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5,578
Chaos in Accretion Disk Dynamos?
, 1995
"... Accretion disks appear to be favourable places for dynamo action, because of their strong differential rotation. A simple estimate of the strength of an accretion disk dynamo indicates that it will be highly nonlinear. In spite of this, most studies hitherto have assumed a linear model for the dyna ..."
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Cited by 1 (0 self)
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Accretion disks appear to be favourable places for dynamo action, because of their strong differential rotation. A simple estimate of the strength of an accretion disk dynamo indicates that it will be highly nonlinear. In spite of this, most studies hitherto have assumed a linear model
The StandardAccretion Disk Dynamo
, 1994
"... We consider the classic MHD turbulent dynamo operating in a thin, Keplerian accretion disk powered by turbulent viscous stress. The character of the turbulence is encapsulated into two constant parameters: the ShakuraSunyaev dimensionless viscosity, ff SS , and the Coriolis number,\Omega = 2ø c ..."
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We consider the classic MHD turbulent dynamo operating in a thin, Keplerian accretion disk powered by turbulent viscous stress. The character of the turbulence is encapsulated into two constant parameters: the ShakuraSunyaev dimensionless viscosity, ff SS , and the Coriolis number,\Omega = 2ø
1 Galactic and Accretion Disk Dynamos
, 1998
"... Dynamos in astrophysical disks are usually explained in terms of the standard alphaomega mean field dynamo model where the local helicity generates a radial field component from an azimuthal field. The subsequent shearing of the radial field gives rise to exponentially growing dynamo modes. There a ..."
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Dynamos in astrophysical disks are usually explained in terms of the standard alphaomega mean field dynamo model where the local helicity generates a radial field component from an azimuthal field. The subsequent shearing of the radial field gives rise to exponentially growing dynamo modes
ASTRONOMY AND ASTROPHYSICS Accretiondisk dynamo models with dynamoinduced alphaeffect
, 1999
"... Abstract. A nonlinear 1D dynamo model with a heuristic αansatz for magnetic fieldinduced turbulence is considered to be growing for weak fields and suppressed by strong fields. The amplification of initial magnetic fields is regarded in accretion disks like both Kepler disks and galaxies. The solu ..."
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Abstract. A nonlinear 1D dynamo model with a heuristic αansatz for magnetic fieldinduced turbulence is considered to be growing for weak fields and suppressed by strong fields. The amplification of initial magnetic fields is regarded in accretion disks like both Kepler disks and galaxies
AccretionDisk Dynamo Models With DynamoInduced AlphaEffect
, 1999
"... . A nonlinear 1D dynamo model with a heuristic ffansatz for magnetic fieldinduced turbulence is considered growing for weak fields and suppressed by strong fields. The amplification of initial magnetic fields is regarded in accretion disks like both Kepler disks and galaxies. The solutions for the ..."
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. A nonlinear 1D dynamo model with a heuristic ffansatz for magnetic fieldinduced turbulence is considered growing for weak fields and suppressed by strong fields. The amplification of initial magnetic fields is regarded in accretion disks like both Kepler disks and galaxies. The solutions
Large Scale Azimuthal Structures Of Turbulence In Accretion Disks Dynamo triggered variability of accretion.
"... ar ..."
AND ASTROPHYSICS On the dynamo driven accretion disks
, 1998
"... Abstract. Weadd the − effect in the dynamo driven accretion disk model proposed by Tout & Pringle (1992), i.e., a dynamo model depends on the physical processes such as Parker instability, BH instability, magnetic field reconnection and−! mean field dynamo as well. The − effect in the dynamo ..."
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Abstract. Weadd the − effect in the dynamo driven accretion disk model proposed by Tout & Pringle (1992), i.e., a dynamo model depends on the physical processes such as Parker instability, BH instability, magnetic field reconnection and−! mean field dynamo as well. The − effect in the dynamo
The Disk Accretion Rate For Dynamo Generated Turbulence
"... Dynamogenerated turbulence is simulated in a modified shearing box approximation that removes scale invariance and allows finite accretion rates for a given distance from the central object. The effective ShakuraSunyaev viscosity parameter, ff SS , is estimated in three different ways using the re ..."
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Cited by 8 (6 self)
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Dynamogenerated turbulence is simulated in a modified shearing box approximation that removes scale invariance and allows finite accretion rates for a given distance from the central object. The effective ShakuraSunyaev viscosity parameter, ff SS , is estimated in three different ways using
The Disk Accretion Rate For Dynamo Generated Turbulence
"... Dynamogenerated turbulence is simulated in a modified shearing box approximation that removes scale invariance and allows finite accretion rates for a given distance from the central object. The effective ShakuraSunyaev viscosity parameter, ff SS , is estimated in three different ways using the re ..."
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Dynamogenerated turbulence is simulated in a modified shearing box approximation that removes scale invariance and allows finite accretion rates for a given distance from the central object. The effective ShakuraSunyaev viscosity parameter, ff SS , is estimated in three different ways using
AN INCOHERENT alphaOmega DYNAMO IN ACCRETION DISKS
, 1997
"... We use the meanfield dynamo equations to show that spatially and temporally incoherent fluctuations in the helicity in mirrorsymmetric turbulence in a shearing flow can generate a largescale, coherent magnetic field. We illustrate this effect with simulations of a few simple systems. For statisti ..."
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Cited by 1 (0 self)
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We use the meanfield dynamo equations to show that spatially and temporally incoherent fluctuations in the helicity in mirrorsymmetric turbulence in a shearing flow can generate a largescale, coherent magnetic field. We illustrate this effect with simulations of a few simple systems
Results 1  10
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5,578