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Journal articles on the topic 'Magnetorotational instability'

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Published: 4 June 2021
Last updated: 21 February 2023

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1

Balbus, Steven. "Magnetorotational instability." Scholarpedia 4, no. 7 (2009): 2409. http://dx.doi.org/10.4249/scholarpedia.2409.

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2

Moiseenko, Sergey G., and Gennady S. Bisnovatyi-Kogan. "Magnetorotational supernovae. Magnetorotational instability. Jet formation." Astrophysics and Space Science 311, no. 1-3 (August 11, 2007): 191–95. http://dx.doi.org/10.1007/s10509-007-9585-6.

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3

Mikhailovskii, A. B., J. G. Lominadze, R. M. O. Galvão, A. P. Churikov, O. A. Kharshiladze, N. N. Erokhin, and C. H. S. Amador. "Nonlocal magnetorotational instability." Physics of Plasmas 15, no. 5 (May 2008): 052109. http://dx.doi.org/10.1063/1.2913613.

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4

Herron, Isom, and Jeremy Goodman. "Gauging magnetorotational instability." Zeitschrift für angewandte Mathematik und Physik 61, no. 4 (January 12, 2010): 663–72. http://dx.doi.org/10.1007/s00033-009-0050-y.

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5

Julien, Keith, and Edgar Knobloch. "Magnetorotational instability: recent developments." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 368, no. 1916 (April 13, 2010): 1607–33. http://dx.doi.org/10.1098/rsta.2009.0251.

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The magnetorotational instability is believed to play an important role in accretion disc physics in extracting angular momentum from the disc and allowing accretion to take place. For this reason the instability has been the subject of numerous numerical simulations and, increasingly, laboratory experiments. In this review, recent developments in both areas are surveyed, and a new theoretical approach to understanding the nonlinear processes involved in the saturation of the instability is outlined.
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6

Chan, Chi-Ho, Julian H. Krolik, and Tsvi Piran. "Magnetorotational Instability in Eccentric Disks." Astrophysical Journal 856, no. 1 (March 20, 2018): 12. http://dx.doi.org/10.3847/1538-4357/aab15c.

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7

Knobloch, Edgar, and Keith Julien. "Saturation of the magnetorotational instability." Physics of Fluids 17, no. 9 (September 2005): 094106. http://dx.doi.org/10.1063/1.2047592.

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8

Mahajan, S. M., and V. Krishan. "Existence of the Magnetorotational Instability." Astrophysical Journal 682, no. 1 (July 20, 2008): 602–7. http://dx.doi.org/10.1086/589321.

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9

Priede, J., I. Grants, and G. Gerbeth. "Paradox of inductionless magnetorotational instability." Journal of Physics: Conference Series 64 (April 1, 2007): 012011. http://dx.doi.org/10.1088/1742-6596/64/1/012011.

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10

Mikhailovskii, A. B., J. G. Lominadze, A. P. Churikov, N. N. Erokhin, and V. S. Tsypin. "Magnetorotational instability in nonmagnetized plasma." Physics Letters A 372, no. 1 (December 2007): 49–51. http://dx.doi.org/10.1016/j.physleta.2007.06.073.

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11

Kirillov, Oleg N., and Frank Stefani. "Standard and Helical Magnetorotational Instability." Acta Applicandae Mathematicae 120, no. 1 (February 16, 2012): 177–98. http://dx.doi.org/10.1007/s10440-012-9689-z.

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12

Salmeron, Raquel, and Mark Wardle. "Magnetorotational instability in protoplanetary discs." Monthly Notices of the Royal Astronomical Society 361, no. 1 (July 2005): 45–69. http://dx.doi.org/10.1111/j.1365-2966.2005.09060.x.

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13

Rüdiger, G., R. Hollerbach, M. Gellert, and M. Schultz. "The azimuthal magnetorotational instability (AMRI)." Astronomische Nachrichten 328, no. 10 (December 2007): 1158–61. http://dx.doi.org/10.1002/asna.200710852.

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14

Usman, S., and A. Mushtaq. "Magnetorotational Instability in Quantum Dusty Plasma." Astrophysical Journal 911, no. 1 (April 1, 2021): 50. http://dx.doi.org/10.3847/1538-4357/abe94e.

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15

Rembiasz, T., M. Obergaulinger, J. Guilet, P. Cerdá-Durán, M. A. Aloy, and E. Müller. "Magnetorotational Instability in Core-Collapse Supernovae." Acta Physica Polonica B Proceedings Supplement 10, no. 2 (2017): 361. http://dx.doi.org/10.5506/aphyspolbsupp.10.361.

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16

Wissing, Robert, Sijing Shen, James Wadsley, and Thomas Quinn. "Magnetorotational instability with smoothed particle hydrodynamics." Astronomy & Astrophysics 659 (March 2022): A91. http://dx.doi.org/10.1051/0004-6361/202141206.

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The magnetorotational instability (MRI) is an important process in driving turbulence in sufficiently ionized accretion disks. It has been extensively studied using simulations with Eulerian grid codes, but remains fairly unexplored for meshless codes. Here, we present a thorough numerical study on the MRI using the smoothed particle magnetohydrodynamics method with the geometric density average force expression. We performed 37 shearing box simulations with different initial setups and a wide range of resolution and dissipation parameters. We show, for the first time, that MRI with sustained turbulence can be simulated successfully with smoothed-particle hydrodynamics (SPH), with results consistent with prior work with grid-based codes, including saturation properties such as magnetic and kinetic energies and their respective stresses. In particular, for the stratified boxes, our simulations reproduce the characteristic “butterfly” diagram of the MRI dynamo with saturated turbulence for at least 100 orbits. On the contrary, traditional SPH simulations suffer from runaway growth and develop unphysically large azimuthal fields, similar to the results from a recent study with meshless methods. We investigated the dependency of MRI turbulence on the numerical Prandtl number (Pm) in SPH, focusing on the unstratified, zero net-flux case. We found that turbulence can only be sustained with a Prandtl number larger than ∼2.5, similar to the critical values for the physical Prandtl number found in grid-code simulations. However, unlike grid-based codes, the numerical Prandtl number in SPH increases with resolution, and for a fixed Prandtl number, the resulting magnetic energy and stresses are independent of resolution. Mean-field analyses were performed on all simulations, and the resulting transport coefficients indicate no α-effect in the unstratified cases, but an active αω dynamo and a diamagnetic pumping effect in the stratified medium, which are generally in agreement with previous studies. There is no clear indication of a shear-current dynamo in our simulation, which is likely to be responsible for a weaker mean-field growth in the tall, unstratified, zero net-flux simulation.
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17

Shalimov, S. L. "Magnetorotational instability in the Earth’s core." Izvestiya, Physics of the Solid Earth 50, no. 4 (July 2014): 463–66. http://dx.doi.org/10.1134/s1069351314040156.

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18

Shtemler, Yu, E. Liverts, and M. Mond. "Explosive magnetorotational instability in Keplerian disks." Physics of Plasmas 23, no. 6 (June 2016): 062301. http://dx.doi.org/10.1063/1.4953051.

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19

Oishi, Jeffrey S., Geoffrey M. Vasil, Morgan Baxter, Andrew Swan, Keaton J. Burns, Daniel Lecoanet, and Benjamin P. Brown. "The magnetorotational instability prefers three dimensions." Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences 476, no. 2233 (January 2020): 20190622. http://dx.doi.org/10.1098/rspa.2019.0622.

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The magnetorotational instability (MRI) occurs when a weak magnetic field destabilizes a rotating, electrically conducting fluid with inwardly increasing angular velocity. The MRI is essential to astrophysical disc theory where the shear is typically Keplerian. Internal shear layers in stars may also be MRI-unstable, and they take a wide range of profiles, including near-critical. We show that the fastest growing modes of an ideal magnetofluid are three-dimensional provided the shear rate, S , is near the two-dimensional onset value, S c . For a Keplerian shear, three-dimensional modes are unstable above S ≈ 0.10 S c , and dominate the two-dimensional modes until S ≈ 2.05 S c . These three-dimensional modes dominate for shear profiles relevant to stars and at magnetic Prandtl numbers relevant to liquid-metal laboratory experiments. Significant numbers of rapidly growing three-dimensional modes remainy well past 2.05 S c . These finding are significant in three ways. First, weakly nonlinear theory suggests that the MRI saturates by pushing the shear rate to its critical value. This can happen for systems, such as stars and laboratory experiments, that can rearrange their angular velocity profiles. Second, the non-normal character and large transient growth of MRI modes should be important whenever three-dimensionality exists. Finally, three-dimensional growth suggests direct dynamo action driven from the linear instability.
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20

Arlt, Reiner. "Magnetorotational instability in Ap star envelopes." Proceedings of the International Astronomical Union 2004, IAUS224 (July 2004): 103–8. http://dx.doi.org/10.1017/s1743921304004430.

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21

GOODMAN, JEREMY, and HANTAO JI. "Magnetorotational instability of dissipative Couette flow." Journal of Fluid Mechanics 462 (July 10, 2002): 365–82. http://dx.doi.org/10.1017/s0022112002008704.

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Axisymmetric stability of viscous resistive magnetized Couette flow is re-examined, with the emphasis on flows that would be hydrodynamically stable according to Rayleigh's criterion: opposing gradients of angular velocity and specific angular momentum. In this regime, magnetorotational instabilities (MRI) may occur. Previous work has focused on the Rayleigh-unstable regime. To prepare for an experimental study of MRI, which is of intense astrophysical interest, we solve for global linear modes in a wide gap with realistic dissipation coefficients. Exchange of stability appears to occur through marginal modes. Velocity eigenfunctions of marginal modes are nearly singular at conducting boundaries, but magnetic eigenfunctions are smooth and obey a fourth-order differential equation in the inviscid limit. The viscous marginal system is of tenth order; an eighth-order approximation previously used for Rayleigh-unstable modes does not permit MRI. Peak growth rates are insensitive to boundary conditions. They are predicted with surprising accuracy by WKB methods even for the largest-scale mode. We conclude that MRI is achievable under plausible experimental conditions using easy-to-handle liquid metals such as gallium.
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22

Ren, Haijun, Zhengwei Wu, Jintao Cao, and Paul K. Chu. "Magnetorotational instability in dissipative dusty plasmas." Physics of Plasmas 16, no. 12 (December 2009): 122107. http://dx.doi.org/10.1063/1.3272092.

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23

Kunz, Matthew W., and Steven A. Balbus. "Ambipolar diffusion in the magnetorotational instability." Monthly Notices of the Royal Astronomical Society 348, no. 1 (February 2004): 355–60. http://dx.doi.org/10.1111/j.1365-2966.2004.07383.x.

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24

Winarto, Himawan. "Review of Progress in Magnetorotational Instability." Journal of Physics: Conference Series 1204 (April 2019): 012097. http://dx.doi.org/10.1088/1742-6596/1204/1/012097.

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25

Urpin, V. "Magnetorotational instability in proto-neutron stars." Astronomy and Astrophysics 509 (November 4, 2009): A35. http://dx.doi.org/10.1051/0004-6361/200912887.

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26

Reyes-Ruiz, Mauricio. "Toward Consistent Models of Protoplanetary Discs." Symposium - International Astronomical Union 202 (2004): 359–61. http://dx.doi.org/10.1017/s0074180900218251.

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In this paper we present results on the effect of the vertical stratification of magnetic diffusivity, expected in current models of protoplanetary discs, on the development of the magnetorotational instability. Specifically, on the basis of a quasi-global, linear analysis we study the operation of the magnetorotational instability across the so-called dead zone of protoplanetary discs. Our results indicate that the predicted strong vertical diffusivity gradients can damp the instability in such regions. This suggests the necessity of a revision of current models for the structure and evolution of protoplanetary discs.
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27

Devlen, Ebru, Ayse Ulubay, and E. Rennan Pekünlü. "Magnetorotational instability in diamagnetic, misaligned protostellar discs." Monthly Notices of the Royal Astronomical Society 491, no. 4 (December 4, 2019): 5481–88. http://dx.doi.org/10.1093/mnras/stz3358.

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ABSTRACT In this study, we addressed the question of how the growth rate of the magnetorotational instability is modified when the radial component of the stellar dipole magnetic field is taken into account in addition to the vertical component. Considering a fiducial radius in the disc where diamagnetic currents are pronounced, we carried out a linear stability analysis to obtain the growth rates of the magnetorotational instability for various parameters such as the ratio of the radial-to-vertical component and the gradient of the magnetic field, the Alfvenic Mach number, and the diamagnetization parameter. Our results show that the interaction between the diamagnetic current and the radial component of the magnetic field increases the growth rate of the magnetorotational instability and generates a force perpendicular to the disc plane that may induce a torque. It is also shown that considering the radial component of the magnetic field and taking into account a radial gradient in the vertical component of the magnetic field causes an increase in the magnitudes of the growth rates of both the axisymmetric (m = 0) and the non-axisymmetric (m = 1) modes.
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28

Stefani, F., G. Gerbeth, Th Gundrum, J. Szklarski, G. Rüdiger, and R. Hollerbach. "Liquid metal experiments on the magnetorotational instability." Magnetohydrodynamics 45, no. 2 (2009): 135–44. http://dx.doi.org/10.22364/mhd.45.2.2.

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29

Guseva, Anna, Ashley P. Willis, Rainer Hollerbach, and Marc Avila. "Transport Properties of the Azimuthal Magnetorotational Instability." Astrophysical Journal 849, no. 2 (November 6, 2017): 92. http://dx.doi.org/10.3847/1538-4357/aa917d.

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30

Rosenberg, Jarrett, and Fatima Ebrahimi. "Onset of Plasmoid Reconnection during Magnetorotational Instability." Astrophysical Journal Letters 920, no. 2 (October 1, 2021): L29. http://dx.doi.org/10.3847/2041-8213/ac2b2e.

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31

Rosenberg, Jarrett, and Fatima Ebrahimi. "Onset of Plasmoid Reconnection during Magnetorotational Instability." Astrophysical Journal Letters 920, no. 2 (October 1, 2021): L29. http://dx.doi.org/10.3847/2041-8213/ac2b2e.

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32

Dziourkevitch, N., D. Elstner, and G. Rüdiger. "Interstellar turbulence driven by the magnetorotational instability." Astronomy & Astrophysics 423, no. 2 (August 2004): L29—L32. http://dx.doi.org/10.1051/0004-6361:200400029.

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33

Masada, Youhei, Takayoshi Sano, and Hideaki Takabe. "Nonaxisymmetric Magnetorotational Instability in Proto–Neutron Stars." Astrophysical Journal 641, no. 1 (April 10, 2006): 447–57. http://dx.doi.org/10.1086/500391.

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34

Bai, Xue-Ning. "MAGNETOROTATIONAL-INSTABILITY-DRIVEN ACCRETION IN PROTOPLANETARY DISKS." Astrophysical Journal 739, no. 1 (September 6, 2011): 50. http://dx.doi.org/10.1088/0004-637x/739/1/50.

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35

Vishniac, Ethan T. "THE SATURATION LIMIT OF THE MAGNETOROTATIONAL INSTABILITY." Astrophysical Journal 696, no. 1 (April 21, 2009): 1021–28. http://dx.doi.org/10.1088/0004-637x/696/1/1021.

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36

Pino, Jesse, and S. M. Mahajan. "Global Axisymmetric Magnetorotational Instability with Density Gradients." Astrophysical Journal 678, no. 2 (May 10, 2008): 1223–29. http://dx.doi.org/10.1086/586705.

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37

Ren, Haijun, Zhengwei Wu, Jintao Cao, Chao Dong, and Paul K. Chu. "Density gradient effects on the magnetorotational instability." Plasma Physics and Controlled Fusion 53, no. 3 (January 28, 2011): 035012. http://dx.doi.org/10.1088/0741-3335/53/3/035012.

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38

Ren, Haijun, Jintao Cao, Zhengwei Wu, and Paul K. Chu. "Magnetorotational instability in a two-fluid model." Plasma Physics and Controlled Fusion 53, no. 6 (April 21, 2011): 065021. http://dx.doi.org/10.1088/0741-3335/53/6/065021.

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39

Kretke, Katherine A., and D. N. C. Lin. "STRUCTURE OF MAGNETOROTATIONAL INSTABILITY ACTIVE PROTOPLANETARY DISKS." Astrophysical Journal 721, no. 2 (September 10, 2010): 1585–92. http://dx.doi.org/10.1088/0004-637x/721/2/1585.

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40

Kral, Quentin, and Henrik Latter. "The magnetorotational instability in debris-disc gas." Monthly Notices of the Royal Astronomical Society 461, no. 2 (June 21, 2016): 1614–20. http://dx.doi.org/10.1093/mnras/stw1429.

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41

Ilgisonis, V. I., and I. V. Khalzov. "Magnetorotational instability in a nonuniform magnetic field." JETP Letters 86, no. 11 (February 2008): 705–8. http://dx.doi.org/10.1134/s002136400723004x.

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42

Piontek, Robert A., and Eve C. Ostriker. "ISM turbulence driven by the magnetorotational instability." Proceedings of the International Astronomical Union 2, S237 (August 2006): 65–69. http://dx.doi.org/10.1017/s1743921307001238.

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AbstractWe have performed numerical simulations which were designed to further our understanding of the turbulent interstellar medium (ISM). Our simulations include a multi-phase thermodynamic model of the ISM, magnetic fields, and sheared rotation, allowing us to study the effects of the magnetorotational instability (MRI) in an environment containing high density cold clouds embedded in a warm, low density, ambient medium. These models have shown that the MRI is indeed a significant source of turbulence, particularly at low mean densities typical of the outer regions of the Milky Way, where star formation rates are low, but high levels of turbulence persist. Here, we summarize past findings, as well as our most recent models which include vertical stratification, allowing us to self-consistently model the vertical distribution of material in the disk.
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43

Sharma, Prateek, Gregory W. Hammett, and Eliot Quataert. "Transition from Collisionless to Collisional Magnetorotational Instability." Astrophysical Journal 596, no. 2 (October 20, 2003): 1121–30. http://dx.doi.org/10.1086/378234.

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44

Araya-Góchez, Rafael A., and Ethan T. Vishniac. "Radiative heat conduction and the magnetorotational instability." Monthly Notices of the Royal Astronomical Society 355, no. 2 (December 2004): 345–51. http://dx.doi.org/10.1111/j.1365-2966.2004.08329.x.

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45

Mikhailovskii, A. B., J. G. Lominadze, A. P. Churikov, N. N. Erokhin, N. S. Erokhin, and V. S. Tsypin. "Effect of pressure anisotropy on magnetorotational instability." Journal of Experimental and Theoretical Physics 106, no. 2 (February 2008): 371–79. http://dx.doi.org/10.1134/s1063776108020155.

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46

Masada, Youhei, and Takayoshi Sano. "Axisymmetric Magnetorotational Instability in Viscous Accretion Disks." Astrophysical Journal 689, no. 2 (December 20, 2008): 1234–43. http://dx.doi.org/10.1086/592601.

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47

Vasil, Geoffrey M. "On the magnetorotational instability and elastic buckling." Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences 471, no. 2177 (May 2015): 20140699. http://dx.doi.org/10.1098/rspa.2014.0699.

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This paper demonstrates an equivalence between rotating magnetized shear flows and a stressed elastic beam. This results from finding the same form of dynamical equations after an asymptotic reduction of the axis-symmetric magnetorotational instability (MRI) under the assumption of almost-critical driving. The analysis considers the MRI dynamics in a non-dissipative near-equilibrium regime. Both the magnetic and elastic systems reduce to a simple one-dimensional wave equation with a non-local nonlinear feedback. Under transformation, the equation comprises a large number of mean-field interacting Duffing oscillators. This system was the first proven example of a strange attractor in a partial differential equation. Finding the same reduced equation in two natural applications suggests the model might result from other applications and could fall into a universal class based on symmetry.
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48

Yokosawa, M., and T. Inui. "Magnetorotational Instability around a Rotating Black Hole." Astrophysical Journal 631, no. 2 (October 2005): 1051–61. http://dx.doi.org/10.1086/432674.

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49

Noguchi, K., V. I. Pariev, S. A. Colgate, H. F. Beckley, and J. Nordhaus. "Magnetorotational Instability in Liquid Metal Couette Flow." Astrophysical Journal 575, no. 2 (August 20, 2002): 1151–62. http://dx.doi.org/10.1086/341502.

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50

Quataert, Eliot, William Dorland, and Gregory W. Hammett. "The Magnetorotational Instability in a Collisionless Plasma." Astrophysical Journal 577, no. 1 (September 20, 2002): 524–33. http://dx.doi.org/10.1086/342174.

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