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Results 1 - 10
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37
WAVES, CORIOLIS FORCE AND THE DYNAMO EFFECT
, 2004
"... Dynamo activity caused by waves in a rotating magneto-plasma is investigated. In astrophysical environments such as accretion disks and at sufficiently small spatial scales, the Hall effect is likely to play an important role. It is shown that a combination of the Coriolis force and Hall effect can ..."
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Dynamo activity caused by waves in a rotating magneto-plasma is investigated. In astrophysical environments such as accretion disks and at sufficiently small spatial scales, the Hall effect is likely to play an important role. It is shown that a combination of the Coriolis force and Hall effect can
NULL FARADAY ROTATION- A CLEAN METHOD FOR DETERMINATION OF RELAXATION TIMES AND EFFECTIVE MASSES IN MIS AND OTHER SYSTEMS
, 1980
"... We determine the relation between photon, cyclotron, collision, and plasma frequencies which ensures a null Faraday rotation for electromag-netic wave propagation i a flee-carrier magnetoplasma. This provides a clean deterinination (in the sense that it is independent of multiple reflections and the ..."
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We determine the relation between photon, cyclotron, collision, and plasma frequencies which ensures a null Faraday rotation for electromag-netic wave propagation i a flee-carrier magnetoplasma. This provides a clean deterinination (in the sense that it is independent of multiple reflections
Physics Drift Effects in the Theory of Instabilities in a Rotating Plasma
"... ABSTRACT. The drift effects are incorporated into the theory of instabilities in a rotating magnetized plasma. It is shown that these effects suppress the rotational-convective instability. © 2008 Bull. Georg. Natl. Acad. Sci. Key words: magneto-rotational instability (MRI), axisymmetric perturbatio ..."
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ABSTRACT. The drift effects are incorporated into the theory of instabilities in a rotating magnetized plasma. It is shown that these effects suppress the rotational-convective instability. © 2008 Bull. Georg. Natl. Acad. Sci. Key words: magneto-rotational instability (MRI), axisymmetric
NUMERICAL SIMULATIONS OF Z-PINCH EXPERIMENTS TO CREATE SUPERSONIC DIFFERENTIALLY-ROTATING PLASMA FLOWS
"... Abstract. In the context of high energy density laboratory astrophysics, we aim to produce and study a rotating plasma relevant to accre-tion discs physics. We devised an experimental setup based on a mo-dified cylindrical wire array and we studied it numerically with the three-dimensional, resistiv ..."
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-dimensional, resistive magneto-hydrodynamic code GORGON. The simulations show that a rotating plasma cylinder is formed, with typical rotation velocity ∼35 km/s and Mach number ∼5. In addi-tion, the plasma ring is differentially rotating and strongly radiatively cooled. The introduction of external magnetic fields
Simulation of Alpha Particles in Rotating Plasma Interacting With a Stationary Ripple
, 2011
"... Abstract—Superthermal E ×B rotation can provide magne-tohydrodynamic stability and enhanced confinement to axisym-metric mirrors. However, the rotation speed has been limited by phenomena at end electrodes. A new prediction is that rotation might instead be produced using a magnetic ripple and alpha ..."
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Abstract—Superthermal E ×B rotation can provide magne-tohydrodynamic stability and enhanced confinement to axisym-metric mirrors. However, the rotation speed has been limited by phenomena at end electrodes. A new prediction is that rotation might instead be produced using a magnetic ripple
Collisionless Damping of Fast MHD Waves in Magneto-rotational Winds
, 2005
"... We propose collisionless damping of fast MHD waves as an important mechanism for the heating and acceleration of winds from rotating stars. Stellar rotation causes magnetic field lines anchored at the surface to form a spiral pattern and magneto-rotational winds can be driven. If the structure is a ..."
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We propose collisionless damping of fast MHD waves as an important mechanism for the heating and acceleration of winds from rotating stars. Stellar rotation causes magnetic field lines anchored at the surface to form a spiral pattern and magneto-rotational winds can be driven. If the structure is a
Collisionless Damping of Fast MHD Waves in Magneto-rotational Winds
, 2005
"... We propose collisionless damping of fast MHD waves as an important mechanism for the heating and acceleration of winds from rotating stars. Stellar rotation causes magnetic field lines anchored at the surface to form a spiral pattern and magneto-rotational winds can be driven. If the structure is a ..."
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We propose collisionless damping of fast MHD waves as an important mechanism for the heating and acceleration of winds from rotating stars. Stellar rotation causes magnetic field lines anchored at the surface to form a spiral pattern and magneto-rotational winds can be driven. If the structure is a
ABSTRACT Title of dissertation: WAVES IN PLASMAS GENERATED BY A ROTATING MAGNETIC FIELD AND IMPLICATIONS TO RADIATION BELTS
"... The interaction of rotating magnetic fields (RMF) with magnetized plasmas is a fundamental plasma physics problem with implications to a wide range of areas, including laboratory and space plasma physics. Despite the importance of the topic the basic physics of the phenomenon remains unexplored. An ..."
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The interaction of rotating magnetic fields (RMF) with magnetized plasmas is a fundamental plasma physics problem with implications to a wide range of areas, including laboratory and space plasma physics. Despite the importance of the topic the basic physics of the phenomenon remains unexplored
GLOBAL SIMULATIONS OF DIFFERENTIALLY ROTATING MAGNETIZED DISKS: FORMATION OF LOW-BETA FILAMENTS AND STRUCTURED CORONA
, 1999
"... We present the results of three-dimensional global magnetohydrodynamic (MHD) simulations of the Parker-shearing instability in a differentially rotating torus initially threaded by toroidal magnetic fields. An equilibrium model of magnetized torus is adopted as an initial condition. When β0 = Pgas/P ..."
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/Pmag ∼ 1 at the initial state, magnetic flux buoyantly escapes from the disk and creates loop-like structures similar to those in the solar corona. Inside the torus, growth of non-axisymmetric magneto-rotational (or Balbus & Hawley) instability generates magnetic turbulence. Magnetic field lines
Results 1 - 10
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37
