vacuum-pair emission (electron–positron-pair Cerenkov radiation). We highlight two scenarios in which Lorentz-violating effects do not necessarily also break electroweak gauge invariance. The first of these involves a restricted set of gauge transformations, a subgroup of [Formula: see text], while in the second where differential Lorentz violation is exclusively introduced by the mixing of the neutrino flavor and mass eigenstates. Our study culminates in a model which fully preserves [Formula: see text] gauge invariance, involves flavor-dependent Lorentz-breaking parameters, and still allows for Cerenkov-type decays to proceed.
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Drewes, Marco, Jamie McDonald, Loïc Sablon, and Edoardo Vitagliano. "Neutrino Emissivities as a Probe of the Internal Magnetic Fields of White Dwarfs." Astrophysical Journal 934, no. 2 (July 28, 2022): 99. http://dx.doi.org/10.3847/1538-4357/ac7874.

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Abstract The evolution of white dwarfs (WDs) depends crucially on thermal processes. The plasma in their core can produce neutrinos that escape from the star, thus contributing to the energy loss. While in the absence of a magnetic field the main cooling mechanism is plasmon decay at high temperature and photon surface emission at low temperature, a large magnetic field in the core hiding beneath the surface even of ordinary WDs, and undetectable to spectropolarimetric measurements, could potentially leave an imprint in the cooling. In this paper, we revisit the contribution to WD cooling stemming from neutrino pair synchrotron radiation and the effects of the magnetic field on plasmon decay. Our key finding is that even if observations limit the magnetic field strength at the stellar surface, magnetic fields in the interior of WDs—with or without a surface magnetic field—can be strong enough to modify the cooling rate, with neutrino pair synchrotron emission being the most important contribution. This effect may not only be relevant for the quantification and interpretation of cooling anomalies, but suggests that the internal magnetic fields of WDs should be smaller than ∼ 6 × 1011 G, slightly improving bounds coming from a stability requirement. While our simplified treatment of the WD structure implies that further studies are needed to reduce the systematic uncertainties, the estimates based on comparing the emissivities illustrate the potential of neutrino emission as a diagnostic tool to study the interior of WDs.
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Crinquand, B., B. Cerutti, and G. Dubus. "Kinetic modeling of the electromagnetic precursor from an axisymmetric binary pulsar coalescence." Astronomy & Astrophysics 622 (February 2019): A161. http://dx.doi.org/10.1051/0004-6361/201834610.

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Context. The recent detection of gravitational waves associated with a binary neutron star merger revives interest in interacting pulsar magnetospheres. Current models predict that a significant amount of magnetic energy should be released prior to the merger, leading to electromagnetic precursor emission. Aims. In this paper, we revisit this problem in the light of the recent progress in kinetic modeling of pulsar magnetospheres. We limit our work to the case of aligned magnetic moments and rotation axes, and thus neglect the orbital motion. Methods. We perform global two-dimensional axisymmetric particle-in-cell simulations of two pulsar magnetospheres merging at a rate consistent with the emission of gravitational waves. Both symmetric and asymmetric systems are investigated. Results. Simulations show a significant enhancement of magnetic dissipation within the magnetospheres as the two stars approach one another. Even though the magnetospheric configuration depends on the relative orientations of the pulsar spins and magnetic axes, all configurations present nearly the same radiative signature, indicating that a common dissipation mechanism is at work. The relative motion of both pulsars drives magnetic reconnection at the boundary between the two magnetospheres, leading to efficient particle acceleration and high-energy synchrotron emission. Polar-cap discharge is also strongly enhanced in asymmetric configurations, resulting in vigorous pair production and potentially additional high-energy radiation. Conclusions. We observe an increase in the pulsar radiative efficiency by two orders of magnitude over the last orbit before the merger, exceeding the spindown power of an isolated pulsar. The expected signal is too weak to be detected at high energies even in the nearby universe. However, if a small fraction of this energy is channeled into radio waves, it could be observed as a non-repeating fast radio burst.
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Florou, Ioulia, Maria Petropoulou, and Apostolos Mastichiadis. "A marginally fast-cooling proton–synchrotron model for prompt GRBs." Monthly Notices of the Royal Astronomical Society 505, no. 1 (May 7, 2021): 1367–81. http://dx.doi.org/10.1093/mnras/stab1285.

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ABSTRACT A small fraction of gamma-ray bursts (GRBs) with available data down to soft X-rays (∼0.5 keV) has been shown to feature a spectral break in the low-energy part (∼1–10 keV) of their prompt emission spectrum. The overall spectral shape is consistent with optically thin synchrotron emission from a population of particles that have cooled on a time-scale comparable to the dynamic time to energies that are still much higher than their rest-mass energy (marginally fast cooling regime). We consider a hadronic scenario and investigate if the prompt emission of these GRBs can originate from relativistic protons that radiate synchrotron in the marginally fast cooling regime. Using semi-analytical methods, we derive the source parameters, such as magnetic field strength and proton luminosity, and calculate the high-energy neutrino emission expected in this scenario. We also investigate how the emission of secondary pairs produced by photopion interactions and γγ pair production affect the broad-band photon spectrum. We support our findings with detailed numerical calculations. Strong modification of the photon spectrum below the break energy due to the synchrotron emission of secondary pairs is found, unless the bulk Lorentz factor is very large (Γ ≳ 103). Moreover, this scenario predicts unreasonably high Poynting luminosities because of the strong magnetic fields (106–107 G) that are necessary for the incomplete proton cooling. Our results strongly disfavour marginally fast cooling protons as an explanation of the low-energy spectral break in the prompt GRB spectra.
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Hirotani, K. "Gamma-ray Emission from Pulsar Outer Magnetospheres." Symposium - International Astronomical Union 195 (2000): 171–80. http://dx.doi.org/10.1017/s0074180900162904.

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We study the γ-ray emission from an outer-gap accelerator around a rotating neutron star. Assuming the existence of global currents in the magnetosphere, the charge depletion causes a large electric field along the magnetic field lines. This electric field accelerates migratory electrons and positrons which radiate gamma-rays via curvature radiation. These gamma-rays, in turn, produce yet more radiating particles by colliding with the X-rays, leading to a pair-production cascade. Imposing a gap-closure condition that a single pair produces one pair in the gap, on average, we explicitly solve the strength of the acceleration field and demonstrate how the peak energy and the luminosity of the curvature-radiated GeV photons and the cutoff energy and luminosity of Compton-scattered TeV photons depend on such parameters as the surface temperature, the rotational frequency, and the magnetic moment. It is demonstrated that both the GeV and TeV emissions of Geminga will be harder than those of B1055-52, B0656+14, and Vela, and that the TeV fluxes are too small to be observed by current ground-based telescopes.
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Itoh, Naoki. "Neutrino Emission Processes in the Weinberg-Salam Theory." International Astronomical Union Colloquium 108 (1988): 434–35. http://dx.doi.org/10.1017/s025292110009429x.

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The neutrino emission processes play essential roles in stellar evolution as expemplified by the observations of the neutrinos from SN 1987a by the KAMIOKANDE-II and IMB experiments. Recently a very extensive study of the various neutrino emission processes based on the Weinberg-Salam theory has been completed by the present author and his collaborators. The neutrino emission processes calculated by the author’s group include pair, photo-, plasma, and bremsstrahlung neutrino processes. The neutrino energy loss rates due to pair, photo-, and plasma processes in the framework of the Weinberg-Salam theory are found to be substantially lower than the result obtained by Beaudet, Petrosian, and Salpeter. The reduction factor α is in the range 0.35 < α < 0.88 depending on the neutrino masses, density, and temperature. The ionic correlation effects play important roles in the bremsstrahlung neutrino process. The present author and his collaborators recently calculated the bremsstrahlung neutrino energy loss rate taking into account the ionic correlation effects in the crystalline lattice state as well as in the liquid metal state. They found that the ionic correlation effects suppress the bremsstrhlung neutrino energy loss typically by a factor 2-20. The present findings will bear great importance in neutrino astronomy.
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Dissertations / Theses on the topic "Radiative Emission of Neutrino Pair"

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Dinh, Nguyen Dinh. "Probing the Possible TeV Scale See-saw Origin of Neutrino Masses with Charged Lepton Flavour Violation Processes and Neutrino Mass Spectroscopy Using Atoms." Doctoral thesis, SISSA, 2013. http://hdl.handle.net/20.500.11767/4727.

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In the first part of this thesis, we perform a detailed analysis of lepton flavour violation (LFV) within minimal see-saw type extensions of the Standard Model (SM), which give a viable mechanism of neutrino mass generation and provide new particle content at the electroweak scale. We focus, mainly, on predictions and constraints set on each scenario from muon and tau decays ($\mu\to e \gamma$, $\mu\to 3e$, $\tau\to (\mu,e) \gamma$ and $\tau\to 3\mu$) and $\mu-e$ conversion in the nuclei. In particular, we show that in some regions of the parameters space of type I and type II see-saw models, the Dirac and Majorana phases of the neutrino mixing matrix, the ordering and hierarchy of the light neutrino mass spectrum as well as the value of the reactor mixing angle $\theta_{13}$ may considerably affect the size of the LFV observables. Besides, the possibilities to observe the LFV processes in the present and future experiments are also considered. The analytic results of the LFV rates might help to discriminate between the three types of neutrino mass generation models considered. In the second part of the thesis, we study a process of collective de-excitation of atoms in a metastable level into emission mode of a single photon plus a neutrino pair, called radiative emission of neutrino pair (RENP). This process is sensitive to the absolute neutrino mass scale, to the neutrino mass hierarchy and to the nature (Dirac or Majorana) of massive neutrinos. We investigate how the indicated neutrino mass and mixing observables can be determined from the measurement of the corresponding continuous photon spectrum on the example of a transition between specific levels of the Yb atom. The possibility of determining the nature of massive neutrinos and, if neutrinos are Majorana fermions, of obtaining information about the Majorana phases in the neutrino mixing matrix, is analyzed in the cases of normal hierarchical, inverted hierarchical and quasi-degenerate types of neutrino mass spectrum. We find, in particular, that the sensitivity to the nature of massive neutrinos depends critically on the atomic level energy difference relevant in the RENP. \vspace{1cm} The content of this thesis is based on the following works: \begin{itemize} \item[ I, ] D.~N.~Dinh, A.~Ibarra, E.~Molinaro and S.~T.~Petcov, \\ \textit{The $\mu\to e$ Conversion in Nuclei, $\mu\rightarrow e +\gamma$, $\mu\rightarrow 3e$ Decays and TeV Scale See-Saw Scenarios of Neutrino Mass Generation},\\ JHEP {\bf 1208} (2012) 125, Erratum-ibid. 1309 (2013) 023 [arXiv:hep-ph/1205.4671v4]. %%% \item[ II, ] D.~N.~Dinh and S.~T.~Petcov,\\ \textit{Lepton Flavor Violating $\tau$ Decays in TeV Scale Type I See-saw and Higgs Triplet Models},\\ JHEP {\bf 09} (2013) 086 [arXiv:hep-ph/1308.4311]. %%% \item[ III, ] D.~N.~Dinh, S.~T.~Petcov, N.~Sasao, M.~Tanaka and M.~Yoshimura,\\ \textit{Observables in Neutrino Mass Spectroscopy Using Atoms},\\ Phys.\ Lett.\ B {\bf 719} (2013) 154 [arXiv:hep-ph/1209.4808]. \end{itemize} Other papers of the same author, which are not discussed in the thesis: \begin{itemize} \item[ I, ] D.~N.~Dinh and S.~T.~Petcov,\\ \textit{Sterile Neutrino Determination Using Radiative Emission of Neutrino Pair},\\ Work in progress. %%% \item[ II, ] D.~N.~Dinh, N.~A.~Ky, N.~T.~H.~Van and P.~Q.~Van,\\ \textit{Model of neutrino effective masses},\\ Phys.\ Rev.\ D {\bf 74} (2006) 077701. \end{itemize}
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Conference papers on the topic "Radiative Emission of Neutrino Pair"

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Titov, A. I., B. Kämpfer, H. Takabe, A. Hosaka, Atsushi Hosaka, Kanchan Khemchandani, Hideko Nagahiro, and Kanabu Nawa. "Neutrino pair emission off electrons in a strong electromagnetic wave field." In INTERNATIONAL CONFERENCE ON THE STRUCTURE OF BARYONS (BARYONS' 10). AIP, 2011. http://dx.doi.org/10.1063/1.3647377.

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Maruyama, Tomoyuki. "Neutron Star Cooling on Strong Magnetic Field : Neutrino -Antineutrino Pair Emission and Direct Urca Processes." In Particles and Nuclei International Conference 2021. Trieste, Italy: Sissa Medialab, 2022. http://dx.doi.org/10.22323/1.380.0320.

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LEINSON, L. B. "PLASMA EFFECTS IN NEUTRINO-PAIR EMISSION DUE TO COOPER PAIRING OF PROTONS IN SUPERCONDUCTING NEUTRON STARS." In Proceedings of the VIII International Workshop. WORLD SCIENTIFIC, 2003. http://dx.doi.org/10.1142/9789812704429_0059.

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Fauchet, P. M., Y. Kostoulas, Ju V. Vandyshev, L. Tsybeskov, K. B. Ucer, L. Waxer, I. A. Walmsley, and V. Petrova-Koch. "Ultrafast Electronic Processes in Porous Silicon." In International Conference on Ultrafast Phenomena. Washington, D.C.: Optica Publishing Group, 1994. http://dx.doi.org/10.1364/up.1994.wc.16.

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The discovery in 1990 [1] that porous silicon is a strong light emitter in the visible at room temperature has changed our assessment of the usefulness of silicon as an optoelectronic material and raises the possibility of practical silicon light emitters [2]. The luminescence from light emitting porous silicon (LEPSi) usually occurs in the deep red to orange region with a quantum efficiency of a few percents at 300 K and >10% at low temperature. The luminescence decays with a lifetime that ranges from ~1-10 μsec at 300 K to >1 msec at low temperature. More than 15 different models have been proposed to explain the strong luminescence from LEPSi [3] but only two models have received strong experimental support. In the first model, light emission results from the recombination of a free electron-hole pair or exciton across the bandgap of silicon nanoparticles [1,4]. The emission is in the visible because the effective bandgap is increased by quantum confinement and the quantum efficiency is high because the bandgap of these silicon nanoparticles has become quasi-direct and because nonradiative recombination is suppressed thanks to the good passivation of the nanoparticle surface. In the second model, light emission results from radiative recombination involving carriers trapped in states localized on the nanoparticle surface [5]. These surface states are in the forbidden gap of the silicon nanocrystallites which is increased by quantumconfinement. The long lifetime of the luminescence is explained by the small overlap between the wavefunctions of carriers localized at physically separated states. To date, no experiment has been able to decide which model is correct.
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Reports on the topic "Radiative Emission of Neutrino Pair"

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Schinder, P. J., D. N. Schramm, P. J. Witta, S. H. Margolis, and D. L. Tubbs. Neutrino emission by the pair, plasma, and photo processes in the Weinberg-Salam model. Office of Scientific and Technical Information (OSTI), June 1986. http://dx.doi.org/10.2172/5140907.

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