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Автор: Grafiati
Опубліковано: 10 грудня 2022
Оновлено: 28 січня 2023

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Статті в журналах з теми "The origin of magnetic field"

1

Dolginov, A. Z., and A. F. Ioffe. "Origin of the Magnetic Field." International Astronomical Union Colloquium 90 (1986): 11–21. http://dx.doi.org/10.1017/s0252921100091120.

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Some progress has been achieved in recent years in the theory of the stellar magnetic field generation but a lot of questions remain unanswered. I would like to give here a brief critical review of the current state of the problem.
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2

Gvaramadze, V. V., J. G. Lominadze, A. A. Ruzmaikin, D. D. Sokoloff, and A. M. Shukurov. "Magnetic field origin in astrophysical jets." Advances in Space Research 8, no. 2-3 (January 1988): 621–24. http://dx.doi.org/10.1016/0273-1177(88)90467-x.

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3

Neiner, Coralie, Stéphane Mathis, Evelyne Alecian, Constance Emeriau, and Jason Grunhut. "The origin of magnetic fields in hot stars." Proceedings of the International Astronomical Union 10, S305 (December 2014): 61–66. http://dx.doi.org/10.1017/s1743921315004524.

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AbstractObservations of stable mainly dipolar magnetic fields at the surface of ~7% of single hot stars indicate that these fields are of fossil origin, i.e. they descend from the seed field in the molecular clouds from which the stars were formed. The recent results confirm this theory. First, theoretical work and numerical simulations confirm that the properties of the observed fields correspond to those expected from fossil fields. They also showed that rapid rotation does not modify the surface dipolar magnetic configurations, but hinders the stability of fossil fields. This explains the lack of correlation between the magnetic field properties and stellar properties in massive stars. It may also explain the lack of detections of magnetic fields in Be stars, which rotate close to their break-up velocity. In addition, observations by the BinaMIcS collaboration of hot stars in binary systems show that the fraction of those hosting detectable magnetic fields is much smaller than for single hot stars. This could be related to results obtained in simulations of massive star formation, which show that the stronger the magnetic field in the original molecular cloud, the more difficult it is to fragment massive cores to form several stars. Therefore, more and more arguments support the fossil field theory.
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4

Qi Wei-Hua, Li Zhuang-Zhi, Ma Li, Tang Gui-De, Wu Guang-Heng, and Hu Feng-Xia. "Molecular field origin for magnetic ordering of magnetic materials." Acta Physica Sinica 66, no. 6 (2017): 067501. http://dx.doi.org/10.7498/aps.66.067501.

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5

Wanas, M. I. "Non-Conventional Origin of Large-Scale Magnetic Fields." Symposium - International Astronomical Union 140 (1990): 518. http://dx.doi.org/10.1017/s0074180900191041.

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One of the models constructed (Wanas, 1985) within the framework of the generalized field theory (Mikhail and Wanas, 1977) is found to give results in favour of Blackett's speculation concerning rotation and the origin of magnetic fields. The formula giving the surface polar magnetic field of a spherical body of mass M, radius R, and uniform rotational velocity w is given by (Mikhail and Wanas, 1989) In case of a typical galaxy, the model gives a magnetic field of the order of 10-5 Gauss.
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6

Wicht, J., M. Mandea, F. Takahashi, U. R. Christensen, M. Matsushima, and B. Langlais. "The Origin of Mercury’s Internal Magnetic Field." Space Science Reviews 132, no. 2-4 (October 2007): 261–90. http://dx.doi.org/10.1007/s11214-007-9280-5.

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7

Kulsrud, R. M. "The origin of our galactic magnetic field." Astronomische Nachrichten 331, no. 1 (January 2010): 22–26. http://dx.doi.org/10.1002/asna.200911295.

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8

Benevolenskaya, E. E. "Origin of the polar magnetic field reversals." Solar Physics 167, no. 1-2 (August 1996): 47–55. http://dx.doi.org/10.1007/bf00146327.

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9

Spruit, Hendrik C. "The source of magnetic fields in (neutron-) stars." Proceedings of the International Astronomical Union 4, S259 (November 2008): 61–74. http://dx.doi.org/10.1017/s1743921309030075.

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AbstractSome arguments, none entirely conclusive, are reviewed about the origin of magnetic fields in neutron stars, with emphasis of processes during and following core collapse in supernovae. Possible origins of the magnetic fields of neutron stars include inheritance from the main sequence progenitor and dynamo action at some stage of evolution of progenitor. Inheritance is not sufficient to explain the fields of magnetars. Energetic considerations point to differential rotation in the final stages of core collapse process as the most likely source of field generation, at least for magnetars. A runaway phase of exponential growth is needed to achieve sufficient field amplification during relevant phase of core collapse; it can probably be provided by a some form of magnetorotational instability. Once formed in core collapse, the field is in danger of decaying again by magnetic instabilities. The evolution of a magnetic field in a newly formed neutron star is discussed, with emphasis on the existence of stable equilibrium configurations as end products of this evolution, and the role of magnetic helicity in their existence. A particularly puzzling problem is the large range of field strengths observed in neutron stars (as well as in A stars and white dwarfs). It implies that a single, deterministic process is insufficient to explain the origin of the magnetic fields in these stars.
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10

Kawka, Adela. "Clues to the origin and properties of magnetic white dwarfs." Proceedings of the International Astronomical Union 15, S357 (October 2019): 60–74. http://dx.doi.org/10.1017/s1743921320000745.

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AbstractA significant fraction of white dwarfs possess a magnetic field with strengths ranging from a few kG up to about 1000 MG. However, the incidence of magnetism varies when the white dwarf population is broken down into different spectral types providing clues on the formation of magnetic fields in white dwarfs. Several scenarios for the origin of magnetic fields have been proposed from a fossil field origin to dynamo generation at various stages of evolution. Offset dipoles are often assumed sufficient to model the field structure, however time-resolved spectropolarimetric observations have revealed more complex structures such as magnetic spots or multipoles. Surface mapping of these field structures combined with measured rotation rates help distinguish scenarios involving single star evolution from other scenarios involving binary interactions. I describe key observational properties of magnetic white dwarfs such as age, mass, and field strength, and confront proposed formation scenarios with these properties.
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Дисертації з теми "The origin of magnetic field"

1

Schwarte, Judith. "Modelling the earth's magnetic field of magnetospheric origin from CHAMP data." [S.l. : s.n.], 2004. http://deposit.ddb.de/cgi-bin/dokserv?idn=971057001.

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2

Xu, Hao. "The AGN origin of cluster magnetic fields." Diss., [La Jolla] : University of California, San Diego, 2009. http://wwwlib.umi.com/cr/ucsd/fullcit?p3356297.

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Thesis (Ph. D.)--University of California, San Diego, 2009.
Title from first page of PDF file (viewed July 7, 2009). Available via ProQuest Digital Dissertations. Vita. Includes bibliographical references (p. 132-139).
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3

Barnes, D. J. "Origin and evolution of large-scale magnetic fields." Thesis, University College London (University of London), 2015. http://discovery.ucl.ac.uk/1466179/.

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Magnetic elds are ubiquitous at all scales in the Universe and have been observed in galaxies and clusters of galaxies via observations of di use radio emission and Faraday Rotation Measures. Despite the observations, the origin and impact of the magnetic elds in these systems is poorly understood. In this thesis we develop a state of the art cosmological Smoothed Particle Magnetohydrodynamics code, GCMHD+, to enable the study of the magnetic elds of the largest bound structures in the Universe. Using a wide range of idealized test problems, we justify our choice of free parameters and demonstrate the performance of the code relative to analytical solutions and the results produced by a grid based MHD scheme. We then used the code to investigate the evolution of a seed magnetic eld due to the formation of structure. By varying the numerical scheme, we demonstrate that the growth of magnetic elds in galaxy clusters are very sensitive to the growth of numerical divergence of the magnetic eld. We nd that amplitude and topology of the cluster magnetic eld are insensitive to the mass or formation history of the cluster. Using high resolution simulations, we show that a primordial seed magnetic eld is capable of reproducing a wide range of observations of large-scale magnetic elds in galaxy clusters. Additionally, we examine the impact of the formation of spiral structure in a disc galaxy on the galactic magnetic eld. We nd that the numerical scheme can become unstable unless the divergence cleaning scheme is limited. We nd that the rotation of the galaxy produces a disc orientated magnetic eld with a spiral structure and large-scale eld reversals. The formation of spiral arms ampli es the ambient G magnetic eld to 20 G, in agreement with the observations of spiral galaxies. We conclude that additional physics is required to produce a more realistic galactic magnetic eld.
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4

Wilmot-Smith, Antonia. "The origin and dynamic interaction of solar magnetic fields." Thesis, St Andrews, 2008. http://hdl.handle.net/10023/417.

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Beck, Alexander Maximilian. "On the origin and growth of cosmic magnetic fields." Diss., Ludwig-Maximilians-Universität München, 2013. http://nbn-resolving.de/urn:nbn:de:bvb:19-164179.

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6

Schwarte, Judith [Verfasser]. "Modelling the earth's magnetic field of magnetospheric origin from CHAMP data / Geoforschungszentrum Potsdam. Von Judith Schwarte." Potsdam : Geoforschungszentrum, 2004. http://d-nb.info/971057001/34.

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7

Pariev, Vladimir Ivanovich. "Magnetic fields: Their origin and manifestation in accretion disks around supermassive black holes." Diss., The University of Arizona, 2001. http://hdl.handle.net/10150/279820.

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The magnetic field dynamo in the inner part of accretion disks around supermassive black holes in AGNs may be an important mechanism for the generation of magnetic fields in galaxies and in extragalactic space. We consider dynamo with the necessary helicity generation produced by star-disk collisions. Gas heated by a star passing through the disk is buoyant and form rising and expanding plume of plasma. Due to Coriolis forces the flow produced by plumes have coherent helicity. This helicity is the source of alpha effect in the alpha-O dynamo in differentially rotating accretion disk. We apply the mean field dynamo theory to the ensemble of plumes produced by star-disk collisions. We demonstrate the existence of the dynamo and evaluate the growth rate of magnetic field. The estimate of the nonlinear saturated state of the dynamo gives the magnetic field exceeding equipartition with the thermal energy in the accretion disk. Thus, star-disk collision dynamo can be important in generating dynamically significant magnetic fields, which could alter the disk structure and be the source of the energy flow in extragalactic jets. We present results of numerical simulations of the kinematic dynamo produced by star-disk collisions. It was found that for about one star-disk collision per period of rotation of the inner edge of an accretion disk, the typical value of the threshold magnetic Reynolds number is of the order of 100. The generated mean magnetic field has predominantly even parity. We also present theoretical consideration of magnetic dynamo in New Mexico dynamo experiment, which is currently under construction. The experiment utilizes Couette flow and driven jets of liquid sodium to simulate astrophysical alpha-O dynamos in the laboratory. We perform numerical simulations with ideally conducting boundary and evaluate the changes, which vacuum boundary conditions introduce in our numerical results. We also develop the theory of the MHD Ekman boundary layer in differentially rotating conducting fluid. The Ekman layer is formed at the end plates in the experiment. We show that the Ekman layer does not influence the generation of the large scale magnetic field in the experiment.
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8

Aoyama, Tadashi. "A study on the origin of small-scale field-aligned currents as observed in topside ionosphere at middle and low latitudes." 京都大学 (Kyoto University), 2017. http://hdl.handle.net/2433/225408.

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9

Beck, Alexander Maximilian [Verfasser], and Harald [Akademischer Betreuer] Lesch. "On the origin and growth of cosmic magnetic fields / Alexander Maximilian Beck. Betreuer: Harald Lesch." München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2013. http://d-nb.info/1046503154/34.

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10

Bertin, Alexandre. "Geometrical frustration and quantum origin of spin dynamics." Thesis, Université Grenoble Alpes (ComUE), 2015. http://www.theses.fr/2015GRENY014/document.

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Cette thèse se concentre sur l'étude de composés magnétiques géométriquement frustrés où les ions magnétiques se situent aux sommets d'un réseau de tétraèdres partageant leurs sommets: les composés pyrochlores. Deux familles de formule chimique R2M2O7, où R est un lanthanide et M= Ti, Sn, sont particulièrement intéressantes puisqu'elles présentent une grande variété d'états magnétiques exotiques. Premièrement, nous avons étudié le champ cristallin agissant au site de la terre rare dans l'approximation de Stevens où uniquement le terme fondamental est considéré. Un jeu unique de paramètres a été déterminé pour chaque famille considérée grâce à une analyse globale incluant des spectres de neutrons inélastiques de plusieurs composés. Ensuite, nous avons caractérisé avec un large éventail de techniques les propriétés physiques à basse température de Nd2Sn2O7. En dessous de la température de transition Tc=0.91 K, ce composé possède un ordre magnétique à longue portée dans la configuration de spins dite "all-in-all-out". Une persistance de la dynamique de spins a été révélée dans la phase ordonnée, attribuée à des excitations unidimensionnelles de spins. Une dynamique de spins anormalement lente est également reportée dans la phase paramagnétique. Enfin, nous avons apporté quelques informations sur les deux états fondamentaux proposés pour le composé très étudié Tb2Ti2O7: premièrement, l'apparition d'une transition Jahn-Teller à basse température est suggérée mais l'absence d'élargissement des pics de Bragg réfute la présence d'une transition structurale. Enfin ce composé pourrait être un exemple d'une glace de spin quantique mais l'existence d'un plateau d'aimantation n'est pas évident jusqu'à T=20 mK
This Phd thesis focuses on the study of magnetically frustrated compounds where magnetic ions lie at the vertices of a corner-sharing tetrahedra network: the pyrochlore compounds. The two series of chemical formula R2M2O7, where R is a lanthanide and M=Ti, Sn, are of peculiar interest since they display a large variety of exotic magnetic ground states. First, we have studied the crystal-electric-field acting at the rare earth within the Stevens approximation where only the ground state multiplet is considered. A single set of parameters for each families of interest has been determined through a global analysis including several inelastic neutron scattering spectra of various compounds. Then, we have characterised with a large panel of techniques the low temperature physical properties of Nd2Sn2O7. This compound enters a long-range magnetic order at transition temperature Tc=0.91 K with an ``all-in-all-out'' spin configuration. A persistence of spin dynamics has been found in the ordered phase, ascribed to one-dimensional spin loops excitations. Anomalously slow paramagnetic spin fluctuations are also reported. Finally, we have brought information on the two proposed ground states of the widely studied compound Tb2Ti2O7: first, a Jahn-Teller transition is claimed to occur at low temperatures but no broadening of the Bragg peaks is seen down to T=4 K precluding premises of a structural transition. Secondly, this compound could be a realisation of a quantum spin-ice but no definitive evidence of a magnetisation plateau is found down to T=20 mK
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Книги з теми "The origin of magnetic field"

1

Volker, Bothmer, Hady Ahmed Abdel, and International Astronomical Union, eds. Solar activity and its magnetic origin: Proceedings of the 233rd symposium of the International Astronomical Union held in Cairo, Egypt, March 31-April 4, 2006. Cambridge: Cambridge University Press, 2006.

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2

A, Balona Luis, Henrichs Huib F, and Medupe Rodney, eds. International Conference on Magnetic Fields in O, B and A Stars: Origin and connection to pulsation, rotation and mass loss : proceedings of a conference held at University of North-West, Mmabatho, South Africa, 27 November - 1 December, 2002. San Francisco, California: Astronomical Society of the Pacific, 2003.

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3

Es'kov, Evgeniy. Biological effects of electromagnetic fields. ru: INFRA-M Academic Publishing LLC., 2021. http://dx.doi.org/10.12737/1229809.

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The monograph, based on the use of literary information and research materials of the author, attempts to systematize the influence of natural and anthropogenic electric fields on biological objects of different levels of complexity. The origin of cosmic and terrestrial magnetism is described and the influence of this factor on the physiological state, viability and development of plant and animal objects is analyzed. The biological effects of magnetic storms are investigated. The mechanisms of generation, perception and use of electric fields in signaling and spatial orientation of animals are analyzed. Much attention is paid to the analysis of specific reactions of animals to electromagnetic fields. The prospects of using electromagnetic fields to control the behavior of animals and direct influence on the growth processes of plant objects are considered. For a wide range of readers interested in the possibilities of controlling animal behavior and influencing plant growth.
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4

Magnetic field(s). Normal, Ill: Dalkey Archive Press, 2002.

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5

Stolle, Claudia, Nils Olsen, Arthur D. Richmond, and Hermann J. Opgenoorth, eds. Earth's Magnetic Field. Dordrecht: Springer Netherlands, 2018. http://dx.doi.org/10.1007/978-94-024-1225-3.

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6

Rajaram, Girija. The earth's magnetic field. New Delhi: Oxford & IBH Pub Co., 1998.

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7

Grönemeyer, D. H. W., and Robert B. Lufkin, eds. Open Field Magnetic Resonance Imaging. Berlin, Heidelberg: Springer Berlin Heidelberg, 2000. http://dx.doi.org/10.1007/978-3-642-59581-3.

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8

Aono, Osamu. Rotation of a magnetic field. Nagoya, Japan: Institute of Plasma Physics, Nagoya University, 1986.

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9

Marshall, Deborah. Magnetic field strength issues in magnetic resonance imaging (MRI). Ottawa: Canadian Coordinating Office for Health Technology Assessment, 1993.

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10

Shao, Yarui. Magnetic flocculation of fine weakly magnetic iron minerals in an applied magnetic field. Birmingham: University of Birmingham, 1997.

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Частини книг з теми "The origin of magnetic field"

1

Dolginov, A. Z., and A. F. Ioffe. "Origin of the Magnetic Field." In Upper Main Sequence Stars with Anomalous Abundances, 11–24. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4714-6_2.

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2

Gottlieb, D., and M. Lagos. "Lattice Unstabilities of Magnetic Origin." In Applications of Statistical and Field Theory Methods to Condensed Matter, 119. Boston, MA: Springer US, 1990. http://dx.doi.org/10.1007/978-1-4684-5763-6_11.

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3

Ruzmaikin, A. A., A. M. Shukurov, and D. D. Sokoloff. "Origin of Magnetic Fields." In Astrophysics and Space Science Library, 95–121. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2835-0_5.

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4

Wicht, J., M. Mandea, F. Takahashi, U. R. Christensen, M. Matsushima, and B. Langlais. "The Origin of Mercury’s Internal Magnetic Field." In Mercury, 79–108. New York, NY: Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-77539-5_5.

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5

M. Kulsrud, Russell. "The Origin of Galactic Magnetic Fields." In Cosmic Magnetic Fields, 69–88. Berlin, Heidelberg: Springer Berlin Heidelberg, 2005. http://dx.doi.org/10.1007/3540313966_4.

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6

Biermann, Peter L., and Cristina F. Galea. "Origin of Cosmic Magnetic Fields." In The Early Universe and the Cosmic Microwave Background: Theory and Observations, 471–88. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-007-1058-0_21.

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7

Rees, Martin J. "Origin of the Seed Magnetic Field for a Galactic Dynamo." In Cosmical Magnetism, 155–60. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1110-2_15.

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8

Sokoloff, D., and A. Shukurov. "The Origin of Magnetic Field in a Swirling Jet." In Astrophysics and Space Science Library, 399–402. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-1924-5_74.

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9

Tajima, T., and T. Shibata. "On the Origin of Cosmic Magnetic Fields." In Galactic and Intergalactic Magnetic Fields, 531–32. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0569-6_171.

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10

Zhang, C. N., J. G. Shi, and F. P. Chen. "Tortion Influence on the Magnetic Field of Rotating Neutron Stars." In The Origin and Evolution of Neutron Stars, 379. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3913-4_71.

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Тези доповідей конференцій з теми "The origin of magnetic field"

1

Field, George B. "Origin of astrophysical magnetic fields." In International conference on plasma physics ICPP 1994. AIP, 1995. http://dx.doi.org/10.1063/1.49002.

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2

Ichiki, Kiyotomo. "Origin of Cosmological Magnetic Fields." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: International Symposium on Origin of Matter and Evolution of Galaxies 2005: New Horizon of Nuclear Astrophysics and Cosmology. AIP, 2006. http://dx.doi.org/10.1063/1.2234439.

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Tatsumi, Toshitaka. "Microscopic origin of the magnetic field in compact stars." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: International Symposium on Origin of Matter and Evolution of Galaxies 2005: New Horizon of Nuclear Astrophysics and Cosmology. AIP, 2006. http://dx.doi.org/10.1063/1.2234399.

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TÖRNKVIST, OLA. "THE ORIGIN OF COSMIC MAGNETIC FIELDS." In Proceedings of the Third International Workshop on Particle Physics and the Early Universe. WORLD SCIENTIFIC, 2000. http://dx.doi.org/10.1142/9789812792129_0040.

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Spruit, H. C., C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Origin of neutron star magnetic fields." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900262.

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6

Chi, X., and A. W. Wolfendale. "The origin of galactic magnetic fields." In The second Compton symposium. AIP, 1994. http://dx.doi.org/10.1063/1.45684.

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7

Zablodskiy, Mykola, Vitaliy Savchenko, Oleksandr Sinyavsky, and Vladyslav Pliuhin. "Interactions Between Magnetic Field and Biological Objects of Plant Origin." In 2018 IEEE 38th International Conference on Electronics and Nanotechnology (ELNANO). IEEE, 2018. http://dx.doi.org/10.1109/elnano.2018.8477484.

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8

Takahashi, Koh. "Uncertain Stellar Evolution: Convection, Rotation, Magnetic Field." In Proceedings of the 15th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG15). Journal of the Physical Society of Japan, 2020. http://dx.doi.org/10.7566/jpscp.31.011030.

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9

Petit, Véronique, Gregg A. Wade, Laurent Drissen, Thierry Montmerle, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Exploring the origin of neutron star magnetic field: magnetic properties of the progenitor OB stars." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900263.

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Luo, Yudong, Toshitaka Kajino, Motohiko Kusakabe, and Grant J. Mathews. "Primordial Magnetic Field and Its Impact on Primordial Nucleosynthesis." In Proceedings of the 15th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG15). Journal of the Physical Society of Japan, 2020. http://dx.doi.org/10.7566/jpscp.31.011042.

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Звіти організацій з теми "The origin of magnetic field"

1

Tzeferacos, Petros. Simulations of Laser Experiments to Study the Origin of Cosmic Magnetic Fields. Office of Scientific and Technical Information (OSTI), January 2020. http://dx.doi.org/10.2172/1637538.

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2

Eric G. Blackman. New Approaches to the Origin and Dynamics of Magnetic Fields of Cosmic Relevance. Office of Scientific and Technical Information (OSTI), November 2004. http://dx.doi.org/10.2172/838500.

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3

Kang, W. N., D. H. Kim, and J. H. Park. Origin of 1/f noise peaks of YBa{sub 2}Cu{sub 3}O{sub x} films in a magnetic field. Office of Scientific and Technical Information (OSTI), February 1994. http://dx.doi.org/10.2172/79036.

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4

Wyntjes, Geert. Photonic Magnetic Field Sensor. Fort Belvoir, VA: Defense Technical Information Center, February 2002. http://dx.doi.org/10.21236/ada409236.

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5

Boozer, A. H. Magnetic field line Hamiltonian. Office of Scientific and Technical Information (OSTI), February 1985. http://dx.doi.org/10.2172/5915503.

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6

Peeraphatdit, Chorthip. Magnetic nanoparticles for applications in oscillating magnetic field. Office of Scientific and Technical Information (OSTI), January 2009. http://dx.doi.org/10.2172/1037982.

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7

Jain, Animesh, John Escallier, George Ganetis, Wing Louie, Andrew Marone, Richard Thomas, and Peter Wanderer. Magnetic Field Measurements for Fast-Changing Magnetic Fields. Office of Scientific and Technical Information (OSTI), June 2005. http://dx.doi.org/10.2172/1661620.

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8

Kippen, Karen Elizabeth. National High Magnetic Field Laboratory-Pulsed Field Facility. Office of Scientific and Technical Information (OSTI), July 2015. http://dx.doi.org/10.2172/1210215.

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9

Kippen, Karen Elizabeth. National High Magnetic Field Laboratory - Pulsed Field Facility. Office of Scientific and Technical Information (OSTI), April 2018. http://dx.doi.org/10.2172/1434442.

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10

Goettee, J. High-magnetic-field research collaborations. Office of Scientific and Technical Information (OSTI), December 1998. http://dx.doi.org/10.2172/307959.

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