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Journal articles on the topic 'Lorentz factor'

Author: Grafiati

Published: 2 June 2025

Last updated: 31 July 2025

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1

Martinez Viladesau, Enrique. "Theory of relativity: Analysis of Lorentz transformation and ‎Lorentz factor." International Journal of Fundamental Physical Sciences 8, no. 3 (2018): 87–91. http://dx.doi.org/10.14331/ijfps.2012.330118.

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2

Martinez Viladesau, Enrique. "Theory of relativity: Analysis of Lorentz transformation and Lorentz factor." International Journal of Fundamental Physical Sciences 8, no. 3 (2018): 87–91. http://dx.doi.org/10.14331/ijfps.2018.330118.

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3

Yinghua, W. "Lorentz–polarization factor for correction of diffraction-line profiles." Journal of Applied Crystallography 20, no. 3 (1987): 258–59. http://dx.doi.org/10.1107/s0021889887086746.

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The Lorentz–polarization factor (1 + cos22 θ)/sin2 θ cos θ for the integrated intensity of a diffraction line is different from the Lorentz–polarization factor (1 + cos2 2θ)/sin2 θ for a diffraction-line profile; nevertheless, in most of the literature it is being used to correct diffraction-line profiles. The errors introduced in the peak shape and position by use of the Lorentz–polarization factor (1 + cos2 2θ)/sin2 θ cos θ are discussed.

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4

Li, Jing, Da-Bin Lin, Rui-Jing Lu, et al. "Jets in a Gamma-Ray Burst during Its Prompt Emission: Evolution of the Lorentz Factor." Astrophysical Journal 943, no. 2 (2023): 145. http://dx.doi.org/10.3847/1538-4357/aca96a.

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Abstract Knowledge about the Lorentz factor and its evolution of relativistic jets in gamma-ray bursts (GRBs) is crucial to understand their physics. An exact value of the bulk Lorentz factor can be estimated based on a high-energy spectral cutoff, which may appear in the GRBs’ prompt emission owing to the absorption of photon–photon pair production. In this work, we focus on an investigation of the bulk Lorentz factor evolution of jets in an individual burst. Based on Fermi observations, we search for bursts with multiple GRB pulses characterized by a high-energy spectral cutoff, and nine GRB

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5

Klinaku, Shukri. "Light clock and the Lorentz factor." Physics Essays 28, no. 4 (2015): 488–90. http://dx.doi.org/10.4006/0836-1398-28.4.488.

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6

Yang, JiangHe, JunHui Fan, and YuHai Yuan. "Lorentz factor estimation for radio sources." Science China Physics, Mechanics and Astronomy 55, no. 8 (2012): 1510–14. http://dx.doi.org/10.1007/s11433-011-4807-x.

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7

Gao, Duan-Yuan, and Yuan-Chuan Zou. "Jet Lorentz Factor Constraint for GRB 221009A Based on the Optical Depth of the TeV Photons." Astrophysical Journal Letters 956, no. 2 (2023): L38. http://dx.doi.org/10.3847/2041-8213/acfed1.

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Abstract The recent detection of teraelectronvolt (TeV) photons from the record-breaking gamma-ray burst GRB 221009A during its prompt phase poses challenges for constraining its Lorentz factor. We reevaluate the constraints on the jet Lorentz factor considering a two-zone model, wherein the TeV photons originate from the external shock region while the lower-energy MeV photons come from the internal prompt emission region. By properly accounting for the evolution of the MeV photon spectrum and light curve, we calculate the optical depth for TeV photons and derive a minimum Lorentz factor of a

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8

Al-Ameen, Talal, Maythem Mahmud, and Imad Muhi. "Can Newtonian kinetic energy and Einsteinian rest-mass energy be expressed by the binomial expansion of the Lorentz factor? And how valid is using Einstein’s E = mc² to calculate the nuclear fission energy?" Journal of Physics: Conference Series 2793, no. 1 (2024): 012002. http://dx.doi.org/10.1088/1742-6596/2793/1/012002.

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Abstract The binomial (Taylor) expansion of the Lorentz factor has been reconsidered here in an attempt to find out whether the Newtonian kinetic energy and the Einsteinian rest-mass energy are implicitly embedded in the mathematical structure of the binomial expansion of the Lorentz factor (as Einstein postulated in his Special Theory of Relativity). Advocates of Standard Special Relativity show that it is possible to obtain these two kinds of energy by multiplying both sides of the expansion of the Lorentz factor by the moving object’s rest mass m 0 and the square of the speed of light c 2.

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9

McPherson, J. W. "Increases in Lorentz Factor with Dielectric Thickness." World Journal of Condensed Matter Physics 06, no. 02 (2016): 152–68. http://dx.doi.org/10.4236/wjcmp.2016.62018.

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10

Kim, Young S. "Lorentz coherence and the proton form factor." Physica Scripta 90, no. 7 (2015): 074037. http://dx.doi.org/10.1088/0031-8949/90/7/074037.

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11

Broomfield, H., J. Hirst, M. Raven, et al. "Testing the validity of the Lorentz factor." Physics Education 53, no. 5 (2018): 055011. http://dx.doi.org/10.1088/1361-6552/aaccdb.

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12

Lange, J. "The Lorentz factor for the Laue technique." Acta Crystallographica Section A Foundations of Crystallography 51, no. 4 (1995): 559–65. http://dx.doi.org/10.1107/s0108767395001358.

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13

Onuchukwu, Chika Christian, and Augustine A. Ubachukwu. "On the Lorentz factor of superluminal sources." Research in Astronomy and Astrophysics 13, no. 5 (2013): 509–16. http://dx.doi.org/10.1088/1674-4527/13/5/002.

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14

VLAHAKIS, NEKTARIOS. "MAGNETOHYDRODYNAMIC MODELING OF RELATIVISTIC OUTFLOWS." International Journal of Modern Physics D 17, no. 10 (2008): 1661–68. http://dx.doi.org/10.1142/s0218271808013273.

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The main characteristics of relativistic, steady, ideal magnetohydrodynamic (MHD) outflows are discussed, focusing on their bulk acceleration and collimation. It is shown that the Bernoulli equation relates the bulk Lorentz factor with the shape of the flow, permitting an analytic estimation of the acceleration efficiency, while the transfield force-balance equation gives a simple relation of the bulk Lorentz factor to the distance.

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15

Onuchukwu, C. C., and A. A. Ubachukwu. "Doppler factor, Lorentz factor and viewing angle of superluminal quasars." Astrophysics and Space Science 348, no. 1 (2013): 193–98. http://dx.doi.org/10.1007/s10509-013-1549-4.

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16

Lee, Jeffrey S., and Gerald B. Cleaver. "Ultra-relativistic thermodynamics and aberrations of the cosmic microwave background radiation." Modern Physics Letters A 30, no. 09 (2015): 1550045. http://dx.doi.org/10.1142/s0217732315500455.

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Ultra-relativistic inertial and non-inertial reference frames would be subjected to a forward-directed heat bath from the Lorentz transformed temperature of the Cosmic Microwave Background (CMB) radiation. Although the Lorentz transformations of heat and temperature continue to be unresolved issues in the literature,1–6 this paper makes use of occupation number (number density of occupied states per phase space element) to support a Lorentz factor inflation of the rest frame temperature. Additionally, Doppler Boosting is examined.

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17

Berisha, Valbone, and Shukri Klinaku. "The law of cosines and the Lorentz factor." Physics Essays 31, no. 4 (2018): 383–86. http://dx.doi.org/10.4006/0836-1398-31.4.383.

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18

Zevin, L. "Lorentz factor for oriented samples in powder diffractometry." Acta Crystallographica Section A Foundations of Crystallography 46, no. 9 (1990): 730–34. http://dx.doi.org/10.1107/s0108767390004676.

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19

Логинов, С. С., та С. П. Шоркин. "Псевдослучайные числа на основе системы Лоренца в методе селективного отображения снижения пик-фактора сигналов с ортогональным частотным мультиплексированием". Vestnik of Volga State University of Technology. Series Radio Engineering and Infocommunication Systems, № 4(60) (16 лютого 2024): 33–40. https://doi.org/10.25686/2306-2819.2023.4.33.

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В данной статье представлены результаты моделирования псевдослучайных чисел на основе системы Лоренца в методе селективного отображения снижения пик-фактора сигналов с ортогональным частотным мультиплексированием (OFDM). Проведено исследование влияния псевдослучайных чисел, формируемых на основе цифровой реализации системы Лоренца с динамическим хаосом, на эффективность снижения пик-фактора сигналов с ортогональным частотным мультиплексированием в методе селективного отображения и выполнен сравнительный анализ снижения пик-фактора сигналов метода селективного отображения (SLM) с использованием

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20

Zhang, Xing-Fu, Ruo-Yu Liu, Hai-Ming Zhang, Yi-Yun Huang, B. Theodore Zhang, and Xiang-Yu Wang. "Constraints on Cosmic-Ray Acceleration in Bright Gamma-Ray Bursts with Observations of Fermi." Astrophysical Journal 980, no. 2 (2025): 188. https://doi.org/10.3847/1538-4357/ada941.

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Abstract Gamma-ray bursts (GRBs) are widely suggested as potential sources of ultrahigh-energy cosmic rays. The kinetic energy of the jets dissipates, leading to the production of an enormous amount of gamma-ray photons and possibly also the acceleration of protons. The accelerated protons will interact with the radiation of the GRB via the photomeson and Bethe–Heitler processes, which can initiate electromagnetic cascades. This process can give rise to broadband radiation up to the GeV–TeV gamma-ray regime. The expected gamma-ray flux from cascades depends on the properties of the GRB jet, su

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21

Miodrag, Mateljević. "Lorentz Transformation and time dilatation." Annals of Mathematics and Physics 7, no. 1 (2024): 016–22. http://dx.doi.org/10.17352/amp.000104.

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We consider two inertial frames S and and suppose that frame moves, for simplicity, in a single direction: the X -direction of frame S with a constant velocity v as measured in frame S. Using homogeneity of space and time we derive a modified Lorentz Transformation (LT) between two inertial reference frames without using the second postulate of Einstein, i.e., we do not assume the invariant speed of light (in vacuum) under LT. Roughly speaking we suppose: (H) Any clock which is at rest in its frame measures a small increment of time by some factor s=s(v). As a corollary of relativity theory (H

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22

Cantor, Jerome. "Is the Lorentz Factor a Probability Function in Superfluid Spacetime?" Applied Physics Research 8, no. 3 (2016): 1. http://dx.doi.org/10.5539/apr.v8n3p1.

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<p class="1Body">A number of studies indicate that spacetime may have properties resembling that of a superfluid, suggesting that percolation theory may provide a useful approach to studying the relationship between velocity and time. By hypothesizing that the effect described by the Lorentz factor may represent an increase in the viscosity of spacetime, it was possible to model time dilation in terms of the movement of a fluid through porous media. Using a random resistor network to equate superfluid percolation with conductance, it is shown that the Lorentz factor corresponds to a prob

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23

Putra, Fima Ardianto. "De Broglie Wave Analysis of the Heisenberg Uncertainty Minimum Limit under the Lorentz Transformation." Jurnal Teras Fisika 1, no. 2 (2018): 1. http://dx.doi.org/10.20884/1.jtf.2018.1.2.1008.

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A simple analysis using differential calculus has been done to consider the minimum limit of the Heisenberg uncertainty principle in the relativistic domain. An analysis is made by expressing the form of and based on the Lorentz transformation, and their corresponding relation according to the de Broglie wave packet modification. The result shows that in the relativistic domain, the minimum limit of the Heisenberg uncertainty is p x ?/2 and/or E t ?/2, with is the Lorentz factor which depend on the average/group velocity of relativistic de Broglie wave packet. While, the minimum limit accordin

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24

MILLAS, D., G. KATSOULAKOS, D. LINGRI, K. KARAMPELAS, and N. VLAHAKIS. "SOLUTIONS OF THE WIND EQUATION IN RELATIVISTIC MAGNETIZED JETS." International Journal of Modern Physics: Conference Series 28 (January 2014): 1460200. http://dx.doi.org/10.1142/s2010194514602002.

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We study the bulk acceleration in relativistic axisymmetric magnetized outflows, by solving the momentum equation along the flow, the so-called wind equation. The solutions for the bulk Lorentz factor depend on the geometry of the field/streamlines through the "bunching function" S. We investigate the general characteristics of the S function and how its choice affects the acceleration. In our study, various fast rise and slow decay examples are selected for S, with a global maximum near the fast magnetosonic critical point, as required from the regularity condition. For each case we determine

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25

Zdziarski, Andrzej A., Alexandra J. Tetarenko, and Marek Sikora. "Jet Parameters in the Black Hole X-Ray Binary MAXI J1820+070." Astrophysical Journal 925, no. 2 (2022): 189. http://dx.doi.org/10.3847/1538-4357/ac38a9.

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Abstract We study the jet in the hard state of the accreting black hole (BH) binary MAXI J1820+070. From the available radio-to-optical spectral and variability data, we put strong constraints on the jet parameters. We find while it is not possible to uniquely determine the jet Lorentz factor from the spectral and variability properties alone, we can estimate the jet opening angle (≈1.°5 ± 1°), the distance at which the jet starts emitting synchrotron radiation (∼3 × 1010 cm), and the magnetic field strength there (∼104 G), with relatively low uncertainty, as they depend weakly on the bulk Lor

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26

Malzac, Julien, and Samia Drappeau. "Spectra and fast multi-wavelength variability of compact jets powered by internal shocks." Proceedings of the International Astronomical Union 10, S313 (2014): 159–63. http://dx.doi.org/10.1017/s1743921315002112.

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AbstractThe emission of steady compact jets observed in the hard spectral state of X-ray binaries is likely to be powered by internal shocks caused by fluctuations of the outflow velocity. The dynamics of the internal shocks and the resulting spectral energy distribution (SED) of the jet is very sensitive to the shape of the Power Spectral Density (PSD) of the fluctuations of the jet Lorentz factor. It turns out that Lorentz factor fluctuations injected at the base of the jet with a flicker noise power spectrum (i.e. P(f) ∝1/f) naturally produce the canonical flat SED observed from radio to IR

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27

Vejnovic, Zdravko, Milos Pavlovic, Marina Kutin, and Milorad Davidovic. "Glow curve analysis by Gauss-Lorentz function." Nuclear Technology and Radiation Protection 28, no. 1 (2013): 45–51. http://dx.doi.org/10.2298/ntrp1301045v.

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A new method for fitting glow curves, described in a mixed order kinetics model, with Gauss-Lorentz function is shown. Theoretical expressions of the mixed order kinetics model are shown in a new way, so that the values of kinetic parameters can be obtained through the geometric parameters. When the model is described in this way it is possible to calculate precisely the kinetic parameters such as activation energy, pre-exponential factor and the factor a= n0/(h + n0). At the same time, obtained values of geometric parameters of the experimental curve, which is described with the Gauss-Lorentz

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28

Wakely, Scott P. "Transition radiation response over large ranges of Lorentz factor." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 522, no. 1-2 (2004): 16–18. http://dx.doi.org/10.1016/j.nima.2004.01.011.

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29

Blinov, L. M., V. V. Lazarev, S. P. Palto, and S. G. Yudin. "Optical probe, local fields, and Lorentz factor in ferroelectrics." JETP Letters 99, no. 8 (2014): 441–45. http://dx.doi.org/10.1134/s0021364014080050.

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30

Egelstaff, P. A., O. J. Eder, W. Glaser, J. Polo, B. Renker, and A. K. Soper. "Dynamic-structure-factor measurements on a model Lorentz gas." Physical Review A 41, no. 4 (1990): 1936–42. http://dx.doi.org/10.1103/physreva.41.1936.

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31

Plyatsko, R. M., and M. T. Fenyk. "On Reaction of a Spinning Particle on the Spacetime Curvature." Ukrainian Journal of Physics 64, no. 11 (2019): 1059. http://dx.doi.org/10.15407/ujpe64.11.1059.

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The reaction of a classical (nonquantum) spinning particle on the spacetime curvature according to the Mathisson–Papapetrou equations is analyzed. From the point of view of the observer comoving with the particle in Schwarzschild’s field, this reaction is a reaction on the gravitomagnetic components of the gravitational field. The values of these components significantly depend on the relativistic Lorentz factor calculated by the particle velocity relative to the Schwarzschild mass. As a result, the value of the spinning particle acceleration relative to the geodesic motion is proportional to

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32

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

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The emission of a charged light lepton pair by a superluminal neutrino has been identified as a major factor in the energy loss of highly energetic neutrinos. The observation of PeV neutrinos by IceCube implies their stability against lepton pair Cerenkov radiation. Under the assumption of a Lorentz-violating dispersion relation for highly energetic superluminal neutrinos, one may thus constrain the Lorentz-violating parameters. A kinematically different situation arises when one assumes a Lorentz-covariant, space-like dispersion relation for hypothetical tachyonic neutrinos, as an alternative

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33

CHICONE, C., B. MASHHOON, and B. PUNSLY. "DYNAMICS OF RELATIVISTIC FLOWS." International Journal of Modern Physics D 13, no. 05 (2004): 945–59. http://dx.doi.org/10.1142/s0218271804004992.

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Dynamics of relativistic outflows along the rotation axis of a Kerr black hole is investigated using a simple model that takes into account the relativistic tidal force of the central source as well as the Lorentz force due to the large-scale electromagnetic field which is assumed to be present in the ambient medium. The evolution of the speed of the flow relative to the ambient medium is studied. In the force-free case, the resulting equation of motion predicts rapid deceleration of the initial flow and an asymptotic relative speed with a Lorentz factor of [Formula: see text]. In the presence

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34

Koide, Shinji, Kazunari Shibata, and Takahiro Kudoh. "General Relativistic Simulation of Jet Formation from Magnetized Accretion Disk." International Astronomical Union Colloquium 163 (1997): 667–71. http://dx.doi.org/10.1017/s0252921100043360.

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AbstractRecently, superluminal motions are observed not only from active galactic nuclei but also in our Galaxy. These phenomena are explained as relativistic jets propagating almost toward us with Lorentz factor more than 2. For the formation of such a relativistic jet, magnetically driven mechanism around a black hole is most promising. We have extended the 2.5D Newtonian MHD jet model (Shibata & Uchida 1986) to general relativistic regime. For this purpose, we have developed a general relativistic magnetohydrodynamic (GRMHD) numerical code and applied it to the simulation of the magneti

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35

Guo, Wen-Di, Qin Tan, and Yu-Xiao Liu. "Quasinormal modes and greybody factor of a Lorentz-violating black hole." Journal of Cosmology and Astroparticle Physics 2024, no. 07 (2024): 008. http://dx.doi.org/10.1088/1475-7516/2024/07/008.

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Abstract Recently, a static spherically symmetric black hole solution was found in gravity nonminimally coupled a background Kalb-Ramond field. The Lorentz symmetry is spontaneously broken when the Kalb-Ramond field has a nonvanishing vacuum expectation value. In this work, we focus on the quasinormal modes and greybody factor of this black hole. The master equations for the perturbed scalar field, electromagnetic field, and gravitational field can be written into a Schrödinger equation. We use three methods to solve the quasinormal frequencies in the frequency domain. The results agree well w

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36

Liu, Jack G. "Lorentz transformation for motion in the opposite direction." Physics Essays 36, no. 3 (2023): 259–60. http://dx.doi.org/10.4006/0836-1398-36.3.259.

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Special relativity is a half-baked theory in which Lorentz transformation only considers the outbound or departing motion where speed and distance change in the same direction. This paper considers the inbound or approaching motion where speed and distance change in the opposite direction. This paper derived a new form of transformation along with the new Lorentz factor, according to which, in addition to well-known time dilation caused by outbound motion, there would be time contraction caused by inbound motion.

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37

Ghirlanda, G., F. Nappo, G. Ghisellini, et al. "Bulk Lorentz factors of gamma-ray bursts." Astronomy & Astrophysics 609 (January 2018): A112. http://dx.doi.org/10.1051/0004-6361/201731598.

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Knowledge of the bulk Lorentz factor Γ0 of gamma-ray bursts (GRBs) allows us to compute their comoving frame properties shedding light on their physics. Upon collisions with the circumburst matter, the fireball of a GRB starts to decelerate, producing a peak or a break (depending on the circumburst density profile) in the light curve of the afterglow. Considering all bursts with known redshift and with an early coverage of their emission, we find 67 GRBs (including one short event) with a peak in their optical or GeV light curves at a time tp. For another 106 GRBs we set an upper limit tpUL. T

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38

Huynh, Cong Tuan, Chang-Mo Ryu, and Chulmin Kim. "Density filamentation nonlinearly driven by the Weibel instability in relativistic beam plasmas." Physics of Plasmas 29, no. 5 (2022): 052304. http://dx.doi.org/10.1063/5.0081199.

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Density filamentation has been observed in many beam-plasma simulations and experiments. Because current filamentation is a pure transverse mode, charge density filamentation cannot be produced directly by the current filamentation process. To explain this phenomenon, several mechanisms are proposed such as the coupling of the Weibel instability to the two-stream instability, coupling to the Langmuir wave, differences in thermal velocities between the beam and return currents, the magnetic pressure gradient force, etc. In this paper, it is shown that the gradient of the Lorentz factor can, in

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39

LI, ZHUO. "ON GRB PHYSICS REVEALED BY FERMI/LAT." International Journal of Modern Physics: Conference Series 23 (January 2013): 223–27. http://dx.doi.org/10.1142/s2010194513011343.

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We discuss the implications of Fermi/LAT observations on several aspects of gamma-ray burst (GRB) physics, including the radiation process, the emission sites, the bulk Lorentz factor, and the pre-shock magnetic field: (1) MeV-range emission favors synchrotron process but the highest energy (> 10 GeV) emission may not be synchrotron origin, more likely inverse Compton origin; (2) GRB should have multi-zone emission region, with MeV emission produced at smaller radii while optical and > 100 MeV emission at larger radii; (3) the bulk Lorentz factor can be a few 100's, much lower than 103,

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40

Liang, Edison, Wen Fu, Markus Böttcher, and Parisa Roustazadeh. "Scaling of Relativistic Shear Flows with the Bulk Lorentz Factor." Astrophysical Journal 854, no. 2 (2018): 129. http://dx.doi.org/10.3847/1538-4357/aaa7f5.

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41

Renaud, N., and G. Henri. "The terminal bulk Lorentz factor of relativistic electron-positron jets." Monthly Notices of the Royal Astronomical Society 300, no. 4 (1998): 1047–56. http://dx.doi.org/10.1046/j.1365-8711.1998.01970.x.

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42

Zou, Yuan-Chuan, Fei-Fei Wang, Reetanjali Moharana, et al. "Determining the Lorentz Factor and Viewing Angle of GRB 170817A." Astrophysical Journal 852, no. 1 (2017): L1. http://dx.doi.org/10.3847/2041-8213/aaa123.

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43

Ioka, K. "Very High Lorentz Factor Fireballs and Gamma-Ray Burst Spectra." Progress of Theoretical Physics 124, no. 4 (2010): 667–710. http://dx.doi.org/10.1143/ptp.124.667.

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44

Granot, J., and P. Kumar. "Distribution of gamma-ray burst ejecta energy with Lorentz factor." Monthly Notices of the Royal Astronomical Society: Letters 366, no. 1 (2006): L13—L16. http://dx.doi.org/10.1111/j.1745-3933.2005.00121.x.

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45

Sonbas, E., G. A. MacLachlan, K. S. Dhuga, P. Veres, A. Shenoy, and T. N. Ukwatta. "GAMMA-RAY BURSTS: TEMPORAL SCALES AND THE BULK LORENTZ FACTOR." Astrophysical Journal 805, no. 2 (2015): 86. http://dx.doi.org/10.1088/0004-637x/805/2/86.

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46

Rossmanith, E. "Relationship between Lorentz factor and peak width. Development of a new peak-width formula and a generalized Lorentz factor for single and multiple diffraction." Acta Crystallographica Section A Foundations of Crystallography 48, no. 4 (1992): 596–610. http://dx.doi.org/10.1107/s0108767392000849.

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47

SCHWARTZ, D. A., F. MASSARO, A. SIEMIGINOWSKA, et al. "MODELING X–RAY EMISSION OF A STRAIGHT JET: PKS 0920-397." International Journal of Modern Physics D 19, no. 06 (2010): 879–85. http://dx.doi.org/10.1142/s0218271810017147.

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We summarize a study of PKS 0920-397 using our 42 ks Chandra observation in conjunction with our ATCA 20GHz image, and HST/ACS F814W and F475W images. We investigate the hypothesis that the jet X–ray emission is due to inverse-Compton (IC) scattering on the cosmic microwave background (CMB) from the same population of relativistic electrons that give rise to the radio emission. To calculate parameters intrinsic to the source, one must finesse the fact that we do not know the true angle of the jet to our line of sight. Typical assumptions are that the Doppler factor equals the bulk Lorentz fact

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Białostocka, Anna Maria, and Piotr Żabiński. "Modification of Electrodeposited FeNi Alloys by Applying External Magnetic Field." Key Engineering Materials 641 (April 2015): 157–63. http://dx.doi.org/10.4028/www.scientific.net/kem.641.157.

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Alloy electrodeposition with superimposed uniform magnetic field leads to Lorentz force generation. The Lorentz force is a factor which is able to modify the deposit structure, its texture, morphology and magnetic properties. The objective of the presented research was to show the composition, morphology and the surface roughness development of Fe-Ni binary alloys electrodeposited under the influence of the uniform magnetic field. The applied magnetic field caused increase of the paramagnetic element content in the alloys. The surface roughness decrease with an external magnetic field applicat

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Roldán, Diego, and Francisco Roldán-Aráuz. "A Transformation Factor for Superluminal Motion That Preserves Symmetrically the Spacetime Intervals." Symmetry 15, no. 6 (2023): 1177. http://dx.doi.org/10.3390/sym15061177.

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While superluminal phenomena are not empirically substantiated, they present an intriguing hypothetical case. For this speculative framework, the Lorentz transformations would necessitate a revision: instead of the standard γ(x−vt), the absolute value of x′ ought to be expressed as γ(vt−x), because if v were to exceed c, then the interval vt traversed by the superluminal frame S′ would surpass the distance covered by light. Under the postulates of relativity, the subluminal scenario leads to the conventional Lorentz factor. Meanwhile, the superluminal scenario introduces an alternative transfo

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Manh, Tran Dinh, Nguyen Dang Nam, Gihad Keyany Abdulrahman, R. Moradi, and Houman Babazadeh. "The influence of hybrid nanoparticle (Fe3O4 + MWCNT) transportation on natural convection inside porous domain." International Journal of Modern Physics C 31, no. 02 (2019): 2050026. http://dx.doi.org/10.1142/s0129183120500266.

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In this study, hybrid nanofluid free convection has been simulated within a permeable domain involving Lorentz effect. To solve and simulate the problem, Control Volume-based Finite Element Method (CVFEM) method is applied. In addition, the non-Darcy model has been used to apply permeable condition in equations. The influence of hybrid nanoparticles (Fe3O4[Formula: see text][Formula: see text][Formula: see text]MWCNT) inside water as base fluid has been studied. Meanwhile, source term of radiation impact has been described for different nanoparticle shapes. The impacts of substantial variables

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