Relevant bibliographies by topics / Magnetorotational instability

Academic literature on the topic 'Magnetorotational instability'

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Published: 4 June 2021
Last updated: 21 February 2023

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Journal articles on the topic "Magnetorotational instability"

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

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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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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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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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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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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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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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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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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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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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Dissertations / Theses on the topic "Magnetorotational instability"

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Salmeron, Raquel. "Magnetorotational Instability in Protostellar Discs." Physics, 2005. http://hdl.handle.net/2123/919.

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Doctor of Philosophy
We investigate the linear growth and vertical structure of the magnetorotational instability (MRI) in weakly ionised, stratified accretion discs. The magnetic field is initially vertical and perturbations have vertical wavevectors only. Solutions are obtained at representative radial locations from the central protostar for different choices of the initial magnetic field strength, sources of ionisation, disc structure and configuration of the conductivity tensor. The MRI is active over a wide range of magnetic field strengths and fluid conditions in low conductivity discs. For the minimum-mass solar nebula model, incorporating cosmic ray and x-ray ionisation and assuming that charges are carried by ions and electrons only, perturbations grow at 1 AU for B < 8G. For a significant subset of these strengths (200mG < B < 5 G), the growth rate is of order the ideal MHD rate (0.75 Omega). Hall conductivity modifies the structure and growth rate of global unstable modes at 1 AU for all magnetic field strengths that support MRI. As a result, at this radius, modes obtained with a full conductivity tensor grow faster and are active over a more extended cross-section of the disc, than perturbations in the ambipolar diffusion limit. For relatively strong fields (e.g. B > 200 mG), ambipolar diffusion alters the envelope shapes of the unstable modes, which peak at an intermediate height, instead of being mostly flat as modes in the Hall limit are in this region of parameter space. Similarly, when cosmic rays are assumed to be excluded from the disc by the winds emitted by the magnetically active protostar, unstable modes grow at this radius for B < 2 G. For strong fields, perturbations exhibit a kink at the height where x-ray ionisation becomes active. Finally, for R = 5 AU (10 AU), unstable modes exist for B < 800 mG (B < 250 mG) and the maximum growth rate is close to the ideal-MHD rate for 20 mG < B < 500 mG (2 mG < B < 50 mG). Similarly, perturbations incorporating Hall conductivity have a higher wavenumber and grow faster than solutions in the ambipolar diffusion limit for B < 100 mG (B < 10 mG). Unstable modes grow even at the midplane for B > 100 mG (B ~ 1 mG), but for weaker fields, a small dead region exists. When a population of 0.1 um grains is assumed to be present, perturbations grow at 10 AU for B < 10 mG. We estimate that the figure for R = 1 AU would be of order 400 mG. We conclude that, despite the low magnetic coupling, the magnetic field is dynamically important for a large range of fluid conditions and field strengths in protostellar discs. An example of such magnetic activity is the generation of MRI unstable modes, which are supported at 1 AU for field strengths up to a few gauss. Hall diffusion largely determines the structure and growth rate of these perturbations for all studied radii. At radii of order 1 AU, in particular, it is crucial to incorporate the full conductivity tensor in the analysis of this instability, and more generally, in studies of the dynamics of astrophysical discs.
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Salmeron, Raquel. "Magnetorotational Instability in Protostellar Discs." Thesis, The University of Sydney, 2004. http://hdl.handle.net/2123/919.

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We investigate the linear growth and vertical structure of the magnetorotational instability (MRI) in weakly ionised, stratified accretion discs. The magnetic field is initially vertical and perturbations have vertical wavevectors only. Solutions are obtained at representative radial locations from the central protostar for different choices of the initial magnetic field strength, sources of ionisation, disc structure and configuration of the conductivity tensor. The MRI is active over a wide range of magnetic field strengths and fluid conditions in low conductivity discs. For the minimum-mass solar nebula model, incorporating cosmic ray and x-ray ionisation and assuming that charges are carried by ions and electrons only, perturbations grow at 1 AU for B < 8G. For a significant subset of these strengths (200mG < B < 5 G), the growth rate is of order the ideal MHD rate (0.75 Omega). Hall conductivity modifies the structure and growth rate of global unstable modes at 1 AU for all magnetic field strengths that support MRI. As a result, at this radius, modes obtained with a full conductivity tensor grow faster and are active over a more extended cross-section of the disc, than perturbations in the ambipolar diffusion limit. For relatively strong fields (e.g. B > 200 mG), ambipolar diffusion alters the envelope shapes of the unstable modes, which peak at an intermediate height, instead of being mostly flat as modes in the Hall limit are in this region of parameter space. Similarly, when cosmic rays are assumed to be excluded from the disc by the winds emitted by the magnetically active protostar, unstable modes grow at this radius for B < 2 G. For strong fields, perturbations exhibit a kink at the height where x-ray ionisation becomes active. Finally, for R = 5 AU (10 AU), unstable modes exist for B < 800 mG (B < 250 mG) and the maximum growth rate is close to the ideal-MHD rate for 20 mG < B < 500 mG (2 mG < B < 50 mG). Similarly, perturbations incorporating Hall conductivity have a higher wavenumber and grow faster than solutions in the ambipolar diffusion limit for B < 100 mG (B < 10 mG). Unstable modes grow even at the midplane for B > 100 mG (B ~ 1 mG), but for weaker fields, a small dead region exists. When a population of 0.1 um grains is assumed to be present, perturbations grow at 10 AU for B < 10 mG. We estimate that the figure for R = 1 AU would be of order 400 mG. We conclude that, despite the low magnetic coupling, the magnetic field is dynamically important for a large range of fluid conditions and field strengths in protostellar discs. An example of such magnetic activity is the generation of MRI unstable modes, which are supported at 1 AU for field strengths up to a few gauss. Hall diffusion largely determines the structure and growth rate of these perturbations for all studied radii. At radii of order 1 AU, in particular, it is crucial to incorporate the full conductivity tensor in the analysis of this instability, and more generally, in studies of the dynamics of astrophysical discs.
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Piontek, Robert Andrew. "Thermal and magnetorotational instability in the interstellar medium." College Park, Md. : University of Maryland, 2005. http://hdl.handle.net/1903/3094.

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Thesis (Ph. D.) -- University of Maryland, College Park, 2005.
Thesis research directed by: Astronomy. Title from t.p. of PDF. Includes bibliographical references. Published by UMI Dissertation Services, Ann Arbor, Mich. Also available in paper.
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Szklarski, Jacek T. "Helical magnetorotational instability in MHD Taylor-Couette flow." Phd thesis, kostenfrei, 2007. http://opus.kobv.de/ubp/volltexte/2008/1600/.

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Bai, Yang. "Study of viscoelastic instabily in Taylor-Couette system as an analog of the magnetorotational instability." Thesis, Le Havre, 2015. http://www.theses.fr/2015LEHA0015/document.

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Cette thèse est consacrée à la vérification de l'analogie entre l'instabilité viscoélastique (VEI) et l'instabilité magnéto-rotationnel (MRI) dans un écoulement képlérien, afin de mieux comprendre le transport du moment dans les disques d'accrétion. Le discriminant de Rayleigh élasto-rotationnel est établi pour clarifier le rôle de l'élasticité dans le VEI. L'analyse de stabilité linéaire (LSA) avec le modèle d’Oldroyd-B est effectuée pour prédire les paramètres critiques des modes viscoélastiques. Il fait apparaître également l'influence de l'élasticité, la viscosité polymérique et d'autres paramètres de contrôle pour le VEI. Des expériences bien contrôlées avec des solutions aqueuses de polyoxyéthylène (POE) et de polyéthylène glycol (PEG) sont effectuées. Nous avons observé le mode stationnaire axisymétrique supercritique avec des solutions de faible élasticité et modes désordonnés sous-critiques avec des solutions de grande élasticité. Les formes et les valeurs critiques de ces modes sont en bon accord avec les prédictions théoriques de LSA. Selon l'analogie, le mode axisymétrique stationnaire est probablement l'analogue de MRI standard, tandis que le mode désordonné est probable que l'analogue de MRI hélicoïdale. La thèse contient aussi des résultats théoriques expérimentaux sur quatre autres régimes de rotation et un cas de limite d'élasticité infinie
This thesis is devoted to the verification of the analogy between the viscoelastic instability (VEI) and the magnetorotational instability (MRI) in a Keplerian flow, in order to get better understanding of the momentum transportation in accretion disks.The elasto-rotational Rayleigh discriminant is deduced to clarify the role of the elasticity in the VEI. The linear stability analysis (LSA) with Oldroyd-B model is performed to predict critical parameters of viscoelastic modes, and it reveals the influence of the elasticity, polymer viscosity on the VEI. Experiments with well controlled aqueous solutions of polyoxyethylene (POE) and polyethylene glycol (PEG) are conducted. We have observed supercritical stationary axisymmetric mode with solutions of small elasticity and subcritical disordered modes with solutions of large elasticity. Both the flow patterns and the critical values of these modes are in good agreement with the LSA predictions. According to the analogy, the stationary axisymmetric mode is likely the analog of the standard MRI while the disordered mode is likely the analog of the helical MRI. The thesis contains also theoretical and experimental results with four other rotation regimes and the limit case of infinite elasticity
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Pessah, Martin Elias. "Magnetohydrodynamic Turbulence and Angular Momentum Transport in Accretion Disks." Diss., The University of Arizona, 2007. http://hdl.handle.net/10150/194324.

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It is currently believed that angular momentum transport in accretion disks is mediated by magnetohydrodynamic (MHD) turbulence driven by the magnetorotational instability (MRI). More than 15 years after its discovery, an accretion disk model that incorporates the MRI as the mechanism driving the MHD turbulence is still lacking. This dissertation constitutes the first in a series of steps towards establishing the formalism and methodology needed to move beyond the standard accretion disk model and incorporating the MRI as the mechanism enabling the accretion process. I begin by presenting a local linear stability analysis of a compressible, differentially rotating flow and addressing the evolution of the MRI beyond the weak-field limit when magnetic tension forces due to strong toroidal fields are considered. Then, I derive the first formal analytical proof showing that, during the exponential growth of the instability, the mean total stress produced by correlated MHD fluctuations is positive and leads to a net outward flux of angular momentum. I also show that some characteristics of the MHD stresses that are determined during this initial phase are roughly preserved in the turbulent saturated state observed in local numerical simulations. Motivated by these results, I present the first mean-field MHD model for angular momentum transport driven by the MRI that is able to account for a number of correlations among stresses found in local numerical simulations. I point out the relevance of a new type of correlation that couples the dynamical evolution of the Reynolds and Maxwell stresses and plays a key role in developing and sustaining the MHD turbulence. Finally, I address how the turbulent transport of angular momentum depends on the magnitude of the local shear. I show that turbulent MHD stresses in accretion disks cannot be described in terms of shear-viscosity.
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Rembiasz, Tomasz [Verfasser], Ewald [Akademischer Betreuer] Müller, and Björn [Akademischer Betreuer] Garbrecht. "Numerical Studies of the Magnetorotational Instability in Core-Collapse Supernovae / Tomasz Rembiasz. Gutachter: Ewald Müller ; Björn Garbrecht. Betreuer: Ewald Müller." München : Universitätsbibliothek der TU München, 2013. http://d-nb.info/1046939777/34.

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Rosin, Mark. "Instabilities and transport in magnetized plasmas." Thesis, University of Cambridge, 2011. https://www.repository.cam.ac.uk/handle/1810/237241.

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In a magnetized plasma, naturally occurring pressure anisotropies facilitate instabilities that are expected to modify the transport properties of the system. In this thesis we examine two such instabilities and, where appropriate, their effects on transport. First we consider the collisional (fluid) magnetized magnetorotational instability (MRI) in the presence of the Braginskii viscosity. We conduct a global linear analysis of the instability in a galactic rotation profile for three magnetic field configurations: purely azimuthal, purely vertical and slightly pitched. Our analysis, numerical and asymptotic, shows that the first two represent singular configurations where the Braginskii viscosity's primary role is dissipative and the maximum growth rate is proportional to the Reynolds number when this is small. For a weak pitched field, the Braginskii viscosity is destabilising and when its effects dominate over the Lorentz force, the growth rate of the MRI can be up to 2√2 times faster than the inviscid limit. If the field is strong, an over-stability develops and both the real and imaginary parts of the frequency increase with the coefficient of the viscosity. Second, in the context of the ICM of galaxy clusters, we consider the pressure-anisotropy-driven firehose instability. The linear instability is fast (~ ion cyclotron period) and small-scale (ion Larmor radius ρi) and so fluid theory is inapplicable. We determine its nonlinear evolution in an ab initio kinetic calculation (for parallel gradients only). We use a particular physical asymptotic ordering to derive a closed nonlinear equation for the firehose turbulence, which we solve. We find secular (α t) growth of magnetic fluctuations and a k-||3 spectrum, starting at scales >~ ρi. When a parallel ion heat flux is present, the parallel firehose instability mutates into the new gyrothermal instability. Its nonlinear evolution also involves secular magnetic energy growth, but its spectrum is eventually dominated by modes with a maximal scale ~ρilT/λmfp,(lT is the parallel temperature gradient scale). Throughout we discuss implications for modelling, transport and other areas of magnetized plasma physics.
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"Modeling Layered Accretion and the Magnetorotational Instability in Protoplanetary Disks." Doctoral diss., 2012. http://hdl.handle.net/2286/R.I.14970.

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abstract: Understanding the temperature structure of protoplanetary disks (PPDs) is paramount to modeling disk evolution and future planet formation. PPDs around T Tauri stars have two primary heating sources, protostellar irradiation, which depends on the flaring of the disk, and accretional heating as viscous coupling between annuli dissipate energy. I have written a "1.5-D" radiative transfer code to calculate disk temperatures assuming hydrostatic and radiative equilibrium. The model solves for the temperature at all locations simultaneously using Rybicki's method, converges rapidly at high optical depth, and retains full frequency dependence. The likely cause of accretional heating in PPDs is the magnetorotational instability (MRI), which acts where gas ionization is sufficiently high for gas to couple to the magnetic field. This will occur in surface layers of the disk, leaving the interior portions of the disk inactive ("dead zone"). I calculate temperatures in PPDs undergoing such "layered accretion." Since the accretional heating is concentrated far from the midplane, temperatures in the disk's interior are lower than in PPDs modeled with vertically uniform accretion. The method is used to study for the first time disks evolving via the magnetorotational instability, which operates primarily in surface layers. I find that temperatures in layered accretion disks do not significantly differ from those of "passive disks," where no accretional heating exists. Emergent spectra are insensitive to active layer thickness, making it difficult to observationally identify disks undergoing layered vs. uniform accretion. I also calculate the ionization chemistry in PPDs, using an ionization network including multiple charge states of dust grains. Combined with a criterion for the onset of the MRI, I calculate where the MRI can be initiated and the extent of dead zones in PPDs. After accounting for feedback between temperature and active layer thickness, I find the surface density of the actively accreting layers falls rapidly with distance from the protostar, leading to a net outward flow of mass from ~0.1 to 3 AU. The clearing out of the innermost zones is possibly consistent with the observed behavior of recently discovered "transition disks."
Dissertation/Thesis
Ph.D. Physics 2012
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Szklarski, Jacek T. [Verfasser]. "Helical magnetorotational instability in MHD Taylor-Couette flow / Jacek T. Szklarski." 2007. http://d-nb.info/987390341/34.

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Book chapters on the topic "Magnetorotational instability"

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Krishan, V., and S. M. Mahajan. "Magnetorotational Instability In Accretion Disks." In Astrophysics and Space Science Proceedings, 233–48. Dordrecht: Springer Netherlands, 2009. http://dx.doi.org/10.1007/978-1-4020-8868-1_15.

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Mignone, Andrea, Attilio Ferrari, Gianluigi Bodo, Paola Rossi, and Fausto Cattaneo. "Aspect Ratio Dependence in Magnetorotational Instability Shearing Box Simulations." In Protostellar Jets in Context, 77–82. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3_9.

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Siegel, Daniel M., and Riccardo Ciolfi. "Magnetic Field Amplification in Hypermassive Neutron Stars via the Magnetorotational Instability." In Springer Proceedings in Physics, 119–24. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-20046-0_14.

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"The Magnetorotational Instability (MRI)." In Magnetic Processes in Astrophysics, 185–246. Weinheim, Germany: Wiley-VCH Verlag GmbH & Co. KGaA, 2013. http://dx.doi.org/10.1002/9783527648924.ch5.

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"Chapter 12: Magnetorotational instability." In Nonconservative Stability Problems of Modern Physics, 364–86. De Gruyter, 2013. http://dx.doi.org/10.1515/9783110270433.364.

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Andersson, Nils. "Cosmic fireworks." In Gravitational-Wave Astronomy, 508–40. Oxford University Press, 2019. http://dx.doi.org/10.1093/oso/9780198568032.003.0020.

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The simulation of matter in general relativity, be it for neutron star mergers or core collapse, is discussed. State-of-the-art simulations for the dynamical bar-mode instability and neutron star merges are summarized. The inclusion of magnetic field is considered and key issues like the magnetorotational instability are explored. General gravitational collapse is discussed, and the progress toward the simulations of explosions in core-collapse studies is explained.
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Conference papers on the topic "Magnetorotational instability"

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HAWLEY, JOHN F. "THE MAGNETOROTATIONAL INSTABILITY." In Open Issues in Core Collapse Supernova Theory. WORLD SCIENTIFIC, 2005. http://dx.doi.org/10.1142/9789812703446_0003.

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Noguchi, Koichi. "Magnetorotational Instability in a Couette Flow of Plasma." In NON-NEUTRAL PLASMA PHYSICS V: Workshop on Non-Neutral Plasmas. AIP, 2003. http://dx.doi.org/10.1063/1.1635188.

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Brandenburg, Axel. "Shearing and embedding box simulations of the magnetorotational instability." In MHD COUETTE FLOWS: Experiments and Models. AIP, 2004. http://dx.doi.org/10.1063/1.1832142.

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Sano, Takayoshi. "Local Behavior of the Magnetorotational Instability in Accretion Disks." In MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. AIP, 2005. http://dx.doi.org/10.1063/1.2077229.

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Zimmerman, Daniel S. "Characterization of the magnetorotational instability from a turbulent background state." In MHD COUETTE FLOWS: Experiments and Models. AIP, 2004. http://dx.doi.org/10.1063/1.1832133.

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Ji, Hantao. "Magnetorotational Instability in a Short Couette Flow of Liquid Gallium." In MHD COUETTE FLOWS: Experiments and Models. AIP, 2004. http://dx.doi.org/10.1063/1.1832134.

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Sawai, Hidetomo, Nobuya Nishimura, Tomoya Takiwaki, and Shoichi Yamada. "R-Process Nucleosynthesis in Core-Collapse Supernovae Aided by Magnetorotational Instability." In Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016). Journal of the Physical Society of Japan, 2017. http://dx.doi.org/10.7566/jpscp.14.020618.

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Nath, Sujit K., and Banibrata Mukhopadhyay. "Emergence of nonlinearity and plausible turbulence in accretion disks via hydromagnetic transient growth faster than magnetorotational instability." In Proceedings of the MG14 Meeting on General Relativity. WORLD SCIENTIFIC, 2017. http://dx.doi.org/10.1142/9789813226609_0072.

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Reports on the topic "Magnetorotational instability"

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HERRON, ISOM H. Magnetorotational Instability of Dissipative MHD Flows. Office of Scientific and Technical Information (OSTI), July 2010. http://dx.doi.org/10.2172/983047.

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Hantao Ji, Jeremy Goodman, and Akira Kageyama. Magnetorotational Instability in a Rotating Liquid Metal Annulus. Office of Scientific and Technical Information (OSTI), March 2001. http://dx.doi.org/10.2172/780617.

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Burns, Keaton J. Investigating the Magnetorotational Instability with Dedalus, and Open-Souce Hydrodynamics Code. Office of Scientific and Technical Information (OSTI), August 2012. http://dx.doi.org/10.2172/1049730.

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Ebrahimi, Fatima. Simulations of Dynamo and Magnetorotational Instability in Madison Plasma Experiments and Astrophysical Disks. Office of Scientific and Technical Information (OSTI), February 2018. http://dx.doi.org/10.2172/1422354.

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Ebrahimi, Fatima. Global Simulations of Dynamo and Magnetorotational Instability in Madison Plasma Experiments and Astrophysical Disks. Office of Scientific and Technical Information (OSTI), July 2014. http://dx.doi.org/10.2172/1177153.

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J Squire, A. Bhattacharjee. Magnetorotational Instability: Nonmodal Growth and the Relationship of Global Modes to the Shearing Box. Office of Scientific and Technical Information (OSTI), July 2014. http://dx.doi.org/10.2172/1179780.

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