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Articles de revues sur le sujet « Neutron emissions »

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Auteur : Grafiati
Publié le 14 mars 2023

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1

Petrucci, Andrea, Alberto Rosada et Emilio Santoro. « Asymmetric neutron emissions from sonicated steel ». Modern Physics Letters B 29, no 14 (29 mai 2015) : 1550067. http://dx.doi.org/10.1142/s0217984915500670.

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Following up published works in which we studied and experimentally verified the assumptions of the theory of "Deformed Space-Time" in relation to piezonuclear emissions, and according to previous experiments of sonication by ultrasounds performed on solid materials with high density, cylindrical bars of AISI 304 steel have been sonicated by ultrasounds of the power of 330 Watts and frequency of 20 KHz. We verified by means of passive detectors CR39 (PADC) pulsed emissions of neutrons. In this work, following a recent proposal, it was decided to perform a stereoscopic measurement of neutron emission. It has been verified that they are characterized by a distribution which is anisotropic and asymmetric in the space. The work shows a wide and accurate description of the experiment and the results of neutron emissions, and we stress that there exist two directions corresponding to maximum emission (maximum dose) and zero emission (null dose).
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2

Albertini, G., V. Calbucci et F. Cardone. « Statistics of piezonuclear emissions : early results ». Modern Physics Letters B 28, no 05 (18 février 2014) : 1450036. http://dx.doi.org/10.1142/s0217984914500365.

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Measurements of ionizing and nonionizing particles are performed during the rupture tests of steel rods having different diameter. A ZnS ( Ag ) alpha detector, a Geiger counter and a 3 He proportional counter for neutrons are used. From the distributions of the recorded intensity maxima, different particles emissions are suggested to occur in broken and nonbroken samples. A hint for the emission of neutrons at rupture is also obtained. Such neutron emissions are predicted in the framework of the piezonuclear theory.
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3

Petrucci, Andrea, et Alberto Rosada. « Ultrasonic Neutron Emissions ». Journal of Advanced Physics 5, no 1 (1 mars 2016) : 63–68. http://dx.doi.org/10.1166/jap.2016.1246.

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4

Pozzi, Sara A., Brian Wieger, Andreas Enqvist, Shaun D. Clarke, Marek Flaska, Matthew Marcath, Edward Larsen, Robert C. Haight et Enrico Padovani. « Correlated Neutron Emissions from252Cf ». Nuclear Science and Engineering 178, no 2 (octobre 2014) : 250–60. http://dx.doi.org/10.13182/nse13-96.

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5

Bradnam, Steven C., Vytautas Astromskas, Zamir Ghani, Mark R. Gilbert, Malcolm J. Joyce et Lee W. Packer. « DEVELOPMENT AND EXPERIMENTAL VALIDATION OF RESPONSE MODELLING FOR TIME-OF-FLIGHT NEUTRON DETECTION AND IMAGING SYSTEMS ». EPJ Web of Conferences 247 (2021) : 16001. http://dx.doi.org/10.1051/epjconf/202124716001.

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The application and feasibility of a time-of-flight neutron detection system is explored for sources with time correlated gamma-ray and neutron emissions, such as the spontaneous fission emitter, Cf-252. For the emission of multiple gamma rays and neutrons from a single spontaneous fission event, a near instantaneous gamma-ray detection followed by a later neutron detection on a multi-detector array allows for an associated time-of-flight to be determined for a neutron arising from that event. Using a suite of purpose developed analysis tools, Monte-Carlo simulation and experimental data are compared for the Cf-252 water tank source facility at Lancaster University. Applying a bespoke time-of-flight imaging algorithm, vector-based optimisation (VBO), the true source location is determined within 21 cm by this approach.
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6

Muraki, Y., K. Koga, T. Goka, H. Matsumoto, T. Obara, O. Okudaira, S. Shibata et T. Yamamoto. « Measurement by FIB on the ISS : Two Emissions of Solar Neutrons Detected ? » Advances in Astronomy 2012 (2012) : 1–14. http://dx.doi.org/10.1155/2012/379304.

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A new type of solar neutron detector (FIB) was launched on board the Space Shuttle Endeavour on July 16, 2009, and began collecting data at the International Space Station (ISS) on August 25, 2009. This paper summarizes the three years of observations obtained by the solar neutron detector FIB until the end of July 2012. The solar neutron detector FIB can determine both the energy and arrival direction of neutrons. We measured the energy spectra of background neutrons over the South Atlantic Anomaly (SAA) region and elsewhere and found the typical trigger rates to be 20 and 0.22 counts/sec, respectively. It is possible to identify solar neutrons to within a level of 0.028 counts/sec, provided that directional information is applied. Solar neutrons were possibly observed in association with the M-class solar flares that occurred on March 7 (M3.7) and June 7 (M2.5) of 2011. This marked the first time that neutrons had been observed in M-class solar flares. A possible interpretation of the production process is provided.
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7

Vartanyan, David, Adam Burrows et David Radice. « Temporal and angular variations of 3D core-collapse supernova emissions and their physical correlations ». Monthly Notices of the Royal Astronomical Society 489, no 2 (21 août 2019) : 2227–46. http://dx.doi.org/10.1093/mnras/stz2307.

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Abstract We provide the time series and angular distributions of the neutrino and gravitational wave emissions of 11 state-of-the-art 3D non-rotating core-collapse supernova models and explore correlations between these signatures and the real-time dynamics of the shock and the proto-neutron star (PNS) core. The neutrino emissions are roughly isotropic on average, with instantaneous excursions about the mean inferred luminosity of as much as ±20 per cent. The deviation from isotropy is least for the ‘νμ’-type neutrinos and the lowest mass progenitors. Instantaneous temporal luminosity variations along a given direction for exploding models average ∼2–4 per cent, but can be as high as ∼10 per cent. For non-exploding models, they can achieve ∼25 per cent. The temporal variations in the neutrino emissions correlate with the temporal and angular variations in the mass accretion rate. We witness the lepton-number emission self-sustained asymmetry (LESA) phenomenon in all our models and find that the vector direction of the LESA dipole and that of the inner Ye distribution are highly correlated. For our entire set of 3D models, we find strong connections between the cumulative neutrino energy losses, the radius of the proto-neutron star, and the f-mode frequency of the gravitational wave emissions. When physically normalized, the progenitor-to-progenitor variation in any of these quantities is no more than ∼10 per cent. Moreover, the reduced f-mode frequency is independent of time after bounce to better than ∼10 per cent. Therefore, simultaneous measurement of gravitational waves and neutrinos from a given supernova event can be used synergistically to extract real physical quantities of the supernova core.
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8

Mohindroo, Kumar S., Yaron Danon, Ezekiel Blain, Matthew Devlin et Keegan J. Kelly. « Quasi-differential neutron induced neutron emissions from 235U, and 239Pu ». Annals of Nuclear Energy 165 (janvier 2022) : 108647. http://dx.doi.org/10.1016/j.anucene.2021.108647.

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9

Kromar, Marjan, et Bojan Kurinčič. « Assessment of the Photon and Neutron Source Term for the NPP Krško Spent Fuel ». Journal of Energy - Energija 68, no 2-3 (8 juillet 2022) : 184–98. http://dx.doi.org/10.37798/2019682-3202.

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Accurate knowledge of the fuel nuclide inventory is important after reactor shut down, during the fuel storage and subsequent reprocessing or disposal to provide adequate shielding from the photon and neutron radiation. In this paper possibility to calculate the NPP Krško photon and neutron source term with the Serpent code has been analysed. Some deficiencies in the supplied ENDF/B-VII.0 decay library have been observed. In addition, Serpent reports only spontaneous fission rates without (α, n) and (β, n) contributions. To get neutron emission, spontaneous fission rates had to be multiplied with the average number of neutrons born for each particular nuclide manually. Comparison with the Origen code has shown acceptable agreement of the ENDF/B-VII.1 results. Influence of several factors such as fuel burnup, enrichment, temperature, moderator temperature (density), soluble boron concentration, average power, and burnable absorbers has been analysed. In addition, it was demonstrated that, except for the burnup and enrichment, averaging of all other parameters is acceptable approach. IFBA fuel should be accounted for explicitly due to relative high impact on the photon and neutron emissions.
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10

Kimura, Shigeo S. « High-energy emissions from neutron star mergers ». EPJ Web of Conferences 210 (2019) : 03001. http://dx.doi.org/10.1051/epjconf/201921003001.

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In 2017, LIGO-Virgo collaborations reported detection of the first neutron star merger event, GW170817, which is accompanied by electromagnetic counterparts from radio to gamma rays. Although high-energy neutrinos were not detected from this event, mergers of neutron stars are expected to produce such high-energy particles. Relativistic jets are launched when neutron stars merge. If the jets contain protons, they can emit high-energy neutrinos through photomeson production. In addition, neutron star mergers produce massive and fast ejecta, which can be a source of Galactic high-energy cosmic rays above the knee. We briefly review what we learned from the multi-messenger event, GW170817, and discuss prospects for multi-messenger detections and hadronic cosmic-ray production related to the neutron star mergers.
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11

Cates, Joshua W., John Steele, Jon Balajthy, Victor Negut, Paul Hausladen, Klaus Ziock et Erik Brubaker. « Front-End Design for SiPM-Based Monolithic Neutron Double Scatter Imagers ». Sensors 22, no 9 (7 mai 2022) : 3553. http://dx.doi.org/10.3390/s22093553.

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Neutron double scatter imaging exploits the kinematics of neutron elastic scattering to enable emission imaging of neutron sources. Due to the relatively low coincidence detection efficiency of fast neutrons in organic scintillator arrays, imaging efficiency for double scatter cameras can also be low. One method to realize significant gains in neutron coincidence detection efficiency is to develop neutron double scatter detectors which employ monolithic blocks of organic scintillator, instrumented with photosensor arrays on multiple faces to enable 3D position and multi-interaction time pickoff. Silicon photomultipliers (SiPMs) have several advantageous characteristics for this approach, including high photon detection efficiency (PDE), good single photon time resolution (SPTR), high gain that translates to single photon counting capabilities, and ability to be tiled into large arrays with high packing fraction and photosensitive area fill factor. However, they also have a tradeoff in high uncorrelated and correlated noise rates (dark counts from thermionic emissions and optical photon crosstalk generated during avalanche) which may complicate event positioning algorithms. We have evaluated the noise characteristics and SPTR of Hamamatsu S13360-6075 SiPMs with low noise, fast electronic readout for integration into a monolithic neutron scatter camera prototype. The sensors and electronic readout were implemented in a small-scale prototype detector in order to estimate expected noise performance for a monolithic neutron scatter camera and perform proof-of-concept measurements for scintillation photon counting and three-dimensional event positioning.
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12

Ghosh, Sudip, Maitreyee Nandy, P. K. Sarkar et N. Chakravarty. « Neutron skin effect in preequilibrium nucleon emissions ». Physical Review C 49, no 2 (1 février 1994) : 1059–65. http://dx.doi.org/10.1103/physrevc.49.1059.

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13

Okumura, Shin, Toshihiko Kawano et Satoshi Chiba. « Prompt and Delayed Neutron Emissions and Fission Product Yield Calculations with Hauser-Feshbach Statistical Decay Theory and Summation Calculation Method ». EPJ Web of Conferences 211 (2019) : 04005. http://dx.doi.org/10.1051/epjconf/201921104005.

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We demonstrate the neutron emission and fission product yield calculations using the Hauser–Feshbach Fission Fragment Decay (HF3D) model and β decay. The HF3D model calculates the statistical decay of more than 500 primary fission fragment pairs formed by the neutron induced fission of 235U. In order to calculate the prompt neutron and photon emissions, the primary fission fragment distributions, i.e. mass, charge, excitation energy, spin and parity are deterministically generated and numerically integrated for all fission fragments. The calculated prompt neutron multiplicities, independent fission product yield are fully consistent each other. We combine the β-decay and the summation calculations with the HF3D model calculation to obtain the cumulative fission product yield, decay heat and delayed neutron yield. The calculated fission observables are compared with available experimental data.
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14

Kurt, Viktoria, Karel Kudela, Boris Yushkov et Vladimir Galkin. « On the Onset Time of Several SPE/GLE Events : Indications from High-Energy Gamma-Ray and Neutron Measurements by CORONAS-F ». Advances in Astronomy 2013 (2013) : 1–15. http://dx.doi.org/10.1155/2013/690921.

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We analyzed the high-energy gamma and neutron emissions observed by the SONG instrument onboard the CORONAS-F satellite during August 25, 2001, October 28, 2003, November 4, 2003, and January 20, 2005 solar flares. These flares produced neutrons and/or protons recorded near Earth. The SONG response was consistent with detection of the pion-decay gamma emission and neutrons in these events. We supposed that a time profile of the soft X-ray derivative was a good proxy of time behavior of the flare energy release. Then we showed that time intervals of the maximum both of energy release and pion-decay-emission coincided well. We determined the onset time of GLEs 65, 69 on the basis of neutron monitor data using the superposed epoch method. The time of high-energy proton onset on November 4, 2003 was found from the GOES data. The time delay between the high-energy gamma ray observation and the high-energy protons onset time was <5 minutes. This time lag corresponds to the least possible proton propagation time. So, we conclude that in these events both protons interacted in the solar atmosphere and the first protons which arrived to Earth, belonged to one and the same population of the accelerated particles.
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15

Sun, X. Y., D. Q. Fang, Y. G. Ma, X. Z. Cai, J. G. Chen, W. Guo, W. D. Tian et H. W. Wang. « Neutron/proton ratio of nucleon emissions as a probe of neutron skin ». Physics Letters B 682, no 4-5 (janvier 2010) : 396–400. http://dx.doi.org/10.1016/j.physletb.2009.11.031.

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16

Elaragi, Gamal M. « Design and Operation of First Egyptian IEC Fusion Plasma Device ». Emerging Science Journal 3, no 4 (30 juillet 2019) : 241–48. http://dx.doi.org/10.28991/esj-2019-01186.

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In this paper, Egyptian first inertial electrostatic confinement fusion (IECF) device, constructed at the Egyptian Atomic Energy Authority (EAEA-IEC), is introduced the characterization of IEC Plasma Device. It consists of 2.8 cm stainless steel cathode, 6.5 cm anode diameter with 10 cm diameter 30 cm height vacuum chamber. The discharge current and voltage of plasma discharge has been recorded using current probe and resistive voltage divider respectively. The X-ray emissions in IEC plasma device were investigated by employing time-resolved detector. The temporal distributions of detected x-rays emission are occurring during the initial 1 microsecond. The calculated rate of DD-neutron generation using the same electrode configuration about 106 – 108 neutrons/second.
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17

Harkness, Ira, Ting Zhu, Yinong Liang, Eric Rauch, Andreas Enqvist et Kelly A. Jordan. « Development of Neutron Energy Spectral Signatures for Passive Monitoring of Spent Nuclear Fuels in Dry Cask Storage ». EPJ Web of Conferences 170 (2018) : 07004. http://dx.doi.org/10.1051/epjconf/201817007004.

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Demand for spent nuclear fuel dry casks as an interim storage solution has increased globally and the IAEA has expressed a need for robust safeguards and verification technologies for ensuring the continuity of knowledge and the integrity of radioactive materials inside spent fuel casks. Existing research has been focusing on “fingerprinting” casks based on count rate statistics to represent radiation emission signatures. The current research aims to expand to include neutron energy spectral information as part of the fuel characteristics. First, spent fuel composition data are taken from the Next Generation Safeguards Initiative Spent Fuel Libraries, representative for Westinghouse 17ˣ17 PWR assemblies. The ORIGEN-S code then calculates the spontaneous fission and (α,n) emissions for individual fuel rods, followed by detailed MCNP simulations of neutrons transported through the fuel assemblies. A comprehensive database of neutron energy spectral profiles is to be constructed, with different enrichment, burn-up, and cooling time conditions. The end goal is to utilize the computational spent fuel library, predictive algorithm, and a pressurized 4He scintillator to verify the spent fuel assemblies inside a cask. This work identifies neutron spectral signatures that correlate with the cooling time of spent fuel. Both the total and relative contributions from spontaneous fission and (α,n) change noticeably with respect to cooling time, due to the relatively short half-life (18 years) of the major neutron source 244Cm. Identification of this and other neutron spectral signatures allows the characterization of spent nuclear fuels in dry cask storage.
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18

Li, Li-Xin. « Radioactive Gamma-Ray Emissions from Neutron Star Mergers ». Astrophysical Journal 872, no 1 (6 février 2019) : 19. http://dx.doi.org/10.3847/1538-4357/aaf961.

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19

Kumar, Satish, J. S. Batra et Raj K. Gupta. « Cluster emissions with daughter from neutron-rich nuclei ». Journal of Physics G : Nuclear and Particle Physics 22, no 2 (1 février 1996) : 215–19. http://dx.doi.org/10.1088/0954-3899/22/2/006.

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20

Takahara, M., et K. Sato. « Phase Transitions in the Newly-Born Neutron Star and Neutrino Emissions from SN1987A ». Progress of Theoretical Physics 80, no 5 (1 novembre 1988) : 861–67. http://dx.doi.org/10.1143/ptp.80.861.

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21

Kiuchi, Kenta, Yuichiro Sekiguchi, Koutarou Kyutoku et Masaru Shibata. « Gravitational waves, neutrino emissions and effects of hyperons in binary neutron star mergers ». Classical and Quantum Gravity 29, no 12 (1 juin 2012) : 124003. http://dx.doi.org/10.1088/0264-9381/29/12/124003.

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22

Nishioka, Takahiro, Aki Miyake, Shailendra Singh, Hisashi Morii, Hidenori Mimura et Toru Aoki. « Thermal Neutron Detection by CdTe Detector ». Advanced Materials Research 222 (avril 2011) : 146–49. http://dx.doi.org/10.4028/www.scientific.net/amr.222.146.

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Thermal neutron detector is developed by using Cadmium telluride (CdTe) semiconductor, due to large thermal neutron capture cross section of Cd. The developed detector demonstrated the occurrence of the 96 keV gamma ray emissions from 113Cd(n, γ) 114Cd reaction.
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23

TEL, E., İ. DEMİRKOL, A. ARASOĞLU et B. ŞARER. « PRE-EQUILIBRIUM EMISSION IN DIFFERENTIAL CROSS-SECTION CALCULATIONS AND ANALYSIS OF EXPERIMENTAL DATA FOR 232Th ». Modern Physics Letters A 19, no 21 (10 juillet 2004) : 1597–614. http://dx.doi.org/10.1142/s0217732304014136.

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In this study, neutron-emission spectra produced by (n,xn) reactions on nuclei 232 Th have been calculated. Angle-integrated cross-sections in neutron induced reactions on targets 232 Th have been calculated at the bombarding energies from 2 MeV to 18 MeV. We have investigated multiple pre-equilibrium matrix element constant from internal transition for 232 Th (n,xn) neutron emission spectra. In the calculations, the geometry dependent hybrid model and the cascade exciton model including the effects of pre-equilibrium have been used. Pre-equilibrium direct effects have been examined by using full exciton model. In addition, we have described how multiple pre-equilibrium emissions can be included in the Feshbach–Kerman–Koonin (FKK) fully quantum-mechanical theory. By analyzing (n,xn) reaction on 232 Th , with the incident energy from 2 MeV to 18 MeV, the importance of multiple pre-equilibrium emission can be seen clearly. All calculated results have been compared with experimental data. The obtained results have been discussed and compared with the available experimental data and found agreement with each other.
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24

Jain, J., J. Moreno, D. Morales, S. Davis, B. Bora, G. Avaria, M. J. Inestrosa-Izurieta et L. Soto. « Observation and interpretation of neutron origin prior to hard X rays and pinch in a hundred joules plasma focus device ». Laser and Particle Beams 35, no 4 (26 octobre 2017) : 656–62. http://dx.doi.org/10.1017/s0263034617000672.

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AbstractThe temporal correlation between neutron and hard X-ray (HXR) emissions from a hundred joules plasma focus device (PF-400J) was studied. A method, time history analysis, to estimate the time of origin of neutrons with respect to HXRs is applied. In most of the discharges, it was found that neutrons are originated before HXRs in the axial direction and after HXRs in the radial direction. In some discharges, the time difference between HXRs and neutrons origin was found large enough, so that it can be interpreted that those neutrons would have been originated before the pinch. A qualitative discussion is conjectured to explain the experimental observations.
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25

Haskell, Brynmor, Marco Antonelli et Pierre Pizzochero. « Continuous Gravitational Wave Emissions from Neutron Stars with Pinned Superfluids in the Core ». Universe 8, no 12 (24 novembre 2022) : 619. http://dx.doi.org/10.3390/universe8120619.

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We investigate the effect of a pinned superfluid component on the gravitational wave emissions of a rotating neutron star. The pinning of superfluid vortices to the flux-tubes in the outer core (where the protons are likely to form a type-II superconductor) is a possible mechanism to sustain long-lived and non-axisymmetric neutron currents in the interior, which break the axial symmetry of the unperturbed hydrostatic configuration. We consider pinning-induced perturbations to a stationary corotating configuration and determine the upper limits on the strength of gravitational wave emissions due to the pinning of vortices with a strong toroidal magnetic field of the kind predicted by recent magneto-hydrodynamic simulations of neutron star interiors. We estimate the contributions to gravitational wave emissions from both the mass and current multipole generated by the pinned vorticity in the outer core and find that the mass quadrupole can be large enough for gravitational waves to provide the dominant spindown torque in millisecond pulsars.
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26

Panikkath, Priyada, Ashwini Udupi et P. K. Sarkar. « Estimation of neutron energy distributions from prompt gamma emissions ». Nuclear Instruments and Methods in Physics Research Section A : Accelerators, Spectrometers, Detectors and Associated Equipment 871 (novembre 2017) : 83–89. http://dx.doi.org/10.1016/j.nima.2017.07.066.

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27

Sakurai, Kunitomo. « Solar Neutron Observations During the Coming Solar Maximum : A Plan on the Japan-China Collaborative Project ». International Astronomical Union Colloquium 104, no 2 (1989) : 173–76. http://dx.doi.org/10.1017/s0252921100154090.

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AbstractNeutrons are sometimes released from solar flares accompanied by generation of high energy protons and other nuclei and some of them occasionally reach the earth before they decay radioactively. Together with the satellite observations on gamma ray and neutron emissions associated with such flares, the ground-based observations of these neutrons give us a clue to understand the possible nuclear interactions of those protons and nuclei with gases ambient in the solar atmosphere. A review is given on the Japan-China collaborative program on the ground-based observations of these neutrons for the coming solar maximum, though there still remain obstacles to be resolved.
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28

Taleyarkhan, R. P., C. D. West, J. S. Cho, R. T. Lahey, R. C. Block et R. Nigmatulin. « Evidence for nuclear emissions during neutron seeded acoustic bubble cavitation ». Journal of the Acoustical Society of America 112, no 5 (novembre 2002) : 2269. http://dx.doi.org/10.1121/1.4779070.

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29

Borla, Oscar, Giuseppe Lacidogna et Alberto Carpinteri. « RETRACTED ARTICLE : Piezonuclear neutron emissions from earthquakes and volcanic eruptions ». Meccanica 50, no 6 (1 juillet 2014) : 1651. http://dx.doi.org/10.1007/s11012-014-9972-3.

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30

Bottau, V., L. Tondut, P. G. Allinei, B. Perot, C. Eleon, C. Carasco, R. De Stefano et G. Faussier. « Study of gamma-ray background noise for radioactive waste drum characterization with plastic scintillators ». EPJ Web of Conferences 225 (2020) : 05004. http://dx.doi.org/10.1051/epjconf/202022505004.

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In the framework of the radioactive waste drum characterization using neutron coincidence counting, the Nuclear Measurement Laboratory of CEA Cadarache is studying plastic scintillators as an alternative to ideal but costly 3He gas proportional counters. Plastic scintillators are at least 5 times cheaper for the same detection efficiency, and in addition, they detect fast neutrons about three orders of magnitude faster than 3He detectors. However, they are sensitive to gamma rays, which implies the necessity to identify precisely gamma background sources that may affect the useful signal. This paper presents a detailed analysis of the gamma-ray spectrum of a radioactive waste drum containing glove box filters contaminated by plutonium dioxide. Gamma emissions accompanying inelastic scattering (n,n’) and (α,n) reactions that can lead to neutron-gamma coincidences parasitizing useful coincidences from plutonium spontaneous fissions are identified. Some of these parasitic gamma rays having energies up to several MeV, we plan to reject high-energy scintillator pulses with an electronics rejection threshold above 1 MeV, which should preserve the major part of useful fission neutron pulses.
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31

Lattimer, James M. « Neutron stars are gold mines ». International Journal of Modern Physics E 26, no 01n02 (janvier 2017) : 1740014. http://dx.doi.org/10.1142/s0218301317400146.

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Neutron stars are not only mines for clues to dense matter physics but may also be the auspicious sources of half of all nuclei heavier than [Formula: see text] in the universe, including the auric isotopes. Although the cold dense matter above the nuclear saturation density cannot be directly explored in the laboratory, gilded constraints on the properties of matter from 1 to 10 times higher density can now be panned from neutron star observations. We show how upcoming observations, such as gravitational wave from mergers, precision timing of pulsars, neutrinos from neutron star birth and X-rays from bursts and thermal emissions, will provide the bullion from which further advances can be smelted.
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32

Inoue, H. « X-ray Bursting Neutron Stars ». Symposium - International Astronomical Union 125 (1987) : 233–43. http://dx.doi.org/10.1017/s0074180900160802.

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The maximum peak luminosity of the X-ray bursts from a burster is most likely interpreted as the Eddington luminosity of a helium-rich envelope surrounding a neutron star. If this interpretation is true, we can obtain a relation between the mass and the radius of the neutron star in terms of the maximum effective temperature of bursts. On the other hand, the most naive understanding of the origin of the 4.1 keV absorption line often detected in X-ray burst spectra gives us another relation of the neutron star mass with its radius. By solving two simultaneous equations, we can determine the values of the mass and the radius of the neutron star, respectively. However, the result is critical to every neutron star model currently considered.The persistent emissions from X-ray bursters are also discussed.
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Manuello Bertetto, Andrea, Battista Grosso, Roberto Ricciu et Daniele Rizzu. « Anisotropic and impulsive neutron emissions from brittle rocks under mechanical load ». Meccanica 50, no 5 (8 juillet 2014) : 1177–88. http://dx.doi.org/10.1007/s11012-014-9987-9.

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Kocharov, L. G., Jeongwoo W. Lee, H. Zirin, G. A. Kovaltsov, I. G. Usoskin, K. R. Pyle, M. A. Shea et D. F. Smart. « Neutron and electromagnetic emissions during the 1990 May 24 solar flare ». Solar Physics 155, no 1 (novembre 1994) : 149–70. http://dx.doi.org/10.1007/bf00670736.

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35

Lai, Dong, et Wynn C. G. Ho. « Matter and Radiation in Superstrong Magnetic Fields and Thermal Emission from Neutron Stars ». Symposium - International Astronomical Union 214 (2003) : 181–90. http://dx.doi.org/10.1017/s0074180900194380.

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Thermal surface emissions have now been detected from more than a dozen isolated neutron stars, including radio pulsars, radio-quiet neutron stars and magnetars. These detections can potentially provide important information on the interior physics, magnetic fields, and surface composition neutron stars. Understanding the properties of matter and radiative transfer in strong magnetic fields is essential for the proper interpretation of the observations. We review current theoretical works on modeling magnetized neutron star atmospheres/surface layers, discussing some of the novel properties of matter and radiative transfer in strong magnetic fields. Of particular interest is the effect of the strong-field vacuum polarization, which dramatically changes the radiative transfer and the emergent X-ray spectra from magnetars.
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36

Singh, N. L., et S. Mukherjee. « Effects of level density in the cross sections of (α, xn), (α, pxn), (α, 2pxn) and (α, αxn) reactions in 197Au, 181Ta, natIn and 93Nb and pre-equilibrium analysis ». Canadian Journal of Physics 87, no 9 (septembre 2009) : 1037–46. http://dx.doi.org/10.1139/p09-067.

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Excitation functions are measured for α-particle-induced reactions on 197Au, 181Ta, natIn, and 93Nb in the energy region 18 to 60 MeV using the activation method and γ-ray spectrometry. The experimental results are compared with semiclassical model codes, STAPRE, ALICE-91, and COMPLET. These models take into account compound nuclei as well as pre-equilibrium emissions. The angular momentum removal effects have also been included in the COMPLET code. The Monte Carlo simulation code PACE4 is also employed for the calculations of equilibrium cross sections. In the case of neutron emission channels, both the model codes give fairly good agreement. The COMPLET code on the other hand, explains the α-particle emission channels in a more convincing manner.
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Burge, F., G. J. Burns, R. A. Burridge, D. J. S. Findlay, D. J. Haynes, A. H. Kershaw, P. A. Masterson, R. McCrohon, G. P. Škoro et P. N. M. Wright. « Monitoring radioactive gaseous emissions from the ISIS Spallation Neutron and Muon Source ». Nuclear Instruments and Methods in Physics Research Section A : Accelerators, Spectrometers, Detectors and Associated Equipment 1013 (octobre 2021) : 165640. http://dx.doi.org/10.1016/j.nima.2021.165640.

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Sipahi, L. B., M. R. Govindaraju et D. C. Jiles. « Monitoring neutron embrittlement in nuclear pressure vessel steels using micromagnetic Barkhausen emissions ». Journal of Applied Physics 75, no 10 (15 mai 1994) : 6981–83. http://dx.doi.org/10.1063/1.356748.

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Fernandez, José Francisco, Fermin Cuevas, Miguel Algueró et Carlos Sánchez. « Experimental Investigation of Neutron Emissions during Thermal Cycling of TiDx(x≈ 2.00) ». Fusion Technology 31, no 2 (mars 1997) : 237–47. http://dx.doi.org/10.13182/fst97-a30826.

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Cárdenas, E. S., E. T. E. Reedy, H. A. Seipel, B. H. Failor et A. W. Hunt. « Comparison of fission signatures from β− delayed γ-ray and neutron emissions ». Nuclear Instruments and Methods in Physics Research Section A : Accelerators, Spectrometers, Detectors and Associated Equipment 792 (août 2015) : 67–73. http://dx.doi.org/10.1016/j.nima.2015.04.039.

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Jakubowski, L., et M. Sadowski. « Correlation of x-ray and neutron emissions from an ion implosion system ». Physics Letters A 116, no 2 (mai 1986) : 49–53. http://dx.doi.org/10.1016/0375-9601(86)90236-7.

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Carpinteri, A., O. Borla, G. Lacidogna et A. Manuello. « Neutron emissions in brittle rocks during compression tests : Monotonic vs. cyclic loading ». Physical Mesomechanics 13, no 5-6 (septembre 2010) : 268–74. http://dx.doi.org/10.1016/j.physme.2010.11.007.

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43

Chupp, Edward L., et James M. Ryan. « High energy neutron and pion-decay gamma-ray emissions from solar flares ». Research in Astronomy and Astrophysics 9, no 1 (janvier 2009) : 11–40. http://dx.doi.org/10.1088/1674-4527/9/1/003.

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44

Joseph, Deepthy Maria, Nithu Ashok et Antony Joseph. « A systematic study of proton, alpha and cluster decays in Rhenium isotopes using the effective liquid drop model ». Modern Physics Letters A 31, no 05 (5 février 2016) : 1650031. http://dx.doi.org/10.1142/s0217732316500310.

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Employing the effective liquid drop model (ELDM), half-lives of proton and alpha decays and probable cluster decays are computed and analyzed for different proton-rich and neutron-rich isotopes of Rhenium. The investigation fortifies the phenomenon of cluster radioactivity (CR) in rare earth nuclei and also affirms the pivotal role played by neutron magicity in cluster decays. ELDM data is compared with that of universal decay law (UDL) model and found to be more efficient than the latter one. Apparently, cluster emissions slacken as the neutron number of daughter nucleus goes up and the linear nature of Geiger–Nuttall (G–N) plots stays unaltered even if the surface potential is incorporated.
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Banerjee, Smaranika, Masaomi Tanaka, Kyohei Kawaguchi, Daiji Kato et Gediminas Gaigalas. « The simulations of early kilonova emission from neutron star mergers ». Proceedings of the International Astronomical Union 16, S363 (juin 2020) : 233–36. http://dx.doi.org/10.1017/s1743921322000904.

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AbstractIn the neutron-star mergers, the radioactive decay of freshly synthesized heavy elements produces emissions in the ultraviolet-optical-infrared range, producing a transient called kilonova. The observational properties of the kilonova depend on the bound-bound opacity of the heavy elements, which was largely unavailable for the conditionssuitable at an early time (t < day). In this article, I share some of our recent progress on modeling the early kilonova light curve, focusing on the atomic opacity calculation.
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Hernandez-Solis, Augusto, Klemen Ambrožič, Dušan Čalič, Luca Fiorito, Bor Kos, Marjan Kromar, Peter Schillebeeckx, Alexey Stankovskiy et Gašper Žerovnik. « BOUNDARY CONDITION MODELING EFFECT ON THE SPENT FUEL CHARACTERIZATION AND FINAL DECAY HEAT PREDICTION FROM A PWR ASSEMBLY ». EPJ Web of Conferences 247 (2021) : 12008. http://dx.doi.org/10.1051/epjconf/202124712008.

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In this paper, two main exercises have been carried out to describe the effect that varying an albedo boundary condition has in the computation of observables such as decay heat, neutron emission rate and nuclide inventory from a PWR fuel assembly (or a configuration of assemblies) during a depletion scenario. The SERPENT2 code was then employed to emphasize the importance of modeling a proper boundary condition for such purposes. Moreover, the effect of taking into account more than a single fuel-pin region for depletion studies while varying the type of boundary condition, was also accounted for. The first exercise has the main objective of comparing in a single fuel assembly the albedo variations ranging from 1.1 up to full vacuum conditions. By comparing to the reference assembly (considered to be the case of full reflective conditions), relative differences up to +17% were observed in decay heat and up to almost -30% in neutron emissions. Also, a clear dependence on the albedo was detected if more than one depletable zone was considered while computing the integral value of observables of interest. Regarding the second exercise, where a 3 × 3 configuration of fuel assemblies is being now considered with a reflector section in the middle, a negligible effect on the observables was observed for the single fuel pin zone case; instead, an effect in the 244Cm computation when analyzing two fuel pin-zones produced a change in the neutron emission rate during cooling time up to 2.5% (while comparing it to the reference single assembly case).
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47

Sumiyoshi, Kohsuke. « Numerical modeling of core-collapse supernovae and compact objects ». Proceedings of the International Astronomical Union 8, S291 (août 2012) : 67–72. http://dx.doi.org/10.1017/s1743921312023186.

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AbstractMassive stars (M ≥ 10M⊙) end their lives with spectacular explosions due to gravitational collapse. The collapse turns the stars into compact objects such as neutron stars and black holes with the ejection of cosmic rays and heavy elements. Despite the importance of these astrophysical events, the mechanism of supernova explosions has been an unsolved issue in astrophysics. This is because clarification of the supernova dynamics requires the full knowledge of nuclear and neutrino physics at extreme conditions, and large-scale numerical simulations of neutrino radiation hydrodynamics in multi-dimensions. This article is a brief overview of the understanding (with difficulty) of the supernova mechanism through the recent advance of numerical modeling at supercomputing facilities. Numerical studies with the progress of nuclear physics are applied to follow the evolution of compact objects with neutrino emissions in order to reveal the birth of pulsars/black holes from the massive stars.
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48

Carpinteri, A., G. Lacidogna, A. Manuello et O. Borla. « Energy emissions from brittle fracture : Neutron measurements and geological evidences of piezonuclear reactions ». Strength, Fracture and Complexity 7, no 1 (2011) : 13–31. http://dx.doi.org/10.3233/sfc-2011-0120.

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Paladugu, Sreya, Katharine Page, Jue Liu, Michelle Everett, Cheng Li, Peter Metz et Stephen Purdy. « Designing next-generation emissions abatement catalysts using operando neutron total scattering ». Acta Crystallographica Section A Foundations and Advances 78, a1 (29 juillet 2022) : a44. http://dx.doi.org/10.1107/s2053273322099557.

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Chupp, E. L. « High-Energy Particle Production in Solar Flares (SEP, Gamma-Ray and Neutron Emissions) ». Physica Scripta T18 (1 janvier 1987) : 5–19. http://dx.doi.org/10.1088/0031-8949/1987/t18/001.

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