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

Author: Grafiati

Published: 14 March 2023

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1

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

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2

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 (2015): 53B06–0. http://dx.doi.org/10.1093/ptep/ptv064.

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3

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 (2010): 523–32. http://dx.doi.org/10.1143/ptp.123.523.

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4

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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5

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 (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 dependenc

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6

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 (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 stem

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7

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 axisymme

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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 (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 r

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9

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 t

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10

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-Sal

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11

Yusof, N., H. Abu Kassim, L. G. Garba, and N. S. Ahmad. "The neutrino emission from thermal processes in very massive stars in the local universe." Monthly Notices of the Royal Astronomical Society 503, no. 4 (2021): 5965–75. http://dx.doi.org/10.1093/mnras/stab762.

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ABSTRACT We present a new overview of the life of very massive stars (VMS) in terms of neutrino emission from thermal processes: pair annihilation, plasmon decay, photoneutrino process, bremsstrahlung, and recombination processes in burning stages of selected VMS models. We use the realistic conditions of temperature, density, electron fraction, and nuclear isotropic composition of the VMS. Results are presented for a set of progenitor stars with mass of 150, 200, and 300 M⊙Z = 0.002 and 500 M⊙Z = 0.006 rotating models which are expected to explode as a pair instability supernova at the end of

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12

ESPOSITO, S., G. MANGANO, G. MIELE, I. PICARDI, and O. PISANTI. "RADIATIVE CORRECTIONS TO NEUTRINO ENERGY LOSS RATE IN STELLAR INTERIORS." Modern Physics Letters A 17, no. 08 (2002): 491–502. http://dx.doi.org/10.1142/s0217732302006643.

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We consider radiative electromagnetic corrections, at order α, to the process [Formula: see text] at finite density and temperature. This process represents one of the main contributions to the cooling of stellar environments in the late stages of star evolution. We find that these corrections affect the energy loss rate by a factor (-4-1)% with respect to the tree level estimate, in the temperature and density ranges where the neutrino pair production via e+e- annihilation is the most efficient cooling mechanism.

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13

Jaikumar, Prashanth, and Madappa Prakash. "Neutrino pair emission from Cooper pair breaking and recombination in superfluid quark matter." Physics Letters B 516, no. 3-4 (2001): 345–52. http://dx.doi.org/10.1016/s0370-2693(01)00916-9.

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14

HATSUDA, T., C. S. LIM, and M. YOSHIMURA. "HARD X-RAY SPECTRUM FROM SN 1987A AND RADIATIVE NEUTRINO DECAY." Modern Physics Letters A 03, no. 12 (1988): 1133–36. http://dx.doi.org/10.1142/s0217732388001355.

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The radiative neutrino decay is shown to explain the hard X-ray energy spectrum (10 keV-200 keV) from SN 1987a, observed by Ginga and Kvant. After the outer expanding shell becomes transparent to the X-ray, the spectrum, in our picture, is nearly constant and directly reflects the dynamical mechanism of the neutrino emission and its subsequent decay.

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15

Rodríguez-Ramírez, J. C., Elisabete M. de Gouveia Dal Pino та R. Alves Batista. "Neutrino and γ-ray Emission from the Core of NGC1275 by Magnetic Reconnection: GRMHD Simulations and Radiative Transfer/Particle Calculations". Proceedings of the International Astronomical Union 14, S342 (2018): 184–88. http://dx.doi.org/10.1017/s1743921318007950.

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AbstractVery high energy (VHE) emission has been detected from the radio galaxy NGC1275, establishing it as a potential cosmic-ray (CR) accelerator and a high energy neutrino source. We here study neutrino and γ-ray emission from the core of NGC1275 simulating the interactions of CRs assumed to be accelerated by magnetic reconnection, with the accreting plasma environment. To do this, we combine (i) numerical general relativistic (GR) magneto-hydrodynamics (MHD), (ii) Monte Carlo GR leptonic radiative transfer and, (iii) Monte Carlo interaction of CRs. A leptonic emission model that reproduces

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16

Barut, A. O., Z. Z. Aydin, and I. H. Duru. "Photoproduction of a neutrino pair from an electron and astrophysical implications of neutrino-emission processes." Physical Review D 32, no. 11 (1985): 3051–54. http://dx.doi.org/10.1103/physrevd.32.3051.

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17

Leinson, Lev B. "Neutrino Emission from Cooper Pairs at Finite Temperatures." Advances in High Energy Physics 2018 (2018): 1–11. http://dx.doi.org/10.1155/2018/8963453.

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A brief review is given of the current state of the problem of neutrino pair emission through neutral weak currents caused by the Cooper pairs breaking and formation (PBF) in superfluid baryon matter at thermal equilibrium. The cases of singlet-state pairing with isotropic superfluid gap and spin-triplet pairing with an anisotropic gap are analyzed with allowance for the anomalous weak interactions caused by superfluidity. It is shown that taking into account the anomalous weak interactions in both the vector and axial channels is very important for a correct description of neutrino energy los

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18

Dzhioev, Alan A., and A. I. Vdovin. "Neutrino-antineutrino pair emission from thermally excited nuclei in stellar collapse." Physics of Atomic Nuclei 77, no. 9 (2014): 1166–72. http://dx.doi.org/10.1134/s1063778814080067.

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19

Leinson, L. B. "Neutrino pair emission from the inner crust of a neutron star." Space Science Reviews 74, no. 3-4 (1995): 481–84. http://dx.doi.org/10.1007/bf00751437.

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20

Maruyama, Tomoyuki, A. Baha Balantekin, Myung-Ki Cheoun, Toshitaka Kajino, and Grand J. Mathews. "Neutrino and Antineutrino pair-Emission in Strong Magnetic Field in Relativistic Quantum Approach." EPJ Web of Conferences 260 (2022): 11029. http://dx.doi.org/10.1051/epjconf/202226011029.

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We study the v\bar v\-pair emission from electrons and protons in a relativistic quantum approach. In this work we calculate the luminosity of the v\bar v\-pairs emitted from neutron-star-matter with a strong magnetic field, and find that this luminosity is much larger than that in the modified Urca process. The v\bar v\-pair emission processes in strong magnetic fields significantly contribute to the cooling of the magnetars.

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21

Smponias, Theodoros. "Synthetic Neutrino Imaging of a Microquasar." Galaxies 9, no. 4 (2021): 80. http://dx.doi.org/10.3390/galaxies9040080.

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Microquasar binary stellar systems emit electromagnetic radiation and high-energy particles over a broad energy spectrum. However, they are so far away that it is hard to observe their details. A simulation offers the link between relatively scarce observational data and the rich theoretical background. In this work, high-energy particle emission from simulated twin microquasar jets is calculated in a unified manner. From the cascade of emission within an element of jet matter to the dynamic and radiative whole jet model, the series of physical processes involved are integrated together. A pro

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22

Chang, Yu-Ling, Bruno Arsioli, Wenlian Li, Donglian Xu, and Liang Chen. "Hunting for Neutrino Emission from Multifrequency Variable Sources." Astrophysical Journal 939, no. 2 (2022): 123. http://dx.doi.org/10.3847/1538-4357/ac8c32.

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Abstract Pinpointing the neutrino sources is crucial to unveil the mystery of high-energy cosmic rays. The search for neutrino source candidates from coincident neutrino-photon signatures and objects with particular electromagnetic flaring behaviors can increase our chances of finding neutrino emitters. In this paper, we first study the temporal correlations of astrophysical flares with neutrinos, considering a few hundred multifrequency sources from the Atacama Large Millimeter/submillimeter Array, the Wide-field Infrared Survey Explorer (WISE), Swift, and Fermi in the containment regions of

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23

CH. ZHUKOVSKY, V., P. A. EMINOV, and A. E. GRIGORUK. "RADIATIVE DECAY OF A MASSIVE NEUTRINO IN THE WEINBERG–SALAM MODEL WITH MIXING IN A CONSTANT UNIFORM MAGNETIC FIELD." Modern Physics Letters A 11, no. 39n40 (1996): 3119–26. http://dx.doi.org/10.1142/s0217732396003106.

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Influence of an external magnetic field on the neutrino decay process with emission of a linearly polarized photon is considered. The decay rate is shown to be enhanced as compared to the free case in the broad region where both the nonvanishing neutrino mass and the field make substantial contributions. In the limit of a negligible neutrino mass the emitted photons are totally linearly polarized, which may help in the identification of these photons.

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24

Shibata, S. "Modes of Energy Loss from Isolated Magnetized Neutron Star." Symposium - International Astronomical Union 125 (1987): 450. http://dx.doi.org/10.1017/s0074180900161121.

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Pulsar may be regarded as a discharge tube by electron-positron pair creation. On this viewpoint we carry out two numerical calculations. The obtained magnetic field is consistent with the flow. We find that pulsars emit their rotational energy through three modes simultaneously. The three modes are (1)relativistic acceleration and following gamma-ray emission in the closed current circuit in the magnetosphere, (2)wind of the electron-positron pair plasma, and (3)dipole radiation.

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25

Caputo, Andrea, Marco Regis, and Marco Taoso. "Searching for sterile neutrino with X-ray intensity mapping." Journal of Cosmology and Astroparticle Physics 2020, no. 03 (2020): 001. http://dx.doi.org/10.1088/1475-7516/2020/03/001.

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The cosmological X-ray emission associated to the possible radiative decay of sterile neutrinos is composed by a collection of lines at different energies. For a given mass, each line corresponds to a given redshift. In this work, we cross correlate such line emission with catalogs of galaxies tracing the dark matter distribution at different redshifts. We derive observational prospects by correlating the X-ray sky that will be probed by the eROSITA and Athena missions with current and near future photometric and spectroscopic galaxy surveys. A relevant and unexplored fraction of the parameter

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26

Rahman, N., H.-T. Janka, G. Stockinger, and S. E. Woosley. "Pulsational pair-instability supernovae: gravitational collapse, black hole formation, and beyond." Monthly Notices of the Royal Astronomical Society 512, no. 3 (2022): 4503–40. http://dx.doi.org/10.1093/mnras/stac758.

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ABSTRACT We investigate the final collapse of rotating and non-rotating pulsational pair-instability supernova progenitors with zero-age-main-sequence masses of 60, 80, and 115 M⊙ and iron cores between 2.37 and 2.72 M⊙ by 2D hydrodynamics simulations. Using the general relativistic NADA-FLD code with energy-dependent three-flavour neutrino transport by flux-limited diffusion allows us to follow the evolution beyond the moment when the transiently forming neutron star (NS) collapses to a black hole (BH), which happens within 350–580 ms after bounce in all cases. Because of high neutrino lumino

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27

Asseo, E., G. Pelletier, and H. Sol. "A Non-Linear Emission Mechanism for Pulsar Radio Radiation." International Astronomical Union Colloquium 128 (1992): 322–25. http://dx.doi.org/10.1017/s0002731600155428.

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Among the various plasma instabilities which could be responsible for coherent pulsar radio emission, we investigate the two-stream instability, first introduced by Ruderman and Sutherland (1975) in order to account for the physical situation expected in the environment of neutron stars. They describe how, in a polar cap model, pair creation arises and leads to the formation of a very energetic beam of e+ (and/or e−) and of an e−e+ plasma, both with relativistic bulk motion along the bundle of dipolar magnetic field lines. The study of their interaction is limited to the cone of open B lines,

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28

Rowe, E. T. "Beams in Magnetised Pair Plasmas." International Astronomical Union Colloquium 177 (2000): 409–10. http://dx.doi.org/10.1017/s0252921100060152.

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AbstractThe radiative instability was considered in the context of pulsar radio emission by Goldreich &amp; Keeley (1971) and rederived and extended by Asséo, Pellat, &amp; Sol (1983) and by Asséo (1995). Their results can be generalised and reproduced by replacing the thin cylindrical ring of charged particles by an infinitesimally thin current carrying sheet in either planar or cylindrical geometry, suggesting that the local ring geometry may not be essential for the instability. It may be useful to further investigate the generalised dispersion equation given below.

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29

AKSENOV, A. G., R. RUFFINI, I. A. SIUTSOU, and G. V. VERESHCHAGIN. "DYNAMICS AND EMISSION OF MILDLY RELATIVISTIC PLASMA." International Journal of Modern Physics: Conference Series 12 (January 2012): 1–9. http://dx.doi.org/10.1142/s2010194512006204.

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Initially optically thick (with τ = 3⋅107) spherically symmetric outflow consisting of electron-positron pairs and photons is considered. We do not assume thermal equilibrium, and include the two-body processes that occur in such plasma: Möller and Bhabha scattering of pairs, Compton scattering, two-photon pair annihilation, two-photon pair production, together with their radiative three-body variants: bremsstrahlung, double Compton scattering, and three-photon pair annihilation, with their inverse processes. We solve numerically the relativistic Boltzmann equations in spherically symmetric ca

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30

Li, Shao-Ze, Yun-Wei Yu, He Gao, Zi-Gao Dai, and Xiao-Ping Zheng. "A Powerful e ^± Outflow Driven by a Proto-strange Quark Star." Astrophysical Journal 922, no. 2 (2021): 214. http://dx.doi.org/10.3847/1538-4357/ac2d2f.

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Abstract An electron–positron layer can cover the surface of a bare strange star (SS), the electric field in which can excite the vacuum and drive a pair wind by taking away the heat of the star. In order to investigate the pair-emission ability of a proto-SS, we establish a toy model to describe its early thermal evolution, where the initial trapping of neutrinos is specially taken into account. It is found that the early cooling of the SS is dominated by the neutrino diffusion rather than the conventional Urca processes, which leads to the appearance of an initial temperature plateau. During

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31

Baring, Matthew G. "Synchrotron Radiation from Energetic Electrons Emitted by AGN: A Probe for Magnetic Fields in External Galaxies." Symposium - International Astronomical Union 140 (1990): 399. http://dx.doi.org/10.1017/s0074180900190631.

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Shock acceleration of protons in the central region of active galaxies can energize them to Lorentz factors as high as 108 (Sikora et al., 1987), and these can subsequently produce a host of other relativistic particles including pions, e+e– pairs and neutrons. The luminosities of each species are expected to be of the same order of magnitude. Rapid decay of the pions leads to the secondary production of photons and pairs with energies of around 109 − 1011 MeV. The electrons and positrons can escape the compact central region and interact with the microwave background forming a pair cascade, a

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32

Leinson, L. B. "Collective neutrino-pair emission due to Cooper pairing of protons in superconducting neutron stars." Nuclear Physics A 687, no. 3-4 (2001): 489–511. http://dx.doi.org/10.1016/s0375-9474(00)00575-3.

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33

Kurihara, Y., J. Fujimoto, T. Ishikawa, Y. Shimizu, and T. Munehisa. ": Event generator for the single- and double-photon emission associated with neutrino pair-production." Computer Physics Communications 136, no. 3 (2001): 250–68. http://dx.doi.org/10.1016/s0010-4655(00)00254-x.

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34

Schinder, Paul J., David N. Schramm, Paul J. Wiita, Steven H. Margolis, and David L. Tubbs. "Neutrino emission by the pair, plasma, and photo processes in the Weinberg-Salam model." Astrophysical Journal 313 (February 1987): 531. http://dx.doi.org/10.1086/164993.

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35

Gajiyeva, B. "General Formula for Impulse Losses in the Process of Emission of Neutrino Pairs by Electrons in a Magnetic Field." Bulletin of Science and Practice 7, no. 9 (2021): 27–31. http://dx.doi.org/10.33619/2414-2948/70/02.

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Considered formula pulsed radiation losses pairs neutrinos electrons in a magnetic field. Gas consisting of polarized electrons in the direction of the magnetic field and spins composed of polarized electrons in the opposite direction of the magnetic field would receive a different impulse due to the asymmetric transmission of the impulse.

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36

Hakobyan, H., B. Ripperda, and A. A. Philippov. "Radiative Reconnection-powered TeV Flares from the Black Hole Magnetosphere in M87." Astrophysical Journal Letters 943, no. 2 (2023): L29. http://dx.doi.org/10.3847/2041-8213/acb264.

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Abstract Active galactic nuclei in general, and the supermassive black hole in M87 in particular, show bright and rapid gamma-ray flares up to energies of 100 GeV and above. For M87, the flares show multiwavelength components, and the variability timescale is comparable to the dynamical time of the event horizon, suggesting that the emission may come from a compact region near the nucleus. However, the emission mechanism for these flares is not well understood. Recent high-resolution general-relativistic magnetohydrodynamic simulations show the occurrence of episodic magnetic reconnection even

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37

Melatos, A. "Neutrinos from Pulsar Environments." Highlights of Astronomy 13 (2005): 18–23. http://dx.doi.org/10.1017/s1539299600014970.

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AbstractRecent calculations of the neutrino fluxes and spectra from pulsar magnetospheres and wind nebulae are reviewed. The neutrinos, produced in pp and pγ collisions via pion decays, are a signature of TeV ions accelerated electrostatically in the magnetosphere, in the wind termination shock (Fermi), or in the wind neutral sheet (wave surfing and/or reconnection). The fluxes and spectra are related to the energy and density of the accelerated ion beam and the densities of the target species, thereby constraining ion-loaded pulsar wind models originally developed to explain the variable wisp

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38

LEVINSON, AMIR. "HIGH-ENERGY ASPECTS OF ASTROPHYSICAL JETS." International Journal of Modern Physics A 21, no. 30 (2006): 6015–54. http://dx.doi.org/10.1142/s0217751x06035063.

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Various aspects of the high-energy emission from relativistic jets associated with compact astrophysical systems are reviewed. The main leptonic and hadronic processes responsible for the production of high-energy γ-rays, very-high-energy neutrinos and ultra-high energy cosmic rays are discussed. Relations between the γγ pair production and photomeson production opacities are derived, and their consequences for the relative emission of γ-rays and neutrinos are examined. The scaling of the size and location of the various emission zones and other quantities with black hole mass and dimensionles

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39

Astraatmadja, Tri L. "Detecting TeV γ-rays from GRBs with km3 neutrino telescopes". Proceedings of the International Astronomical Union 7, S279 (2011): 321–22. http://dx.doi.org/10.1017/s1743921312013154.

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AbstractObserving TeV photons from GRBs can greatly enhance our understanding of their emission mechanisms. Under-sea/ice neutrino telescopes—such as ANTARES in the Mediterranean Sea or IceCube at the South Pole—can also operate as a γ-ray observatory by detecting downgoing muons from the electromagnetic cascade induced by the interaction of the photons with the Earth's atmosphere. Theoretical calculations of the number of detectable muons from single GRB events, located at different redshifts and zenith distances, have been performed. The attenuation by pair production of TeV photons with cos

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40

Leinson, L. B. "Neutrino-pair emission due to electron-phonon scattering in a neutron star crust: a reappraisal." Physics Letters B 469, no. 1-4 (1999): 166–70. http://dx.doi.org/10.1016/s0370-2693(99)01278-2.

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41

Pétri, Jérôme. "Electrodynamics and Radiation from Rotating Neutron Star Magnetospheres." Universe 6, no. 1 (2020): 15. http://dx.doi.org/10.3390/universe6010015.

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Neutron stars are compact objects rotating at high speed, up to a substantial fraction of the speed of light (up to 20% for millisecond pulsars) and possessing ultra-strong electromagnetic fields (close to and sometimes above the quantum critical field of 4.4 × 10 9 T ). Moreover, due to copious e ± pair creation within the magnetosphere, the relativistic plasma surrounding the star is forced into corotation up to the light cylinder where the corotation speed reaches the speed of light. The neutron star electromagnetic activity is powered by its rotation which becomes relativistic in the neigh

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42

Ito, Hirotaka, Amir Levinson, and Shigehiro Nagataki. "Monte Carlo simulations of relativistic radiation-mediated shocks: II. photon-starved regime." Monthly Notices of the Royal Astronomical Society 492, no. 2 (2019): 1902–13. http://dx.doi.org/10.1093/mnras/stz3591.

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ABSTRACT Radiation-mediated shocks (RMS) play a key role in shaping the early emission observed in many transients. In most cases, e.g. shock breakout in supernovae, llGRBs, and neutron star mergers, the upstream plasma is devoid of radiation, and the photons that ultimately reach the observer are generated predominantly inside and downstream of the shock. Predicting the observed spectrum requires detailed calculations of the shock structure and thermodynamic state that account properly for the shock microphysics. We present results of self-consistent Monte Carlo simulations of photon-starved

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43

Buchal, Ch, and M. Löken. "Silicon-Based Metal-Semiconductor-Metal Detectors." MRS Bulletin 23, no. 4 (1998): 55–59. http://dx.doi.org/10.1557/s088376940003027x.

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Photodetectors must provide fast and efficient conversion of photons to charge carriers. When considering semiconductor light sources, the indirect bandgap of silicon and germanium represents a serious obstacle to radiative electron-hole recombinations. Momentum conservation demands the simultaneous interaction of the electron-hole pair with a momentum-matching phonon. As a consequence, radiative recombinations are five orders of magnitude less probable in Si if compared to a direct semiconductor such as GaAs.Although the absorption of a photon and the generation of an electron-hole pair may b

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Wang, Ze-Rui, and Rui Xue. "Hadronuclear interpretation of the possible neutrino emission from PKS B1424-418, GB6 J1040+0617 and PKS 1502+106." Research in Astronomy and Astrophysics 21, no. 12 (2021): 305. http://dx.doi.org/10.1088/1674-4527/21/12/305.

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Abstract In addition to neutrino event IceCube-170922A which is observed to be associated with a γ-ray flare from blazar TXS 0506+056, there are also several neutrino events that may be associated with blazars. Among them, PKS B1424-418, GB6 J1040+0617 and PKS 1502+106 are low synchrotron peaked sources, which are usually believed to have the broad line region in the vicinity of the central black hole. They are considered as counterparts of IceCube event 35, IceCube-141209A and IceCube-190730A, respectively. By considering the proton-proton (pp) interactions between the dense gas clouds in the

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Nava, L., L. Sironi, G. Ghisellini, A. Celotti, and G. Ghirlanda. "Afterglow emission in gamma-ray bursts – I. Pair-enriched ambient medium and radiative blast waves." Monthly Notices of the Royal Astronomical Society 433, no. 3 (2013): 2107–21. http://dx.doi.org/10.1093/mnras/stt872.

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Zhang, Lian, Hua-Yu Wang, Ning Wang, et al. "Broadband enhancement of spontaneous emission by optical dipole nanoantenna on metallic substrate: An intuitive model of surface plasmon polariton." Acta Physica Sinica 71, no. 11 (2022): 118101. http://dx.doi.org/10.7498/aps.70.20212290.

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<sec>Optical nanoantennas can achieve electromagnetic-field enhancement under far-field excitation or spontaneous-emission enhancement under excitation by radiating emitters. Among them, nanoantennas on a metallic substrate (i.e. the so-called nanoparticle-on-mirror antennas) have aroused great research interest due to their ease in forming metallic gaps of sizes down to a few nanometers or even subnanometer. Here we propose an optical dipole nanoantenna on a metallic substrate with a broadband enhancement of spontaneous emission. Its total and radiative emission-rate enhancement factors

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Dundovic, A., C. Evoli, D. Gaggero, and D. Grasso. "Simulating the Galactic multi-messenger emissions with HERMES." Astronomy & Astrophysics 653 (September 2021): A18. http://dx.doi.org/10.1051/0004-6361/202140801.

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Context. The study of nonthermal processes such as synchrotron emission, inverse Compton scattering, bremsstrahlung, and pion production is crucial to understanding the properties of the Galactic cosmic-ray population, to shed light on their origin and confinement mechanisms, and to assess the significance of exotic signals possibly associated to new physics. Aims. We present a public code called HERMES which is designed generate sky maps associated to a variety of multi-messenger and multi-wavelength radiative processes, spanning from the radio domain all the way up to high-energy gamma-ray a

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Svensson, Roland. "Physical Processes in Active Galactic Nuclei." International Astronomical Union Colloquium 89 (1986): 324–45. http://dx.doi.org/10.1017/s0252921100086152.

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AbstractActive galactic nuclei (AGNs) emit continuum radiation evenly spread over up to ten decades in frequency from the radio into the gamma-ray range. Plausible emission mechanisms and their characteristics are reviewed. In the deep potential wells around black holes the mean energy per proton can reach 100 MeV. Part or all of this energy may be channeled to all electrons equally (thermal plasma) or, preferentially, into only a small fraction of the electrons (nonthermal plasma). In the former case thermal Comptonization of soft photons may be the dominant emission mechanism, while in the l

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Zhdankin, Vladimir, Dmitri A. Uzdensky, Gregory R. Werner, and Mitchell C. Begelman. "Kinetic turbulence in shining pair plasma: intermittent beaming and thermalization by radiative cooling." Monthly Notices of the Royal Astronomical Society 493, no. 1 (2020): 603–26. http://dx.doi.org/10.1093/mnras/staa284.

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ABSTRACT High-energy astrophysical systems frequently contain collision-less relativistic plasmas that are heated by turbulent cascades and cooled by emission of radiation. Understanding the nature of this radiative turbulence is a frontier of extreme plasma astrophysics. In this paper, we use particle-in-cell simulations to study the effects of external inverse Compton radiation on turbulence driven in an optically thin, relativistic pair plasma. We focus on the statistical steady state (where injected energy is balanced by radiated energy) and perform a parameter scan spanning from low magne

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Faran, Tamar, and Re'em Sari. "Shock Breakout from Stellar Envelopes: The Relativistic Limit." Astrophysical Journal 943, no. 2 (2023): 97. http://dx.doi.org/10.3847/1538-4357/aca7fd.

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Abstract We calculate the observed luminosity and spectrum following the emergence of a relativistic shock wave from a stellar edge. Shock waves propagating at 0.6 < Γsh β sh, where Γsh is the shock Lorentz factor, and β sh is its associated reduced velocity, heat the stellar envelope to temperatures exceeding ∼50 keV, allowing for a vigorous production of electron and positron pairs. Pairs significantly increase the electron-scattering optical depth and regulate the temperature through photon generation, producing distinct observational signatures in the escaping emission. Assuming Wien eq

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