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Автор: Grafiati

Опубліковано: 6 вересня 2023

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1

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

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2

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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3

Ignatovich, V. K. "On neutron surface waves." Crystallography Reports 54, no. 1 (January 2009): 116–21. http://dx.doi.org/10.1134/s1063774509010209.

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4

Cousin, Fabrice, and 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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Анотація:

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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5

Mamontov, Eugene, Heloisa N. Bordallo, Olivier Delaire, Jonathan Nickels, Judith Peters, Gerald J. Schneider, Jeremy C. Smith, and 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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6

Voronin, Vladimir, Valery Fedorov, Sergey Semenikhin, and 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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7

Mamontov, E., C. Boone, M. J. Frost, K. W. Herwig, T. Huegle, J. Y. Y. Lin, B. McCormick, et al. "A concept of a broadband inverted geometry spectrometer for the Second Target Station at the Spallation Neutron Source." Review of Scientific Instruments 93, no. 4 (April 1, 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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8

Sieniawska, Magdalena, and Michał Bejger. "Continuous Gravitational Waves from Neutron Stars: Current Status and Prospects." Universe 5, no. 11 (October 31, 2019): 217. http://dx.doi.org/10.3390/universe5110217.

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Анотація:

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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9

Piro, Anthony L., and Lars Bildsten. "Neutron Star Crustal Interface Waves." Astrophysical Journal 619, no. 2 (February 2005): 1054–63. http://dx.doi.org/10.1086/426682.

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10

Andersson, Nils. "Gravitational waves from neutron stars." Proceedings of the International Astronomical Union 5, H15 (November 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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11

Schutz, Bernard F. "Gravitational Waves and Neutron Stars." International Astronomical Union Colloquium 177 (2000): 727–32. http://dx.doi.org/10.1017/s0252921100061078.

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AbstractThe first generation of laser-interferomteric gravitational wave observatories will make intensive searches for gravitational radiation from spinning neutron stars. Sensitivity to a number of possible sources, including the Crab pulsar, will be better than any existing observational limits, and will improve dramatically over the next decade. This paper reviews these developments and expectations, and discusses ways in which pulsar radio astronomers and gravitational wave astronomers can benefit from one another’s work.

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12

Dzyublik, A. Ya, V. I. Slisenko, and V. V. Mykhaylovskyy. "Symmetric Laue Diffraction of Spherical Neutron Waves in Absorbing Crystals." Ukrainian Journal of Physics 63, no. 2 (March 2, 2018): 174. http://dx.doi.org/10.15407/ujpe63.2.174.

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Well-known Kato's theory of the Laue diffraction of spherical x-ray waves is generalized to the case of the neutron diffraction in strongly absorbing crystals, taking into consideration both the potential and the resonant scattering of neutrons by nuclei. The saddle-point method is applied for estimation of the angular integrals, being more adequate in the case of strongly absorbing crystals than the stationary-phase approximation used by Kato. It is found that the distribution of intensity of diffracted and refracted beams along the basis of the Borrmann triangle strongly depends on the deviation of the neutron energy from the nuclear resonant level.

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13

Lee, Chang-Hwan. "Gravitational waves from neutron star binaries." International Journal of Modern Physics E 26, no. 01n02 (January 2017): 1740015. http://dx.doi.org/10.1142/s0218301317400158.

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With H. A. Bethe, G. E. Brown worked on the merger rate of neutron star binaries for the gravitational wave detection. Their prediction has to be modified significantly due to the observations of [Formula: see text] neutron stars and the detection of gravitational waves. There still, however, remains a possibility that neutron star-low mass black hole binaries are significant sources of gravitational waves for the ground-based detectors. In this paper, I review the evolution of neutron star binaries with super-Eddington accretion and discuss the future prospect.

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14

Leinson, L. B. "Neutrino emission from spin waves in neutron spin-triplet superfluid." Physics Letters B 689, no. 2-3 (May 2010): 60–65. http://dx.doi.org/10.1016/j.physletb.2010.04.046.

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15

Nosov, V. G., and A. I. Frank. "Superslow neutrons and the dispersion law for neutron waves in matter." Physical Review A 55, no. 2 (February 1, 1997): 1129–39. http://dx.doi.org/10.1103/physreva.55.1129.

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16

HOROWITZ, C. J. "MULTI-MESSENGER OBSERVATIONS OF NEUTRON-RICH MATTER." International Journal of Modern Physics E 20, no. 10 (October 2011): 2077–100. http://dx.doi.org/10.1142/s0218301311020332.

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Анотація:

At very high densities, electrons react with protons to form neutron-rich matter. This material is central to many fundamental questions in nuclear physics and astrophysics. Moreover, neutron-rich matter is being studied with an extraordinary variety of new tools such as Facility for Rare Isotope Beams (FRIB) and the Laser Interferometer Gravitational Wave Observatory (LIGO). We describe the Lead Radius Experiment (PREX) that uses parity violating electron scattering to measure the neutron radius in 208Pb. This has important implications for neutron stars and their crusts. We discuss X-ray observations of neutron star radii. These also have important implications for neutron-rich matter. Gravitational waves (GW) open a new window on neutron-rich matter. They come from sources such as neutron star mergers, rotating neutron star mountains, and collective r-mode oscillations. Using large scale molecular dynamics simulations, we find neutron star crust to be very strong. It can support mountains on rotating neutron stars large enough to generate detectable gravitational waves. Finally, neutrinos from core collapse supernovae (SN) provide another, qualitatively different probe of neutron-rich matter. Neutrinos escape from the surface of last scattering known as the neutrino-sphere. This is a low density warm gas of neutron-rich matter. Neutrino-sphere conditions can be simulated in the laboratory with heavy ion collisions. Observations of neutrinos can probe nucleosyntheses in SN. Simulations of SN depend on the equation of state (EOS) of neutron-rich matter. We discuss a new EOS based on virial and relativistic mean field calculations. We believe that combing astronomical observations using photons, GW, and neutrinos, with laboratory experiments on nuclei, heavy ion collisions, and radioactive beams will fundamentally advance our knowledge of compact objects in the heavens, the dense phases of QCD, the origin of the elements, and of neutron-rich matter.

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17

Futakawa, Masatoshi. "Proton Bombardment in Mercury Target for Neutron Production - Impact Dynamics on Interface between Liquid and Solid Metals." Applied Mechanics and Materials 566 (June 2014): 26–33. http://dx.doi.org/10.4028/www.scientific.net/amm.566.26.

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Innovative researches using neutrons are being performed at the Materials & Life Science Experimental Facility (MLF) in the Japan Proton Accelerator Research Complex (J-PARC), in which a mercury target system is installed as MW-class pulse spallation neutron sources. In order to produce neutrons by the spallation reaction, proton beams are injected into the mercury target. At the moment when the intense proton beam hits the target, pressure waves are generated in mercury because of abrupt heat deposition. The pressure waves interact with the target vessel leading to negative pressure that may cause cavitation along the vessel wall, i.e. the interface between liquid and solid metals. Localized impacts by microjets and/or shock waves that are caused by cavitation bubble collapse impose pitting damage on the vessel wall. The pitting damage that degrades the structural integrity of the target vessel is a crucial issue for the high power mercury targets. Therefore, the mitigation techniques for the pitting damages and cavitation are needed to reach the MW-class pulsed spallation neutron sources.

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18

Hanauske, Matthias, and Lukas R. Weih. "Neutron star collisions and gravitational waves." Astronomische Nachrichten 342, no. 5 (June 2021): 788–98. http://dx.doi.org/10.1002/asna.202113994.

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19

Aksenov, V. L., V. K. Ignatovich, and Yu V. Nikitenko. "Neutron standing waves in layered systems." Crystallography Reports 51, no. 5 (October 2006): 734–53. http://dx.doi.org/10.1134/s1063774506050038.

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20

Hamilton, W. A., A. G. Klein, G. I. Opat, and P. A. Timmins. "Neutron diffraction by surface acoustic waves." Physical Review Letters 58, no. 26 (June 29, 1987): 2770–73. http://dx.doi.org/10.1103/physrevlett.58.2770.

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21

Giampieri, G. "Gravitational waves from Galactic neutron stars." Monthly Notices of the Royal Astronomical Society 292, no. 2 (December 1997): 218–24. http://dx.doi.org/10.1093/mnras/292.2.218.

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22

Melatos, A. "Gravitational waves from accreting neutron stars." Advances in Space Research 40, no. 10 (January 2007): 1472–79. http://dx.doi.org/10.1016/j.asr.2007.04.020.

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23

ZHUGE, XING, JOAN CENTRELLA, and STEPHEN MCMILLAN. "Gravitational Waves from Coalescing Neutron Stars." Annals of the New York Academy of Sciences 759, no. 1 (September 1995): 503–6. http://dx.doi.org/10.1111/j.1749-6632.1995.tb17595.x.

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24

Rauch, H. "The neutron hidden in quantum waves." Journal of Optics B: Quantum and Semiclassical Optics 4, no. 4 (August 1, 2002): S318—S323. http://dx.doi.org/10.1088/1464-4266/4/4/314.

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25

Kokkotas, Kostas D., Erich Gaertig, and Antonella Colaiuda. "Neutron star dynamics and gravitational waves." Journal of Physics: Conference Series 222 (April 1, 2010): 012031. http://dx.doi.org/10.1088/1742-6596/222/1/012031.

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26

Soldateschi, Jacopo, and Niccolò Bucciantini. "Detectability of Continuous Gravitational Waves from Magnetically Deformed Neutron Stars." Galaxies 9, no. 4 (November 10, 2021): 101. http://dx.doi.org/10.3390/galaxies9040101.

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Neutron stars are known to contain extremely powerful magnetic fields. Their effect is to deform the shape of the star, leading to the potential emission of continuous gravitational waves. The magnetic deformation of neutron stars, however, depends on the geometry and strength of their internal magnetic field as well as on their composition, described by the equation of state. Unfortunately, both the configuration of the magnetic field and the equation of state of neutron stars are unknown, and assessing the detectability of continuous gravitational waves from neutron stars suffers from these uncertainties. Using our recent results relating the magnetic deformation of a neutron star to its mass and radius—based on models with realistic equations of state currently allowed by observational and nuclear physics constraints—and considering the Galactic pulsar population, we assess the detectability of continuous gravitational waves from pulsars in the galaxy by current and future gravitational waves detectors.

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27

Ho, Wynn C. G. "Gravitational waves from neutron stars and asteroseismology." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 376, no. 2120 (April 16, 2018): 20170285. http://dx.doi.org/10.1098/rsta.2017.0285.

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Neutron stars are born in the supernova explosion of massive stars. Neutron stars rotate as stably as atomic clocks and possess densities exceeding that of atomic nuclei and magnetic fields millions to billions of times stronger than those created in laboratories on the Earth. The physical properties of neutron stars are determined by many areas of fundamental physics, and detection of gravitational waves can provide invaluable insights into our understanding of these areas. Here, we describe some of the physics and astrophysics of neutron stars and how traditional electromagnetic wave observations provide clues to the sorts of gravitational waves we expect from these stars. We pay particular attention to neutron star fluid oscillations, examining their impact on electromagnetic and gravitational wave observations when these stars are in a wide binary or isolated system, then during binary inspiral right before merger, and finally at times soon after merger. This article is part of a discussion meeting issue ‘The promises of gravitational-wave astronomy’.

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28

Kim, Myungkuk, Chang-Hwan Lee, Young-Min Kim, Kyujin Kwak, Yeunhwan Lim, and Chang Ho Hyun. "Neutron star equations of state and their applications." International Journal of Modern Physics E 29, no. 07 (July 2020): 2030007. http://dx.doi.org/10.1142/s0218301320300076.

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This paper reviews the properties of neutron stars based on the recent multi-messenger observations including electromagnetic waves from the low-mass X-ray binaries and gravitational waves from the merger of neutron star binaries. Based on these observations, we investigate theoretical models for dense nuclear matter and discuss their implications to the neutron star observations such as mass, radius, cooling, and tidal deformability. We also discuss the uncertainties in the neutron star cooling, neutron star properties with Bayesian approaches, and an expansion scheme applied to the nuclear energy density functional theory.

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29

ANDREEV, P. A., and L. S. KUZ'MENKOV. "WAVES OF MAGNETIC MOMENT AND GENERATION OF WAVES BY NEUTRON BEAM IN QUANTUM MAGNETIZED PLASMA." International Journal of Modern Physics B 26, no. 32 (December 11, 2012): 1250186. http://dx.doi.org/10.1142/s021797921250186x.

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This paper is devoted to studying of dispersion of waves in the magnetized plasma with the spin and exploring of new methods of the generation wave in the plasma. We consider the dispersion of waves, existed in the plasma in consequence of dynamic of the magnetic moments. It is shown there are nine new waves in the magnetized plasma because of the magnetic moments dynamic. We show there are instabilities at propagation of the neutron beam through the plasma. Increments of instabilities caused by neutron beam are calculated. For studying of this effects we generalize and use the method of the many-particle quantum hydrodynamics. Described processes can play important role at calculation of the stability and the safeness of the nuclear reactors and the studying of the processes in the atmosphere of the neutron stars.

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30

Yi, Tong, Fang Geng, and Mao Xinjie. "The X-ray Radiation Mechanism of the Compact (Neutron) Binary Stars." Symposium - International Astronomical Union 125 (1987): 249. http://dx.doi.org/10.1017/s0074180900160851.

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Usually we think a X-ray source may be a compact(neutron) binary star on which the X-ray radiation might be generated by gravitational acceleration for the particles coming from the primary and going along magnetic field lines of the compact star to the poles. But, in the past, people don't consider well the problem of particle acceleration. It seems to be simplified for the situation only to consider the gravitation effect, because some electric-magnetic effect in a strong magnetic field could not be neglected. However, it is unreasonable to neglect the plasma turbulent waves in an electric-magnetic field, because strong enough turbulent waves such as Alfven waves, whistlers generated nearby the surface of neutron stars probably contribute energy to accelerate particles, which may be more important than gravitation sometimes. For a binary system with a neutron star if ion number density N > 1017 /cm3 in its surface atmosphere, the turbulent wavess will be stimulated that will accelerate the particles reaching a speed over 108cm/s. they strike the atmosphere of the compact star in the system, so that a shock wave is formed which turns part of kinetic energy to heat to form hot spots of about 108K to emit X-ray.

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31

Jones, D. I., and N. Andersson. "Gravitational waves from freely precessing neutron stars." Monthly Notices of the Royal Astronomical Society 331, no. 1 (March 2002): 203–20. http://dx.doi.org/10.1046/j.1365-8711.2002.05180.x.

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32

Jones, D. I. "Gravitational waves from rotating strained neutron stars." Classical and Quantum Gravity 19, no. 7 (March 12, 2002): 1255–65. http://dx.doi.org/10.1088/0264-9381/19/7/304.

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33

Ferrari, V., L. Gualtieri, J. A. Pons, and A. Stavridis. "Gravitational waves from rotating proto-neutron stars." Classical and Quantum Gravity 21, no. 5 (February 5, 2004): S515—S519. http://dx.doi.org/10.1088/0264-9381/21/5/019.

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34

Lasky, Paul D., Burkhard Zink, and Kostas D. Kokkotas. "Gravitational waves from strongly magnetised neutron stars." Journal of Physics: Conference Series 363 (June 1, 2012): 012020. http://dx.doi.org/10.1088/1742-6596/363/1/012020.

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35

Watts, Anna L., and Badri Krishnan. "Detecting gravitational waves from accreting neutron stars." Advances in Space Research 43, no. 7 (April 2009): 1049–54. http://dx.doi.org/10.1016/j.asr.2009.01.006.

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36

Antia, M. "ASTROPHYSICS: Neutron Stars Spin Out Gravity Waves." Science 280, no. 5371 (June 19, 1998): 1835a—1835. http://dx.doi.org/10.1126/science.280.5371.1835a.

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37

BENHAR, OMAR. "NEUTRON STAR MATTER EQUATION OF STATE AND GRAVITATIONAL WAVE EMISSION." Modern Physics Letters A 20, no. 31 (October 10, 2005): 2335–49. http://dx.doi.org/10.1142/s0217732305018335.

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Анотація:

The EOS of strongly interacting matter at densities ten to fifteen orders of magnitude larger than the typical density of terrestrial macroscopic objects determines a number of neutron star properties, including the pattern of gravitational waves emitted following the excitation of nonradial oscillation modes. This paper reviews some of the approaches employed to model neutron star matter, as well as the prospects for obtaining new insights from the experimental study of gravitational waves emitted by neutron stars.

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38

Nimtz, Guenter, and Paul Bruney. "On the Universal Scattering Time of Neutrons." Zeitschrift für Naturforschung A 73, no. 10 (October 25, 2018): 919–21. http://dx.doi.org/10.1515/zna-2018-0331.

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AbstractTunnelling and barrier interaction times of neutrons were previously measured. Here we show that the neutron interaction time with barriers corresponds to the universal tunnelling time of wave mechanics which was formerly observed with elastic, electromagnetic and electron waves. The universal tunnelling time seems to hold for neutrons also. Such an adequate general wave mechanical behaviour was conjectured by Brillouin. Remarkably, wave mechanical effects, and even virtual particles, hold from the microcosm to the macrocosm.

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39

Riles, Keith. "Recent searches for continuous gravitational waves." Modern Physics Letters A 32, no. 39 (December 21, 2017): 1730035. http://dx.doi.org/10.1142/s021773231730035x.

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Gravitational wave astronomy opened dramatically in September 2015 with the LIGO discovery of a distant and massive binary black hole coalescence. The more recent discovery of a binary neutron star merger, followed by a gamma ray burst (GRB) and a kilonova, reinforces the excitement of this new era, in which we may soon see other sources of gravitational waves, including continuous, nearly monochromatic signals. Potential continuous wave (CW) sources include rapidly spinning galactic neutron stars and more exotic possibilities, such as emission from axion Bose Einstein “clouds” surrounding black holes. Recent searches in Advanced LIGO data are presented, and prospects for more sensitive future searches are discussed.

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40

Guetta, Dafne. "Multimessenger Probes of High-energy Sources." EPJ Web of Conferences 209 (2019): 01036. http://dx.doi.org/10.1051/epjconf/201920901036.

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Multimessenger observations may hold the key to learn about the most energetic sources in the universe. The recent construction of large scale observatories opened new possibilities in testing non thermal cosmic processes with alternative probes, such as high energy neutrinos and gravitational waves. We propose to combine information from gravitational wave detections, neutrino observations and electromagnetic signals to obtain a comprehensive picture of some of the most extreme cosmic processes. Gravitational waves are indicative of source dynamics, such as the formation, evolution and interaction of compact objects. These compact objects can play an important role in astrophysical particle acceleration, and are interesting candidates for neutrino and in general high-energy astroparticle studies. In particular we will concentrate on the most promising gravitational wave emitter sources: compact stellar remnants. The merger of binary black holes, binary neutron stars or black hole-neutron star binaries are abundant gravitational wave sources and will likely make up the majority of detections. However, stellar core collapse with rapidly rotating core may also be significant gravitational wave emitter, while slower rotating cores may be detectable only at closer distances. The joint detection of gravitational waves and neutrinos from these sources will probe the physics of the sources and will be a smoking gun of the presence of hadrons in these objects which is still an open question. Conversely, the non-detection of neutrinos or gravitational waves from these sources will be fundamental to constrain the hadronic content.

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41

Hanauske, Matthias, Luke Bovard, Elias Most, Jens Papenfort, Jan Steinheimer, Anton Motornenko, Volodymyr Vovchenko, Veronica Dexheimer, Stefan Schramm, and Horst Stöcker. "Detecting the Hadron-Quark Phase Transition with Gravitational Waves." Universe 5, no. 6 (June 20, 2019): 156. http://dx.doi.org/10.3390/universe5060156.

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The long-awaited detection of a gravitational wave from the merger of a binary neutron star in August 2017 (GW170817) marks the beginning of the new field of multi-messenger gravitational wave astronomy. By exploiting the extracted tidal deformations of the two neutron stars from the late inspiral phase of GW170817, it is now possible to constrain several global properties of the equation of state of neutron star matter. However, the most interesting part of the high density and temperature regime of the equation of state is solely imprinted in the post-merger gravitational wave emission from the remnant hypermassive/supramassive neutron star. This regime was not observed in GW170817, but will possibly be detected in forthcoming events within the current observing run of the LIGO/VIRGO collaboration. Numerous numerical-relativity simulations of merging neutron star binaries have been performed during the last decades, and the emitted gravitational wave profiles and the interior structure of the generated remnants have been analysed in detail. The consequences of a potential appearance of a hadron-quark phase transition in the interior region of the produced hypermassive neutron star and the evolution of its underlying matter in the phase diagram of quantum cromo dynamics will be in the focus of this article. It will be shown that the different density/temperature regions of the equation of state can be severely constrained by a measurement of the spectral properties of the emitted post-merger gravitational wave signal from a future binary compact star merger event.

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42

BASTRUKOV, S., I. MOLODTSOVA, J. YANG, and V. PAPOYAN. "PULSATING NEUTRON STAR AS A SOURCE OF QUASISTATIC WAVES OF GRAVITY IN INTERSTELLAR MEDIUM." International Journal of Modern Physics A 20, no. 32 (December 30, 2005): 7593–602. http://dx.doi.org/10.1142/s0217751x05025425.

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The hydrodynamic waves of gravity in the galactic interstellar medium generated by a pulsating neutron star are discussed in this paper. It is shown that the frequency of oscillations of interstellar gas–dust matter in this wave is proportional to that for the g-mode in the neutron star bulk. The corresponding periods are of the millisecond duration. The collective oscillations of charged species in the interstellar wave of gravity can produce electromagnetic radiation, and that the only radio waves of this radiation can freely travel through the galactic gas–dust clouds, suggests that this kind of interstellar waves can manifest itself in the radio range of spectra of a neutron star undergoing pulsations triggered by starquake. This inference is in line with the statement that quasiperiodic micropulses with a time scale of a few milliseconds located in the windows of the main pulse train of the radio pulsar spectra owe their origin to pulsations of neutron stars.

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43

Chen, Hsin-Yu, and Katerina Chatziioannou. "Distinguishing Binary Neutron Star from Neutron Star–Black Hole Mergers with Gravitational Waves." Astrophysical Journal 893, no. 2 (April 22, 2020): L41. http://dx.doi.org/10.3847/2041-8213/ab86bc.

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44

Bushuev, V. A., and A. I. Frank. "Goos–Hänchen effect in neutron optics and the reflection time of neutron waves." Physics-Uspekhi 61, no. 10 (October 31, 2018): 952–64. http://dx.doi.org/10.3367/ufne.2017.11.038235.

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45

Hasegawa, Yuji, Claus Schmitzer, Hannes Bartosik, Jürgen Klepp, Stephan Sponar, Katharina Durstberger-Rennhofer, and Gerald Badurek. "Falsification of Leggett's model using neutron matter waves." New Journal of Physics 14, no. 2 (February 17, 2012): 023039. http://dx.doi.org/10.1088/1367-2630/14/2/023039.

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46

Nelson, Ann E., Sanjay Reddy, and Dake Zhou. "Dark halos around neutron stars and gravitational waves." Journal of Cosmology and Astroparticle Physics 2019, no. 07 (July 4, 2019): 012. http://dx.doi.org/10.1088/1475-7516/2019/07/012.

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47

Ferrari, V., G. Miniutti, and J. A. Pons. "Gravitational waves from newly born, hot neutron stars." Monthly Notices of the Royal Astronomical Society 342, no. 2 (June 21, 2003): 629–38. http://dx.doi.org/10.1046/j.1365-8711.2003.06580.x.

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48

Piro, Anthony L., and Eric Thrane. "GRAVITATIONAL WAVES FROM FALLBACK ACCRETION ONTO NEUTRON STARS." Astrophysical Journal 761, no. 1 (November 21, 2012): 63. http://dx.doi.org/10.1088/0004-637x/761/1/63.

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49

Chattopadhyay, Debatri, Simon Stevenson, Jarrod R. Hurley, Luca J. Rossi, and Chris Flynn. "Modelling double neutron stars: radio and gravitational waves." Monthly Notices of the Royal Astronomical Society 494, no. 2 (March 19, 2020): 1587–610. http://dx.doi.org/10.1093/mnras/staa756.

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ABSTRACT We have implemented prescriptions for modelling pulsars in the rapid binary population synthesis code Compact Object Mergers: Population Astrophysics and Statistics. We perform a detailed analysis of the double neutron star (DNS) population, accounting for radio survey selection effects. The surface magnetic field decay time-scale (∼1000 Myr) and mass-scale (∼0.02 M⊙) are the dominant uncertainties in our model. Mass accretion during common envelope evolution plays a non-trivial role in recycling pulsars. We find a best-fitting model that is in broad agreement with the observed Galactic DNS population. Though the pulsar parameters (period and period derivative) are strongly biased by radio selection effects, the observed orbital parameters (orbital period and eccentricity) closely represent the intrinsic distributions. The number of radio observable DNSs in the Milky Way at present is about 2500 in our model, corresponding to approximately 10 per cent of the predicted total number of DNSs in the Galaxy. Using our model calibrated to the Galactic DNS population, we make predictions for DNS mergers observed in gravitational waves. The DNS chirp mass distribution varies from 1.1 to 2.1 M⊙ and the median is found to be 1.14 M⊙. The expected effective spin χeff for isolated DNSs is ≲0.03 from our model. We predict that 34 per cent of the current Galactic isolated DNSs will merge within a Hubble time, and have a median total mass of 2.7 M⊙. Finally, we discuss implications for fast radio bursts and post-merger remnant gravitational waves.

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50

Zhu, Xing-Jiang, and Gregory Ashton. "Characterizing Astrophysical Binary Neutron Stars with Gravitational Waves." Astrophysical Journal 902, no. 1 (October 7, 2020): L12. http://dx.doi.org/10.3847/2041-8213/abb6ea.

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