Gotowe bibliografie tematyczne / Neutron Waves

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Gotowa bibliografia na temat „Neutron Waves”

Autor: Grafiati
Data publikacji: 6 września 2023

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Artykuły w czasopismach na temat "Neutron Waves"

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Aksenov, V. L., i Yu V. Nikitenko. "Neutron standing waves investigations with polarized neutrons". Physica B: Condensed Matter 267-268 (czerwiec 1999): 313–19. http://dx.doi.org/10.1016/s0921-4526(99)00023-x.

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Haidar, Nassar H. S. "Neutron density waves versus temperature waves". International Journal of Advanced Nuclear Reactor Design and Technology 3 (2021): 206–12. http://dx.doi.org/10.1016/j.jandt.2021.09.004.

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Ignatovich, V. K. "On neutron surface waves". Crystallography Reports 54, nr 1 (styczeń 2009): 116–21. http://dx.doi.org/10.1134/s1063774509010209.

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Cousin, Fabrice, i Giulia Fadda. "An introduction to neutron reflectometry". EPJ Web of Conferences 236 (2020): 04001. http://dx.doi.org/10.1051/epjconf/202023604001.

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Specular neutron reflectivity is a neutron diffraction technique that provides information about the structure of surfaces or thin films. It enables the measurement of the neutron scattering length density profile perpendicular to the plane of a surface or an interface, and thereby gives access to the profile of the chemical composition of the film. The wave-particle duality allows to describe neutrons as waves; at an interface between two media of different refractive indexes, neutrons are partially reflected and refracted by the interface. Interferences can occur between waves reflected at the top and at the bottom of a thin film at an interface, which gives rise to interference fringes in the reflectivity profile directly related to its thickness. The characteristic sizes that can be probed range from 5Å to 2000 Å. Neutron-matter interaction directly occurs between neutron and the atom nuclei, which enable to tune the contrast by isotopic substitution. This makes it particularly interesting in the fields of soft matter and biophysics. This course is composed of two parts describing respectively its principle and the experimental aspects of the method (instruments, samples). Examples of applications of neutron reflectometry in the biological domain are presented by Y. Gerelli in the book section “Applications of neutron reflectometry in biology”.
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Mamontov, Eugene, Heloisa N. Bordallo, Olivier Delaire, Jonathan Nickels, Judith Peters, Gerald J. Schneider, Jeremy C. Smith i Alexei P. Sokolov. "Broadband Wide-Angle VElocity Selector (BWAVES) neutron spectrometer designed for the SNS Second Target Station". EPJ Web of Conferences 272 (2022): 02003. http://dx.doi.org/10.1051/epjconf/202227202003.

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A recently proposed wide-angle velocity selector (WAVES) device for choosing the velocity of detected neutrons after they have been scattered by the sample paves the way for inverted geometry neutron spectrometers with continuously adjustable final neutron wavelength. BWAVES broadband inverted geometry spectrometer proposed for the Second Target Station at the Spallation Neutron Source at Oak Ridge National Laboratory is designed using WAVES to simultaneously probe dynamic processes spanning 4.5 decades in time (energy transfer). This makes BWAVES a uniquely flexible instrument which can be viewed as either a quasielasitc neutron scattering (QENS) spectrometer with a practically unlimited (overlapping with the vibrational excitations) range of energy transfers, or a broadband inelastic vibrational neutron spectrometer with QENS capabilities, including a range of accessible momentum transfer (Q) and a sufficiently high energy resolution at the elastic line. The new capabilities offered by BWAVES will expand the application of neutron scattering in ways not possible with existing neutron spectrometers.
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Voronin, Vladimir, Valery Fedorov, Sergey Semenikhin i Yaroslav Berdnikov. "Neutron spin rotation effect at Laue diffraction in a weakly deformed and nonabsorbing crystal with no center of symmetry". EPJ Web of Conferences 219 (2019): 06003. http://dx.doi.org/10.1051/epjconf/201921906003.

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The effect of the neutron spin rotation at Laue diffraction in a weakly deformed noncentrosymmetric and transparent for the neutrons crystal has been theoretically described and experimentally investigated. This effect arises in the deformed crystal because of the curvature of the neutron trajectory in the crystal. A certain type of deformation leads to the escape outside the crystal of one of the two neutron waves excited at Laue diffraction. This two waves propagate in the crystal without a center of symmetry in electric fields with the opposite sign. In this case the spin of the remaining neutron wave will be rotating relative to the original direction due to the interaction of the magnetic moment of the moving neutron with the crystal's intracrystalline electric field. In a perfect undeformed crystal such spin rotation effect is absent. There is only a depolarization of the beam since both waves in opposite electric fields are present with the same amplitudes. A technique for controlled deformation of a perfect single crystal by creating a temperature gradient has been developed. Thus a new possibility to measure the electric fields which act on the neutron in noncentrosymmetric crystals has been realized. There also appeared a way to control these fields in experiments on the study of the neutron fundamental properties.
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Mamontov, E., C. Boone, M. J. Frost, K. W. Herwig, T. Huegle, J. Y. Y. Lin, B. McCormick i in. "A concept of a broadband inverted geometry spectrometer for the Second Target Station at the Spallation Neutron Source". Review of Scientific Instruments 93, nr 4 (1.04.2022): 045101. http://dx.doi.org/10.1063/5.0086451.

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BWAVES is an acronym for Broadband Wide-Angle VElocity Selector spectrometer, indicating that a novel WAVES (Wide-Angle VElocity Selector) device will be used to select the velocity/wavelength of the detected neutrons after they are scattered by the sample. We describe a conceptual design of BWAVES, a time-of-flight broadband inverted-geometry neutron spectrometer for the Second Target Station at the Spallation Neutron Source operated by Oak Ridge National Laboratory. Being the first inverted geometry spectrometer where the energy of the detected neutrons can be chosen by a WAVES device mechanically, irrespective of the limitations imposed by the crystal analyzers or filters, BWAVES will feature a uniquely broad, continuous dynamic range of measurable energy transfers, spanning 4.5 decades. This will enable measurements of both vibrational and relaxational excitations within the same, continuous scattering spectra. Novel approaches that are necessary for the implementation of a WAVES device at the BWAVES spectrometer will result in a spectrometer with the design and characteristics much different from those displayed by the neutron spectrometers in existence today.
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Sieniawska, Magdalena, i Michał Bejger. "Continuous Gravitational Waves from Neutron Stars: Current Status and Prospects". Universe 5, nr 11 (31.10.2019): 217. http://dx.doi.org/10.3390/universe5110217.

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Gravitational waves astronomy allows us to study objects and events invisible in electromagnetic waves. It is crucial to validate the theories and models of the most mysterious and extreme matter in the Universe: the neutron stars. In addition to inspirals and mergers of neutrons stars, there are currently a few proposed mechanisms that can trigger radiation of long-lasting gravitational radiation from neutron stars, such as e.g., elastically and/or magnetically driven deformations: mountains on the stellar surface supported by the elastic strain or magnetic field, free precession, or unstable oscillation modes (e.g., the r-modes). The astrophysical motivation for continuous gravitational waves searches, current LIGO and Virgo strategies of data analysis and prospects are reviewed in this work.
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Piro, Anthony L., i Lars Bildsten. "Neutron Star Crustal Interface Waves". Astrophysical Journal 619, nr 2 (luty 2005): 1054–63. http://dx.doi.org/10.1086/426682.

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Andersson, Nils. "Gravitational waves from neutron stars". Proceedings of the International Astronomical Union 5, H15 (listopad 2009): 137–40. http://dx.doi.org/10.1017/s1743921310008525.

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AbstractIn this presentation, I will outline some of the different ways that neutron stars can generate gravitational waves, discuss recent improvements in modeling the relevant scenarios in the context of improving detector sensitivity, and show how observations are beginning to put interesting “constraints” on our theoretical models.
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Rozprawy doktorskie na temat "Neutron Waves"

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Lee, Wai-Tung. "Neutron scalar Aharonov-Bohm effect and spin density waves in chromium /". free to MU campus, to others for purchase, 1998. http://wwwlib.umi.com/cr/mo/fullcit?p9901258.

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Haskell, Brynmor Dylan Luigi. "Gravitational waves from deformed rotating neutron stars". Thesis, University of Southampton, 2007. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.438658.

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Tennant, David Alan. "Neutron scattering studies of spin waves and spinons". Thesis, University of Oxford, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.259852.

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GILIBERTI, ELIA. "ON NEUTRON STARS'CRUST BREAKING AND GRAVITATIONAL WAVES EMISSION". Doctoral thesis, Università degli Studi di Milano, 2020. http://hdl.handle.net/2434/704603.

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Many different astrophysical events related to pulsars are taught to be due to starquakes, that could be caused by various possible loadings acting on the crust. However, at the present time, there is still a lack of theoretical well based modelling for most of these loadings and, therefore, we have only a very rough knowledge of the physics of neutron stars’ crust response. This PhD work wants to be a first development of a quite realistic calculation of the effects of chosen loadings, being that the forces due to uniform rotation, differential rotation or pinning, on the crust of pulsars. A Newtonian model, already used in Geophysics, has been adapted to the very different physical conditions of neutron stars’ physics and used to describe self-gravitating neutron stars, both in the incompressible and compressible scenario, subjected to different kinds of loadings. In particular, the deformations due to uniform rotation, differential rotation and slack pinning are studied. It is found that the response of the star is very sensitive to the adiabatic index value, while it is weakly influenced by the stellar mass. In all the cases, the strain developed between two glitches is found to be insufficient to break the crust, a result that challenges the standard picture of pulsar glitches based on crustquakes. Finally, attention is focused on accreting neutron stars in low-mass X-ray binaries and millisecond pulsars. The scenario is the following: the star spins up due to the accretion of matter thus building up stress; the mass quadrupole moment associated with crustal failures leads to the emission of gravitational waves which, in turn, spins down the star until equilibrium. The equilibrium frequency calculated is found compatible with observations. It is also argued that these gravitational waves could be potentially detected by the LIGO-Virgo interferometers in the near future.
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Bastarrika, Mikel. "Bayesian analysis of burst gravitational waves from galactic neutron stars". Thesis, University of Glasgow, 2010. http://theses.gla.ac.uk/2363/.

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This thesis summarises my work in relation to data analysis for gravitational wave detection. Most of the personal contribution relates to the assessment of the detectability of potential burst-type gravitational wave signals from the galactic population of neutron stars and to the parameter estimation of the models used to represent these signals. A small part of the work, confined to the last chapter, describes the experimental work carried at the beginning of the research period and aimed to measure the shot-noise level of the modulated laser-light in the gravitational wave detectors. Chapter 1 is introductory and presents generic information about gravitational wave radiation, a postulate of the theory of general relativity. The polarisation of the radiation and the approximate values of amplitudes and frequencies of the signals expected from astrophysical events are presented, together with most important gravitational radiation sources for ground-based detectors. Chapter 2 presents the study on the detectability of burst-type gravitational wave signals incoming from neutron stars located in our galaxy. Three differently shaped galactic neutron star populations are introduced and the detectability of ground-based detectors to signals of different polarisation degree coming from these source populations is investigated. Based on the time- and polarisation-averaged antenna pattern and antenna power values, approximated by Monte Carlo methods, detectability is measured in terms of a) the geographical location and orientation of hypothetical detectors, and b) the current detectors, either working individually or as a part of a network. Also, the sidereal times at which each detector is more sensitive to the sources of the neutron star populations defined are inferred. Chapter 3 introduces a mathematical model of the burst-type gravitational wave ringdown signal investigated in this work, which represents a short-lived gravitational polarised radiation generated by an oscillating neutron star: an exponentially damped sinusoid comprised of a sine and a cosine component, of the same frequency but different amplitude, as the two polarisation components of the signal. The model of the signal is given, in the time- and in the frequency-domain. Chapter 4 is devoted to present the Bayesian probability tools necessary to carry out ‘model comparison’ and ‘parameter estimation’ for the detectability study of our particular burst-type signal. Comparison of models allows choosing the one that better represents the data and subsequently focusing on in order to compute the most likely parameter values of that model. Also, in this section, the way in which the detector data can be simulated in the frequency domain, combining the signal and a noise realisation corresponding to the power spectrum of the noise that characterizes the detector, is explained. The likelihood function for a signal corresponding to one oscillation mode and seen by one detector is derived both in the time- and in the frequency-domain. The nested sampling technique is summarised, a useful tool to compute effectively the marginal likelihood of the hypotheses considered. Chapter 5 presents the results of the model selection and the parameter estimation exercise. The expression of the likelihood is generalised so that it can adopt more than one oscillation mode and been seen by various detectors of a network. Depending whether one, f-mode, or two oscillation modes, f and p, are suspect, two different scenarios of various hypotheses are considered. For each hypothesis the minimum strength of the signal to claim detection is studied and a parameter estimation exercise is carried out to characterise the signal and define the location of the source in the sky. Signals of known parameters and differing strengths were injected into the synthetic noise of three advanced detectors comprising a network. The values of the parameters were estimated using Bayesian inference for two different scenarios: when only the f-mode is suspect (scenario 1), or when both f- and p-modes are suspect (scenario 2). Posterior probabilities of the parameters in Scenario 1 are better defined and constrained than those for Scenario 2, due to the added uncertainty of including another oscillation mode. As expected, the uncertainty of the probability distributions of the parameter values decreases and the mode shifts toward the exact injected value as the signal strength increases. For both scenarios the frequency value can be accurately estimated, but not so well the damping time, especially for the p-mode oscillation, which is suspected to have longer time durations than f-modes, typically several seconds. The ability to estimate the polarisation degree of the signal is also quite limited and strong signals are required for the mode of the distribution to approximate the exact value. Similarly, determining the most probable location for the source is possible in both scenarios. The two-fold degeneracy of the sky position and related to the travel time of the signal to the detectors has been broken; relatively strong (high SNR) signals, especially for scenario 2, are needed for the source location to be constrained with accuracy. Chapter 6 presents the experimental work carried out, by which the measuring of the shot-noise level of differently modulated and demodulated laser light was intended. Due to the poor outcome of this experiment and the lack of useful results the emphasis has been placed on a detailed description of the modulation apparatus, opto-electronic set up and the control system put together. Chapter 7 looks to the future and briefly presents how to take this data analysis work forward.
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Vinciguerra, Serena. "Studying neutron-star and black-hole binaries with gravitational-waves". Thesis, University of Birmingham, 2018. http://etheses.bham.ac.uk//id/eprint/8159/.

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The revolutionary discoveries of the last few years have opened a new era of astronomy. With the detection of gravitational-waves, we now have the opportunity of investigating new phenomena, such as mergers of black-holes. Furthermore, multi-messenger observations now allow us to combine information from different channels, providing insight into the physics involved. With this rapid evolution and growth of the field, many challenges need to be faced. In this thesis we propose three data analysis strategies to efficiently study the coalescences of compact binaries. First we propose an algorithm to reduce the computational cost of Bayesian inference on gravitational-wave signals. Second we prove that machine-learning signal classification could enhance the significance of gravitational-wave candidates in unmodelled searches for transients. Finally we develop a tool, saprEMo, to predict the number of electromagnetic events, which according to a specific emission model, should be present in a particular survey.
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Santiago, Prieto Ricardo Ignacio. "Transient gravitational waves at r-mode frequencies from neutron stars". Thesis, University of Glasgow, 2014. http://theses.gla.ac.uk/5530/.

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A search for long transient gravitational waves associated with neutron stars is presented. The estimated length of these sources is from hours to weeks. Two types of astrophysical sources are considered: pulsar timing glitches associated with r-modes oscillations in the interior of isolated neutron stars, and Type I X-Ray bursts in neutron stars from binary systems. These signals follow the model of an e-folding sinusoid signal with a duration dependant on dissipation processes in the interior of the neutron stars and the gravitational radiation reaction. Estimations of the timescales of gravitational wave signals emitted by stable stars are presented. From this study, it is concluded that detecting signals from faster spinning neutron stars is more feasible than from slower neutron stars. The study of this type of transient gravitational wave signals is explored for the first time using an adaptation of the F-statistic gravitational wave search method used regularly in continuous gravitational wave searches. This adaptation, proposed by Prix et al, is a search methodology in which the duration of a signal plays a significant role in its detection. This code is part of the LAL/LAL-apps data analysis algorithm libraries of the LIGO and VIRGO scientific collaborations (LVC). The use of this method in the gravitational wave search presented in this thesis was implemented in two different environments: gaussian noise data and data in gravitational wave detector-like noise. For the latter, injections of long transient signals with durations ∼ 10,000 s on the LVC Engineering Run 3 were done. A comparison between the results obtained in these two studies is presented. It shows that, by having a good characterisation of unwanted noise lines, it is possible to distinguish the frequency of the injected signal within a small search band of only a few frequency bins. On the other hand, the recovery of the duration of the signal would require a broad search band over time. This estimation is set to be approximately ±τ, where τ is the damping time of the injected signal, in order to construct a complete τ distribution. For example, for a signal that last ∼ 3.5 days, an total τ interval of ∼ 6.5 − 7 days is required.
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González, Boquera Claudia. "Neutron-rich matter in atomic nuclei and neutron stars". Doctoral thesis, Universitat de Barcelona, 2020. http://hdl.handle.net/10803/668774.

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The proper understanding of the equation of state (EoS) of highly asymmetric nuclear matter is essential when studying systems such as neutron stars (NSs). Using zero-range Skyrme interactions and finite-range interactions such as Gogny forces, momentum-dependent interactions (MDI) and simple effective interactions (SEI), we analyze the properties of the EoS and the influence they may have on the calculations for NSs. We start by studying the convergence properties of the Taylor series expansion of EoS in powers of the isospin asymmetry. Next, we analyze the accuracy of the results for β-stable nuclear matter, which is found in the interior of NSs, when it is computed using the Taylor expansion of the EoS. The agreement with the results obtained using the full expression of the EoS is better for interactions with small-to-moderate values of the slope of the symmetry energy L. The mass and radius relation for a NS is obtained by integrating the so-called Tolman-Oppenheimer-Volkoff (TOV) equations, where the input is the EoS of the system. We have studied the mass-radius relation for Skyrme and Gogny interactions, and we see that that very soft forces are not able to give stable solutions of the TOV equations and only the stiff enough parametrizations can provide 2M0 NSs. We also notice that none of the existing parametrizations of the standard Gogny D1 interaction is able to provide a NS inside the observational constraints. Because of that, we propose a new parametrization, which we name D1M∗, that is able to provide NSs of 2M0 while still providing the same good description of finite nuclei as D1M. A parametrization D1M∗∗ is also presented, which is fitted in the same way as D1M∗ and provides NSs up to 1.91M0. Moreover, we estimate the core-crust transition in NSs by finding where the nuclear matter in the core is unstable against fluctuations of the density. To do that, we employ two methods, the thermodynamical method and the dynamical method. In the case of finite-range interactions, such as the Gogny ones, to use the dynamical method we have had to derive the explicit expression of the energy curvature matrix in momentum space for this type of interactions. We observe a decreasing trend of the transition density with the slope L of the symmetry energy, while the correlation between the transition pressure and L is much lower. Finally different NS properties are studied. The crustal properties, such as the crustal mass, crustal thickness and crustal fraction of the moment of inertial have lower values if one computes them using the core-crust transition density obtained with the dynamical method instead of the one obtained with the thermodynamical method, pointing out the importance of the accurate evaluation of the transition density when studying observational phenomena. We have also studied the moment of inertia of NSs, which is compared to constraints proposed in the literature. Finally, the tidal deformability for NSs is also calculated and compared with the constraints coming from the GW170817 event detected by the LIGO and Virgo observatories and which accounts for the merger of two NSs in a binary system.
El coneixement de l’equació d’estat (EoS) de matèria altament densa i assimètrica és essencial per tal d’estudiar les estrelles de neutrons (NSs). En aquesta tesi s’analitzen, utilitzant interaccions de camp mig no relativistes, les propietats de l’EoS i la seva influència en càlculs de NSs. Primerament, s’estudia la convergència del desenvolupament en sèrie de Taylor de l’EoS en potències de l'assimetria d’isospí. Seguidament, s’analitza l’exactitud dels resultats per matèria β-estable, la qual es troba a l’interior de les NSs, quan es calcula utilitzant el desenvolupament de Taylor de l’EoS. La relació entre la massa i el radi obtinguda integrant les equacions Tolman-Oppenheimer-Volkoff (TOV) també és estudiada. A causa de que les interaccions de Gogny de la família D1 no aconsegueixen donar NSs compatibles amb observacions astrofísiques, en aquesta tesi proposem dues noves forces de Gogny, anomenades D1M∗ i D1M∗∗, les quals poden donar, respectivament, NSs de 2 i 1.91 masses solars. Una altra part de la tesi es dedica a l’estudi de la transició entre l’escorça i el nucli, buscant la densitat a la qual la matèria uniforme al nucli és inestable contra fluctuacions de densitat. Ho estudiem amb dos mètodes, el mètode termodinàmic i el mètode dinàmic. Finalment, s’analitzen diverses propietats de les NSs, com són la relació entre la massa i el radi de l’estrella, les propietats de l’escorça, el moment d’inèrcia, així com la deformació deguda als corrents de marea (tidal deformability) que està relacionada amb l’emissió d’ones gravitacionals en sistemes binaris d’estrelles de neutrons.
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Clark, Michael C. "Bowen-type initial data for simulations of neutron stars in binary systems". Diss., Georgia Institute of Technology, 2016. http://hdl.handle.net/1853/55005.

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A new method for generating initial data for simulations of neutron stars in binary systems. The construction of physically relevant initial data is crucial to accurate assessment of gravitational wave signals relative to theoretical predictions. This method builds upon the Bowen-York curvature for puncture black holes. This data is evolved and compared against simulations in the literature with respect to orbital eccentricity, merger and collapse times, and emitted energy and angular momentum. The data exhibits some defects, including large central density oscillations in stars and center of mass drift in unequal-mass systems. Some approaches for improvements in potential future work are discussed.
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Ashton, Gregory. "Timing variations in neutron stars : models, inference and their implications for gravitational waves". Thesis, University of Southampton, 2016. https://eprints.soton.ac.uk/401822/.

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Timing variations in pulsars, low frequency ubiquitous structure known as timing noise and sudden increases in the rotational frequency which we call glitches, provide a means to study neutron stars. Since the first observations, many models have been proposed, yet no definitive explanation has arisen. In this thesis, we aim to improve this situation by developing models of timing noise. We focus chiefly on precession models which explain periodic modulation seen in radio pulsar data. Developing models and testing them provides an opportunity to infer the elemental properties of neutron stars: evidence for long period precession has implications for the superfluid component predicted by models used to explain glitches. However, often more than one model can qualitatively explain the data, therefore we need a method to decide which model best fits the data. This is precisely the case for PSR B1828-11 which has been used as evidence for both precession and so-called magnetospheric switching. We address this confusion by applying the tools of probability theory to develop a Bayesian model comparison and find that the evidence is in favour of precession. In the second part of this thesis, we will discuss the implications of timing variations for the detection of continuous gravitational waves from neutron stars. To search for these signals, matched filtering methods are used which require a template, a guess for what the signal ‘looks like’. Timing variations, as seen in the electromagnetic signal, may also exist in the gravitational wave signal. If detected, these could provide an invaluable source of information about neutron stars. However, if not included in the template, they may mean that the gravitational wave signal is not detected in the first place. We investigate this issue for both timing noise and glitches, using electromagnetic observations to predict for what types of gravitational wave searches this may be an issue. We find that while timing noise is unlikely to be an issue for current gravitational wave searches, glitches may cause a significant problem in all-sky searches for gravitational waves from neutron stars.
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Książki na temat "Neutron Waves"

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Peter, Mészáros, Begelman Mitchell C i United States. National Aeronautics and Space Administration., red. Why 'galactic' gamma-ray bursts might depend on environment: Blast waves around neutron stars. [Washington, DC: National Aeronautics and Space Administration, 1994.

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Peter, Mészáros, Begelman Mitchell C i United States. National Aeronautics and Space Administration., red. Why 'galactic' gamma-ray bursts might depend on environment: Blast waves around neutron stars. [Washington, DC: National Aeronautics and Space Administration, 1994.

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Peter, Mészáros, Begelman Mitchell C i United States. National Aeronautics and Space Administration., red. Why 'galactic' gamma-ray bursts might depend on environment: Blast waves around neutron stars. [Washington, DC: National Aeronautics and Space Administration, 1994.

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International, School on Nuclear Physics Neutron Physics and Nuclear Energy (8th 1987 Varna Bulgaria). Nuclei, neutrons, and energy: Proceedings of the VIII International School on Nuclear Physics, Neutron Physics, and Nuclear Energy, Varna, Bulgaria, 19-28 Nov. 1987. Singapore: World Scientific, 1988.

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Rubinstein, Robert. Non-ideal gas effects on shock waves in weakly ionized gases. Hampton, VA: Institute for Computer Applications in Science and Engineering, NASA Langley Research Center, 2000.

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Rubinstein, Robert. Non-ideal gas effects on shock waves in weakly ionized gases. Hampton, VA: Institute for Computer Applications in Science and Engineering, NASA Langley Research Center, 2000.

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Rubinstein, Robert. Non-ideal gas effects on shock waves in weakly ionized gases. Hampton, VA: Institute for Computer Applications in Science and Engineering, NASA Langley Research Center, 2000.

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Rubinstein, Robert. Non-ideal gas effects on shock waves in weakly ionized gases. Hampton, VA: Institute for Computer Applications in Science and Engineering, NASA Langley Research Center, 2000.

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Rubinstein, Robert. Non-ideal gas effects on shock waves in weakly ionized gases. Hampton, VA: Institute for Computer Applications in Science and Engineering, NASA Langley Research Center, 2000.

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Rubinstein, Robert. Non-ideal gas effects on shock waves in weakly ionized gases. Hampton, VA: Institute for Computer Applications in Science and Engineering, NASA Langley Research Center, 2000.

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Części książek na temat "Neutron Waves"

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Feldbaum, David M. "Neutron Stars". W Gravitational Waves: An Overview, 83–84. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-031-02613-3_15.

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Rauch, Helmut. "Quantum Neutron Optics". W Waves and Particles in Light and Matter, 99–123. Boston, MA: Springer US, 1994. http://dx.doi.org/10.1007/978-1-4615-2550-9_9.

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Patel, J. R. "X-Ray Standing Waves". W X-Ray and Neutron Dynamical Diffraction, 211–24. Boston, MA: Springer US, 1996. http://dx.doi.org/10.1007/978-1-4615-5879-8_14.

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Lagomarsino, S. "Long-Period X-Ray Standing Waves". W X-Ray and Neutron Dynamical Diffraction, 249–58. Boston, MA: Springer US, 1996. http://dx.doi.org/10.1007/978-1-4615-5879-8_17.

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Haskell, Brynmor, Nils Andersson, Caroline D‘Angelo, Nathalie Degenaar, Kostas Glampedakis, Wynn C. G. Ho, Paul D. Lasky i in. "Gravitational Waves from Rapidly Rotating Neutron Stars". W Gravitational Wave Astrophysics, 85–102. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-10488-1_8.

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Wood, Kent S. "Neutron Stars, X-Rays, and Gravitational Waves". W Cosmic Gamma Rays, Neutrinos, and Related Astrophysics, 609–16. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0921-2_42.

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Escribe-Filippini, C., J. P. Pouget, R. Currat, B. Hennion i J. Marcus. "Neutron studies of the blue bronzes K0.3MoO3 and Rb0.3MoO3". W Charge Density Waves in Solids, 71–75. Berlin, Heidelberg: Springer Berlin Heidelberg, 1985. http://dx.doi.org/10.1007/3-540-13913-3_187.

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Sá, Paulo M., i Brigitte Tomé. "Gravitational waves from r-modes". W Isolated Neutron Stars: From the Surface to the Interior, 557–61. Dordrecht: Springer Netherlands, 2007. http://dx.doi.org/10.1007/978-1-4020-5998-8_75.

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Patel, J. R., i E. Fontes. "X Ray Standing Waves: Thermal Vibration Amplitudes at Surfaces". W X-Ray and Neutron Dynamical Diffraction, 235–47. Boston, MA: Springer US, 1996. http://dx.doi.org/10.1007/978-1-4615-5879-8_16.

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Hinderer, Tanja, Luciano Rezzolla i Luca Baiotti. "Gravitational Waves from Merging Binary Neutron-Star Systems". W The Physics and Astrophysics of Neutron Stars, 575–635. Cham: Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-97616-7_10.

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Streszczenia konferencji na temat "Neutron Waves"

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Pushin, Dmitry, Dusan Sarenac, Charles W. Clark, David G. Cory, Connor Kapahi, Benjamin Heacock, Michael G. Huber, Joachim Nsofini i Chandra B. Shahi. "Structured neutron waves". W Optical, Opto-Atomic, and Entanglement-Enhanced Precision Metrology, redaktorzy Selim M. Shahriar i Jacob Scheuer. SPIE, 2019. http://dx.doi.org/10.1117/12.2515469.

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Perego, Albino. "Matter ejection and kilonova emission from binary neutron star mergers". W Gravitational-waves Science&Technology Symposium. Trieste, Italy: Sissa Medialab, 2018. http://dx.doi.org/10.22323/1.325.0033.

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Owen, Benjamin J. "Gravitational waves from the r-modes of rapidly rotating neutron stars". W Third edoardo amaldi conference on gravitational waves. AIP, 2000. http://dx.doi.org/10.1063/1.1291840.

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Buchenau, U. "Neutron scattering from low-frequency excitations in a-sio2". W 1987 Twelth International Conference on Infrared and Millimeter Waves. IEEE, 1987. http://dx.doi.org/10.1109/irmm.1987.9126972.

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Sekiguchi, Yuichiro. "Exploring Physics of Neutron Star Matter by Gravitational Waves". W Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017). Journal of the Physical Society of Japan, 2018. http://dx.doi.org/10.7566/jpscp.20.011045.

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Benhar, O. "Gravitational waves from neutron stars described by modern EOS". W GENERAL RELATIVITY AND GRAVITATIONAL PHYSICS: 16th SIGRAV Conference on General Relativity and Gravitational Physics. AIP, 2005. http://dx.doi.org/10.1063/1.1891555.

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Wylde, Richard, Jonas Kindervater, Stuart Froud, Randolph Hammond i Collin Broholm. "Electron spin resonance to enhance neutron scattering measurements". W 2017 42nd International Conference on Infrared, Millimeter, and Terahertz Waves (IRMMW-THz). IEEE, 2017. http://dx.doi.org/10.1109/irmmw-thz.2017.8066933.

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Lai, Dong. "Secular bar-mode evolution and gravitational waves from neutron stars". W Workshop on astrophysical sources for ground-based gravitational wave detectors. AIP, 2001. http://dx.doi.org/10.1063/1.1387316.

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Gabbiani, F. "Effective Field Theory for Neutron-Deuteron Scattering: Higher Partial Waves". W Theory and Experiment III. WORLD SCIENTIFIC, 2001. http://dx.doi.org/10.1142/9789812810977_0089.

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Kamitakahara, W. A., P. Boolchand i R. L. Cappelletti. "Vibrational densities of states for glassy se-ge alloys by neutron scattering". W 1987 Twelth International Conference on Infrared and Millimeter Waves. IEEE, 1987. http://dx.doi.org/10.1109/irmm.1987.9126973.

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Raporty organizacyjne na temat "Neutron Waves"

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Yousef, Shahinaz, Zeinab A. Mabrouk i Mostafa Kamal Ahmed. Evolution of the binary neutron star system PSR1913+16 due to gravitational waves emission. MTPR Journal, grudzień 2016. http://dx.doi.org/10.19138/mtpr/(16)11-19.

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Clauser, John F. Neutral Atom deBroglie-Wave Interferometry. Fort Belvoir, VA: Defense Technical Information Center, styczeń 1990. http://dx.doi.org/10.21236/ada231301.

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Clauser, John F. Neutral Atom deBroglie-Wave Interferometry. Fort Belvoir, VA: Defense Technical Information Center, lipiec 1990. http://dx.doi.org/10.21236/ada226085.

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Clauser, John F. Neutral Atom deBroglie-Wave Interferometry. Fort Belvoir, VA: Defense Technical Information Center, listopad 1990. http://dx.doi.org/10.21236/ada229368.

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Mughabghab, S. F. What Do s- and p-Wave Neutron Average Radiative Widths Reveal. Office of Scientific and Technical Information (OSTI), kwiecień 2010. http://dx.doi.org/10.2172/1013497.

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Vidnovic, Theodore, III. Di-Neutral Pion Production in the Triplet P Wave States of Charmonium. Office of Scientific and Technical Information (OSTI), grudzień 2002. http://dx.doi.org/10.2172/1420946.

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Manheimer, Wallace M. A Simple Scheme for Implementing Wave Absorption in Quasi-Neutral PIC Simulations of ECR Plasma. Fort Belvoir, VA: Defense Technical Information Center, styczeń 1998. http://dx.doi.org/10.21236/ada336333.

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watts, Christopher. Coupling of the Photosphere to the Solar Corona: A laboratory and observational study of Alfv?n wave interaction with a neutral gas. Office of Scientific and Technical Information (OSTI), styczeń 2010. http://dx.doi.org/10.2172/972630.

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Fritts, D. C. Gravity Wave Dynamics and Tidal Interactions in the MLT and at the Bottomside F Layer and Their Potential Contributions to Neutral and Plasma Dynamics. Fort Belvoir, VA: Defense Technical Information Center, kwiecień 2012. http://dx.doi.org/10.21236/ada559865.

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UK, Ipsos. Survey of public attitudes towards precision breeding. Food Standards Agency, październik 2022. http://dx.doi.org/10.46756/sci.fsa.ouv127.

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Streszczenie:
The Genetic Technology (Precision Breeding) Bill is currently going through Parliament. Although this bill is ‘England only’ and food and feed safety and hygiene is a devolved issue, the Food Standards Agency (FSA) will introduce a separate regulatory framework for precision bred organisms (PBOs), should the Bill become law. The FSA will also work with stakeholders in Scotland, Wales and Northern Ireland to ensure consumers’ interests are protected in relation to PBOs. The FSA / Food Standard Scotland (FSS) is science and evidence led. In August 2022, the FSA and FSS commissioned Ipsos UK to conduct a two-phase social research project on precision breeding. Phase One, now complete, involved a survey of 4,177 UK residents with robust samples in each UK nation to allow comparisons between and within nations. Phase Two, scheduled to start in September 2022 and report in early 2023, will comprise a series of Citizens’ Forums in England, Wales and Northern Ireland(footnote 1). The overall aims of this project are to: explore consumer attitudes towards precision breeding gather consumer views on the FSA’s proposed regulatory framework understand consumer information needs inform how to communicate with consumers about precision breeding. This document presents interim findings for this project, reporting descriptive data from Phase One. Phase One’s core aims were to provide a snapshot of consumers’ awareness and self-assessed knowledge of precision breeding, its perceived acceptability, risks and benefits, and consumer appetite for information about this production method. These data show that awareness of precision breeding is very low, something which should be borne in mind when considering these findings. While these data reveal that there is a general openness to trying precision bred foods across the UK, with more people anticipating benefits than disbenefits from the use of precision breeding, there is a large degree of uncertainty about what impact precision bred foods may have on the different parts of the food system. This is reflected in the relatively large proportions of people taking a neutral stance or indicating they do not know enough to answer survey questions and in the strong appetite expressed for information about precision breeding to be provided. The next phase of this project will be essential for the FSA’s ability to interpret these findings’ implications, and to understand what is informing consumers’ views. The purpose of Phase One has always been to let the FSA know ‘what’ consumers think about precision breeding; Phase Two’s purpose is to build our understanding ‘why’ they think it. This will allow the FSA to develop a more nuanced understanding of consumers’ needs and incorporate this into the design of the future regulatory framework and any engagement with consumers on precision breeding. FSS will be carrying out further research in Scotland.
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