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Journal articles on the topic 'Magnetic flux'

Author: Grafiati

Published: 4 June 2021

Last updated: 31 July 2024

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1

OKADA, Yohji, Hidetoshi MIYAZAWA, Ryou KONDO, and Masato ENOKIZONO. "2A21 Flux Concentrated Hybrid Magnetic Bearing." Proceedings of the Symposium on the Motion and Vibration Control 2010 (2010): _2A21–1_—_2A21–12_. http://dx.doi.org/10.1299/jsmemovic.2010._2a21-1_.

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2

Grebenikov, V. V., R. V. Gamaleya, and A. N. Sokolovsky. "ELECTRIC MACHINE WITH AXIAL MAGNETIC FLUX, PERMANENT MAGNETS AND MULTILAYERED PRINTING WINDINGS." Tekhnichna Elektrodynamika 2020, no. 2 (February 26, 2020): 28–35. http://dx.doi.org/10.15407/techned2020.02.028.

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3

Schmieder, Brigitte, and Etienne Pariat. "Magnetic flux emergence." Scholarpedia 2, no. 12 (2007): 4335. http://dx.doi.org/10.4249/scholarpedia.4335.

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4

Thomas, John H., and Benjamin Montesinos. "Magnetic Flux Concentration by Siphon Flows in Isolated Magnetic Flux Tubes." Symposium - International Astronomical Union 138 (1990): 263–66. http://dx.doi.org/10.1017/s0074180900044211.

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Siphon flows along arched, isolated magnetic flux tubes, connecting photospheric footpoints of opposite magnetic polarity, cause a significant increase in the magnetic field strength of the flux tube due to the decreased internal gas pressure associated with the flow (the Bernoulli effect). These siphon flows offer a possible mechanism for producing intense, inclined, small-scale magnetic structures in the solar photosphere.

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5

Harada, Y., W. Hioe, and E. Goto. "Quantum flux parametron with magnetic flux regulator." IEEE Transactions on Appiled Superconductivity 1, no. 2 (June 1991): 90–94. http://dx.doi.org/10.1109/77.84614.

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6

Liu, Jiang, V. Angelopoulos, Xu-Zhi Zhou, and A. Runov. "Magnetic flux transport by dipolarizing flux bundles." Journal of Geophysical Research: Space Physics 119, no. 2 (February 2014): 909–26. http://dx.doi.org/10.1002/2013ja019395.

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7

Jiu, Shu-Ping. "Numerical Simulation of the Explosive Events in the Solar Atmosphere." International Astronomical Union Colloquium 141 (1993): 134–37. http://dx.doi.org/10.1017/s0252921100028955.

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AbstractExplosive events are the earliest indicators of flare activity and potentially predict the imminent occurrence of a flare at a specific location. They are highly energetic small-scale phenomena which are frequently detected throughout the quiet and active sun. The observations show that explosive events are related to emerging magnetic flux and tend to occur on the edges of high photospheric magnentic field regions. The cancellation of photospheric magnetic flux are the manifestation of explosive events, so that they are identified as the magnetic reconnection of flux elements. We assume that emerging flux are convected to the network boundaries with the typical velocity of intranetwork elements. Two-dimension (2D) compressible MHD simulations are performed to explore the reconnection process between emerging intranework flux and network field. The numerical results clearly show the cancellation of magnetic flux and the acceleration of the plasma flow.

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8

Neuber, A. A., and J. C. Dickens. "Magnetic flux compression Generators." Proceedings of the IEEE 92, no. 7 (July 2004): 1205–15. http://dx.doi.org/10.1109/jproc.2004.829001.

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9

Dahlburg, R. B., S. K. Antiochos, and D. Norton. "Magnetic flux tube tunneling." Physical Review E 56, no. 2 (August 1, 1997): 2094–103. http://dx.doi.org/10.1103/physreve.56.2094.

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10

Xia, Chun, and Rony Keppens. "Modeling Magnetic Flux Ropes." Proceedings of the International Astronomical Union 8, S300 (June 2013): 121–24. http://dx.doi.org/10.1017/s1743921313010843.

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AbstractThe magnetic configuration hosting prominences can be a large-scale helical magnetic flux rope. As a necessary step towards future prominence formation studies, we report on a stepwise approach to study flux rope formation. We start with summarizing our recent three-dimensional (3D) isothermal magnetohydrodynamic (MHD) simulation where a flux rope is formed, including gas pressure and gravity. This starts from a static corona with a linear force-free bipolar magnetic field, altered by lower boundary vortex flows around the main polarities and converging flows towards the polarity inversion. The latter flows induce magnetic reconnection and this forms successive new helical loops so that a complete flux rope grows and ascends. After stopping the driving flows, the system relaxes to a stable helical magnetic flux rope configuration embedded in an overlying arcade. Starting from this relaxed isothermal endstate, we next perform a thermodynamic MHD simulation with a chromospheric layer inserted at the bottom. As a result of a properly parametrized coronal heating, and due to radiative cooling and anisotropic thermal conduction, the system further relaxes to an equilibrium where the flux rope and the arcade develop a fully realistic thermal structure. This paves the way to future simulations for 3D prominence formation.

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11

Golubović, D. S., and V. V. Moshchalkov. "Linear magnetic flux amplifier." Applied Physics Letters 87, no. 14 (October 3, 2005): 142501. http://dx.doi.org/10.1063/1.2077855.

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12

Filippov, Boris, Olesya Martsenyuk, Abhishek K. Srivastava, and Wahab Uddin. "Solar Magnetic Flux Ropes." Journal of Astrophysics and Astronomy 36, no. 1 (March 2015): 157–84. http://dx.doi.org/10.1007/s12036-015-9321-5.

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13

PAVLOV, V. D. "MAGNETIC FLOW AND ITS QUANTIZATION." Izvestia Ufimskogo Nauchnogo Tsentra RAN, no. 4 (December 11, 2020): 25–28. http://dx.doi.org/10.31040/2222-8349-2020-0-4-25-28.

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It is noted that the elementary electric charge is equal to e , from which fact the well-known principle of quantization of the electric charge definitely follows, namely, the electric charge is quantized and a quantum is the charge of the electron e (or positron). Or any change in the charge is equal to an integer number of electrons (or positrons). The formally identical transformation of the principle of quantization of the electric charge allows formulating the principle of quantization of the magnetic flux, namely, the quantity inverse to the magnetic flux is quantized and a quantum is the inverse of the quantum of the F. London magnetic flux. Or any change in the reciprocal of the magnetic flux is equal to an integer number of quantities inverse to the quantum of the F. London magnetic flux. The reciprocal of the magnetic flux quantum is equal to the sum of two quantities inverse to the quantum of the F. London magnetic flux. The validity of the principle of quantization of the magnetic flux with respect to the hydrogen atom is illustrated by Theorem 1: quantization of the energy of the hydrogen atom is a consequence of the principle of quantization of the magnetic flux. Theorem 2 is proved: the magnetic flux of a hydrogen atom in the ground state is equal to the quantum of the F. London magnetic flux. Theorem 3 is proved: the quantum of the magnetic flux is not the minimum possible for a nonzero magnetic flux. It is established that the quantum of the magnetic flux is not a quantum in the sense of a portion (like the F. London quantum). A quantum is the inverse of the quantum of the F. London magnetic flux. It is established that the magnitude of the magnetic flux quantum is not the minimum possible for a nonzero magnetic flux. It is established that the magnetic flux of a hydrogen atom in the ground state is equal to the quantum of the F. London magnetic flux. A discrete set of energies of the hydrogen atom is noted to be a consequence of the solution of the Schrödinger equation, which, in turn, is phenomenological. The reverse discourse used in the proof of Theorem 1 can show that the Schrödinger equation is a consequence of the principle of quantization of the magnetic flux.

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14

Il'ichev, E., and Ya S. Greenberg. "Flux qubit as a sensor of magnetic flux." Europhysics Letters (EPL) 77, no. 5 (February 27, 2007): 58005. http://dx.doi.org/10.1209/0295-5075/77/58005.

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15

Archontis, V., and T. Török. "Eruption of magnetic flux ropes during flux emergence." Astronomy & Astrophysics 492, no. 2 (November 20, 2008): L35—L38. http://dx.doi.org/10.1051/0004-6361:200811131.

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16

Cameron, R. H., and M. Schüssler. "Loss of toroidal magnetic flux by emergence of bipolar magnetic regions." Astronomy & Astrophysics 636 (April 2020): A7. http://dx.doi.org/10.1051/0004-6361/201937281.

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The polarity of the toroidal magnetic field in the solar convection zone periodically reverses in the course of the 11/22-year solar cycle. Among the various processes that contribute to the removal of “old-polarity” toroidal magnetic flux is the emergence of flux loops forming bipolar regions at the solar surface. We quantify the loss of subsurface net toroidal flux by this process. To this end, we determine the contribution of an individual emerging bipolar loop and show that it is unaffected by surface flux transport after emergence. Together with the linearity of the diffusion process this means that the total flux loss can be obtained by adding the contributions of all emerging bipolar magnetic regions. The resulting total loss rate of net toroidal flux amounts to 1.3 × 1015 Mx s−1 during activity maxima and 6.1 × 1014 Mx s−1 during activity minima, to which ephemeral regions contribute about 90 and 97%, respectively. This rate is consistent with the observationally inferred loss rate of toroidal flux into interplanetary space and corresponds to a decay time of the subsurface toroidal flux of about 12 years, also consistent with a simple estimate based on turbulent diffusivity. Consequently, toroidal flux loss by flux emergence is a relevant contribution to the budget of net toroidal flux in the solar convection zone. The consistency between the toroidal flux loss rate due to flux emergence and what is expected from turbulent diffusion, and the similarity between the corresponding decay time and the length of the solar cycle are important constraints for understanding the solar cycle and the Sun’s internal dynamics.

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17

Borg, A. L., M. G. G. T. Taylor, and J. P. Eastwood. "Observations of magnetic flux ropes during magnetic reconnection in the Earth's magnetotail." Annales Geophysicae 30, no. 5 (May 3, 2012): 761–73. http://dx.doi.org/10.5194/angeo-30-761-2012.

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Abstract. We present an investigation of magnetic flux ropes observed by the four Cluster spacecraft during periods of magnetic reconnection in the Earth's magnetotail. Using a list of 21 Cluster encounters with the reconnection process in the period 2001–2006 identified in Borg et al. (2012), we present the distribution and characteristics of the flux ropes. We find 27 flux ropes embedded in the reconnection outflows of only 11 of the 21 reconnection encounters. Reconnection processes associated with no flux rope observations were not distinguishable from those where flux ropes were observed. Only 7 of the 27 flux ropes show evidence of enhanced energetic electron flux above 50 keV, and there was no clear signature of the flux rope in the thermal particle measurements. We found no clear correlation between the flux rope core field and the prevailing IMF By direction.

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18

Nieves-Chinchilla, Teresa, Miguel Angel Hidalgo, and Hebe Cremades. "Distorted-toroidal Flux Rope Model for Heliospheric Flux Ropes." Astrophysical Journal 947, no. 2 (April 1, 2023): 79. http://dx.doi.org/10.3847/1538-4357/acb3c1.

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Abstract The 3D characterization of magnetic flux ropes observed in the heliosphere has been a challenging task for decades. This is mainly due to the limitations on inferring the 3D global topology and physical properties from the 1D time series from any spacecraft. To advance our understanding of magnetic flux ropes whose configuration departs from the typical stiff geometries, here we present an analytical solution for a 3D flux rope model with an arbitrary cross section and a toroidal global shape. This constitutes the next level of complexity following the elliptic-cylindrical (EC) geometry. The mathematical framework was established by Nieves-Chinchilla et al. with the EC flux rope model, which describes a magnetic topology with an elliptical cross section as a first approach to changes in the cross section. In the distorted-toroidal flux rope model, the cross section is described by a general function. The model is completely described by a nonorthogonal geometry and the Maxwell equations can be consistently solved to obtain the magnetic field and relevant physical quantities. As a proof of concept, this model is generalized in terms of the radial dependence of current density components. The last part of this paper is dedicated to a specific function, F ( φ ) = δ ( 1 − λ cos φ ) , to illustrate possibilities of the model. This model paves the way toward the investigation of complex distortions of magnetic structures in the solar wind. Future investigations will explore these distortions in depth by analyzing specific events; studying implications for physical quantities, such as magnetic fluxes, helicity, or energy; and evaluating the force balance with the ambient solar wind that allows such distortions.

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19

Leitão, D. C., I. G. Trindade, R. Fermento, João P. Araújo, S. Cardoso, P. P. Freitas, and João Bessa Sousa. "Magnetic Field Enhancement with Soft Magnetic Flux Guides." Materials Science Forum 587-588 (June 2008): 313–17. http://dx.doi.org/10.4028/www.scientific.net/msf.587-588.313.

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In this work, a study of the sensitivity enhancement of spin valve sensors, when located in close proximity to magnetic flux guides, is presented. The magnetoresistance (MR) of spin-valve sensors, lithographically patterned into stripes with lateral dimensions, (length) l = 500 µm, (width) wsensor = 1, 2, 6 µm and placed near one/two Co93.5Zr2.8Nb3.7 (CZN) magnetic flux guide, is characterized at room temperature. CZN has a high permeability that together with a defined microstructured shape, is able to concentrate the magnetic flux in a small area, leading to an increase in sensor's sensitivity. The magnetic field amplification is estimated by comparison of sensor sensitivity with/without magnetic flux guides, in the linear operation range, and studied as a function of different parameters. Besides an enhancement in sensitivity, sensors also exhibit an important increase in the hard axis coercivity and a shift from MR(H=0) = 0.5, both attributed to the magnetic flux guides. Amplification factors of the order of 20 are observed..

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20

Welsch, B. T. "Magnetic Flux Cancellation and Coronal Magnetic Energy." Astrophysical Journal 638, no. 2 (February 20, 2006): 1101–9. http://dx.doi.org/10.1086/498638.

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21

Attie, R., and D. E. Innes. "Magnetic balltracking: Tracking the photospheric magnetic flux." Astronomy & Astrophysics 574 (February 2015): A106. http://dx.doi.org/10.1051/0004-6361/201424552.

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22

Démoulin, P., M. Janvier, and S. Dasso. "Magnetic Flux and Helicity of Magnetic Clouds." Solar Physics 291, no. 2 (December 23, 2015): 531–57. http://dx.doi.org/10.1007/s11207-015-0836-3.

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23

Mei, Z. X., R. Keppens, I. I. Roussev, and J. Lin. "Magnetic reconnection during eruptive magnetic flux ropes." Astronomy & Astrophysics 604 (August 2017): L7. http://dx.doi.org/10.1051/0004-6361/201731146.

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24

Lorrain, Paul, and Nikos Salingaros. "Local currents in magnetic flux tubes and flux ropes." American Journal of Physics 61, no. 9 (September 1993): 811–17. http://dx.doi.org/10.1119/1.17445.

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25

Hewitt, A. J., A. Ahfock, and S. A. Suslov. "Magnetic flux density distribution in axial flux machine cores." IEE Proceedings - Electric Power Applications 152, no. 2 (2005): 292. http://dx.doi.org/10.1049/ip-epa:20055039.

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26

Murai, Kunitoshi, Jun’ya Hori, Yoshiko Fujii, Jonah Shaver, and Gregory Kozlowski. "Magnetic flux pinning and flux jumps in polycrystalline MgB2." Cryogenics 45, no. 6 (June 2005): 415–20. http://dx.doi.org/10.1016/j.cryogenics.2005.03.001.

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27

Nya’Ubit, Ilham Rizkia, Gigih Priyandoko, Fitrian Imaduddin, Dimas Adiputra, and Ubaidillah. "Torque Characterization of T-shaped Magnetorheological Brake Featuring Serpentine Magnetic Flux." Journal of Advanced Research in Fluid Mechanics and Thermal Sciences 78, no. 2 (December 10, 2020): 85–97. http://dx.doi.org/10.37934/arfmts.78.2.8597.

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Recently, T-shaped Magnetorheological Brake (MRB) usually utilize more than one wire coil electromagnetic to maximize magnetic flux reaching all Magnetorheological Fluid (MRF) gaps. This research was focused on the usage of a single wire coil on MRB with uniformly magnetic flux distribution. To achieve the goal, the serpentine magnetic flux profile was adopted to maximize all MRF gaps that only use a single coil. Firstly, the magnetic circuit which implementing serpentine magnetic flux was design in a two-dimensional model. It was then followed by magnetostatic simulation using Finite Element Method Magnetics (FEMM) to determine the amount of magnetic flux density. The data were then employed to calculate the braking torque. After having the final dimension and completing the workshop drawing, an MRB prototype was fabricated. Thus, the prototype was characterized using the braking test apparatus to figure out the torque profiles. Moreover, the experimental results were compared to the simulation results. This process justified the validity of the proposed mathematical model of the T-shaped MRB. It was investigated that the maximum braking torque from simulations and experimental works were 1.51 Nm and 1.91 Nm at 1 A, respectively. Overall the between differences of simulations and experimental works were about 10%. It is therefore, the mathematical model can be used for further application in the actuator control system.

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28

Deng, Jiang Hua, Chao Tang, Yan Ran Zhan, and Xing Ying Jiang. "Distribution of Magnetic Flux Density and Magnetic Force in EMR." Advanced Materials Research 652-654 (January 2013): 2248–53. http://dx.doi.org/10.4028/www.scientific.net/amr.652-654.2248.

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Distribution of magnetic flux density and magnetic force in electromagnetic riveting was investigated with the electromagnetic field coupling model established by the finite element method. The results show the radial magnetic flux density presents a sinusoidal exponential decaying form at a point and the maximum value of radial magnetic flux density lies in about half of the driver plate radius along the driver plate radius direction. The distribution of magnetic force is determined by that of magnetic flux density and the magnetic force is a body force, which weakens very quickly from the inside to the outside of the driver plate. In order to prevent penetration of magnetic field, the thickness of driver plate is an important parameter to increase the energy utilization ratio.

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29

Kara, Okan, and Hasan Hüseyin Çelik. "A Novel Nonlinear Magnetic Equivalent Circuit Model for Magnetic Flux Leakage System." Applied Sciences 14, no. 10 (May 10, 2024): 4071. http://dx.doi.org/10.3390/app14104071.

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To ensure efficient inspection using the magnetic flux leakage (MFL) method, generating a flux density near the saturation level within the tested material is essential. This requirement brings high flux density conditions in the system’s pole regions. Hence, leakage flux within the slot is excessively triggered, leading to distortion of the defect signal. In this context, the system dimensions stand out as one of the most significant factors affecting the mentioned flux distributions. Therefore, various alternative solutions with different system dimensions arise in the design process of the MFL system. This study proposes a magnetic equivalent circuit (MEC) model to achieve optimal system design. The proposed MEC model is designed considering the nonlinear behavior of the material, leakage flux, and fringing effects. Verification results demonstrate that the MEC model consistently tracks the finite element analysis (FEA) results in calculating the flux densities. Furthermore, the relative errors in the flux density calculations of the tested material are at a maximum level of 10.2% and an average of 5.2% compared to the FEA. These findings indicate that the proposed MEC model can be effectively utilized in rapid prototyping and optimization procedures of MFL system design by providing fast solutions with reasonable accuracy.

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30

Ismail, Izwan, Saiful Amri Mazlan, and Abdul Ghani Olabi. "Magnetic Circuit Simulation for Magnetorheological (MR) Fluids Testing Rig in Squeeze Mode." Advanced Materials Research 123-125 (August 2010): 991–94. http://dx.doi.org/10.4028/www.scientific.net/amr.123-125.991.

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In this study, a testing rig in squeeze was designed and developed with the ability to conduct various tests especially for quasi-static squeezing at different values of magnetic field strength. Finite Element Method Magnetics (FEMM) was utilized to simulate the magnetic field distribution and magnetic flux lines generation from electromagnetic coil to the testing rig. Tests were conducted with two types of MR fluid. MRF-132DG was used to obtain the behaviour of MR fluid, while synthesized epoxy-based MR fluid was used for investigating the magnetic field distribution with regards to particle chains arrangement. Simulation results of the rig design showed that the magnetic flux density was well distributed across the tested materials. Magnetic flux lines were aligned with force direction to perform squeeze tests. Preliminary experimental results showed that stress-strain pattern of MR fluids were in agreement with previous results. The epoxy-based MR samples produced excellent metallographic samples for carbonyl iron particles distributions and particle chain structures investigation.

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31

Gilbert, Andrew D., Joanne Mason, and Steven M. Tobias. "Flux expulsion with dynamics." Journal of Fluid Mechanics 791 (February 24, 2016): 568–88. http://dx.doi.org/10.1017/jfm.2016.60.

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In the process of flux expulsion, a magnetic field is expelled from a region of closed streamlines on a $TR_{m}^{1/3}$ time scale, for magnetic Reynolds number $R_{m}\gg 1$ ($T$ being the turnover time of the flow). This classic result applies in the kinematic regime where the flow field is specified independently of the magnetic field. A weak magnetic ‘core’ is left at the centre of a closed region of streamlines, and this decays exponentially on the $TR_{m}^{1/2}$ time scale. The present paper extends these results to the dynamical regime, where there is competition between the process of flux expulsion and the Lorentz force, which suppresses the differential rotation. This competition is studied using a quasi-linear model in which the flow is constrained to be axisymmetric. The magnetic Prandtl number $R_{m}/R_{e}$ is taken to be small, with $R_{m}$ large, and a range of initial field strengths $b_{0}$ is considered. Two scaling laws are proposed and confirmed numerically. For initial magnetic fields below the threshold $b_{core}=O(UR_{m}^{-1/3})$, flux expulsion operates despite the Lorentz force, cutting through field lines to result in the formation of a central core of magnetic field. Here $U$ is a velocity scale of the flow and magnetic fields are measured in Alfvén units. For larger initial fields the Lorentz force is dominant and the flow creates Alfvén waves that propagate away. The second threshold is $b_{dynam}=O(UR_{m}^{-3/4})$, below which the field follows the kinematic evolution and decays rapidly. Between these two thresholds the magnetic field is strong enough to suppress differential rotation, leaving a magnetically controlled core spinning in solid body motion, which then decays slowly on a time scale of order $TR_{m}$.

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32

Urasaki, Shinpachiro, Yoshimitsu Kobayashi, Yasushi Kami, Yuichiroh Mitani, and Eitaku Nobuyama. "Control Design Considering Magnetic Flux Characteristic Uncertainty for Magnetic Levitation System with Magnetic Flux and Current Feedback." IEEJ Transactions on Electronics, Information and Systems 139, no. 10 (October 1, 2019): 1159–66. http://dx.doi.org/10.1541/ieejeiss.139.1159.

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33

DeForest, C. E., T. A. Howard, and D. J. McComas. "DISCONNECTING OPEN SOLAR MAGNETIC FLUX." Astrophysical Journal 745, no. 1 (December 28, 2011): 36. http://dx.doi.org/10.1088/0004-637x/745/1/36.

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34

Gekelman, Walter, Bart Van Compernolle, Tim DeHaas, and Stephen Vincena. "Chaos in magnetic flux ropes." Plasma Physics and Controlled Fusion 56, no. 6 (February 12, 2014): 064002. http://dx.doi.org/10.1088/0741-3335/56/6/064002.

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35

Mikheenko, P., R. Chakalov, R. I. Chakalova, M. S. Colclough, and C. M. Muirhead. "Magnetic Flux Penetration into MgB2." Modern Physics Letters B 17, no. 10n12 (May 20, 2003): 675–89. http://dx.doi.org/10.1142/s0217984903005706.

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We report magnetization and transport measurements on MgB2 in the form of powder, bulk ceramic, wire made by diffusion of Mg into B, and pulsed laser deposited thin films. Ceramic and wire forms show strong intergranular links, and we compare their properties with those of single crystals. The powder shows a magnetic moment versus temperature curve that scales with the moment at the lowest temperature, consistent with a distribution of grain sizes, on the scale of the London penetration depth. The ceramics shows anisotropic magnetization behavior, which is probably a consequence of the anisotropic compressional forces used in its manufacture. In both powder and ceramic, we have observed intriguing negative magnetic moments and steps therein upon changing temperature, well above the obvious superconducting transition. These could indicate small amounts of some higher Tc superconducting phases. However, magnetization loops measured in this regime show ferromagnetism, which we suggest is the origin of the magnetic properties above Tc. The wire shows a linear diamagnetic response up to an Hc1 of 236 Oe, has a normal state resistivity of 2.6 × 10-6 Ω·cm just above the transition and a resistivity ratio of 21, which is also similar to those of single crystals. The thin films are composed of large crystalline platelets, have a Tc of 35 K, and are diamagnetic.

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36

Davey, Kent, Larry McDonald, and Travis Hutson. "Axial Flux Cycloidal Magnetic Gears." IEEE Transactions on Magnetics 50, no. 4 (April 2014): 1–7. http://dx.doi.org/10.1109/tmag.2013.2287181.

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37

Moldwin, Mark B., and W. Jeffrey Hughes. "Plasmoids as magnetic flux ropes." Journal of Geophysical Research: Space Physics 96, A8 (August 1, 1991): 14051–64. http://dx.doi.org/10.1029/91ja01167.

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38

Eckern, Ulrich. "Quantum phase and magnetic flux." Nature 329, no. 6141 (October 1987): 676. http://dx.doi.org/10.1038/329676a0.

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39

Roberts, B. "Waves in Magnetic Flux Tubes." Symposium - International Astronomical Union 142 (1990): 159–74. http://dx.doi.org/10.1017/s0074180900087891.

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The basic aspects of wave propagation in a magnetic flux tube are reviewed, with particular emphasis on the types of flux tube that occur in the solar atmosphere. Two fundamental speeds arise naturally in a description of wave propagation in a flux tube: the slow magnetoacoustic (cusp) speed cT, which is both subsonic and sub-Alfvénic, and a mean Alfvén speed ck. Both surface and body modes are supported by a tube. It is stressed that a flux tube may act as a wave guide, similar to the guidance of light by a fibre optic, or sound in an ocean layer, or seismic waves in the Earth's crust.

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40

Feng, HengQiang, GuoQing Zhao, and JieMin Wang. "Small interplanetary magnetic flux rope." Science China Technological Sciences 63, no. 2 (June 27, 2019): 183–94. http://dx.doi.org/10.1007/s11431-018-9481-1.

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41

Post, E. J. "Linking and enclosing magnetic flux." Physics Letters A 119, no. 1 (November 1986): 47–49. http://dx.doi.org/10.1016/0375-9601(86)90644-4.

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42

Schrijver, C. J., and K. L. Harvey. "The photospheric magnetic flux budget." Solar Physics 150, no. 1-2 (March 1994): 1–18. http://dx.doi.org/10.1007/bf00712873.

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43

Carpena, P., and A. V. Coronado. "Easy calculation of magnetic flux." European Journal of Physics 19, no. 4 (July 1, 1998): 325–29. http://dx.doi.org/10.1088/0143-0807/19/4/002.

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44

Popov, I. P. "MAGNETIC FLUX SCATTERING IN TRANSFORMERS." Bulletin of the Tver State Technical University. Series «Building. Electrical engineering and chemical technology», no. 4 (2020): 81–88. http://dx.doi.org/10.46573/2658-7459-2020-4-81-88.

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Existing methods do not allow measuring leakage reactance for each transformer winding separately, therefore, for simplicity, they are often assumed to be equal to each other. The purpose of the study is to substantiate the possibility of experimental determination of leakage reactance for each transformer winding separately. The dissipation reactance of each transformer winding separately can be determined by at least three experimental methods that give satisfactory agreement of the results. An almost paradoxical result – the capacitive nature of the leakage resistance of the inner winding of the transformer was obtained only for concentric cylindrical windings. It should not be generalized to other types of windings. The presented experimental methods are not tied to the character of the leakage resistance reactivity. They are universal - they can be used with any type of winding. The results obtained are recommended for use in the design and study of transformers.

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Russell, C. T. "Physics of magnetic flux ropes." Eos, Transactions American Geophysical Union 70, no. 26 (1989): 684. http://dx.doi.org/10.1029/89eo00206.

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46

Zwaan, Cornelis. "The emergence of magnetic flux." Solar Physics 100, no. 1-2 (October 1985): 397–414. http://dx.doi.org/10.1007/bf00158438.

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Song, Wenbin, and Jingxiu Wang. "Periodicities in photospheric magnetic flux." Science in China Series G 49, no. 2 (March 26, 2006): 246–56. http://dx.doi.org/10.1007/s11433-006-0246-5.

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Castaño, Diego J., and Teresa M. Castaño. "Self-inductance and magnetic flux." American Journal of Physics 91, no. 8 (August 1, 2023): 622–28. http://dx.doi.org/10.1119/5.0098417.

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The canonical equation for self-inductance involving magnetic flux is examined, and a more general form is presented that can be applied to continuous current distributions. We attempt to clarify and extend the use of the standard equation by recasting it in its more versatile form.

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Fischer, C. E., J. M. Borrero, N. Bello González, and A. J. Kaithakkal. "Observations of solar small-scale magnetic flux-sheet emergence." Astronomy & Astrophysics 622 (February 2019): L12. http://dx.doi.org/10.1051/0004-6361/201834628.

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Aims. Two types of flux emergence were recently discovered in numerical simulations: magnetic loops and magnetic sheet emergence. While magnetic loop emergence has been documented well in recent years using high-resolution full Stokes data from ground-based telescopes as well as satellites, magnetic sheet emergence is still an understudied process. We report here on the first clear observational evidence of a magnetic sheet emergence and characterise its development. Methods. Full Stokes spectra from the Hinode spectropolarimeter were inverted with the Stokes Inversion based on Response functions (SIR) code to obtain solar atmospheric parameters such as temperature, line-of-sight velocities, and full magnetic field vector information. Results. We analyse a magnetic flux emergence event observed in the quiet-Sun internetwork. After a large-scale appearance of linear polarisation, a magnetic sheet with horizontal magnetic flux density of up to 194 Mx cm−2 hovers in the low photosphere spanning a region of 2–3 arcsec. The magnetic field azimuth obtained through Stokes inversions clearly shows an organised structure of transversal magnetic flux density emerging. The granule below the magnetic flux sheet tears the structure apart leaving the emerged flux to form several magnetic loops at the edges of the granule. Conclusions. A large amount of flux with strong horizontal magnetic fields surfaces through the interplay of buried magnetic flux and convective motions. The magnetic flux emerges within 10 minutes and we find a longitudinal magnetic flux at the foot points of the order of ∼1018 Mx. This is one to two orders of magnitude larger than what has been reported for small-scale magnetic loops. The convective flows feed the newly emerged flux into the pre-existing magnetic population on a granular scale.

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Lites, Bruce, Hector Socas-Navarro, Masahito Kubo, Thomas E. Berger, Zoe Frank, Richard A. Shine, Theodore D. Tarbell, et al. "Hinode Observations of Horizontal Quiet Sun Magnetic Flux and the “Hidden Turbulent Magnetic Flux”." Publications of the Astronomical Society of Japan 59, sp3 (November 30, 2007): S571—S576. http://dx.doi.org/10.1093/pasj/59.sp3.s571.

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