arXiv subjects

G. Ruediger

Publications and source records attributed to G. Ruediger.

49 records · Page 3Linked to original sources

arXiv2005

The stability of MHD Taylor-Couette flow with current-free spiral magnetic fields between conducting cylinders

We study the magnetorotational instability in cylindrical Taylor-Couette flow, with the (vertically unbounded) cylinders taken to be perfect conductors, and with externally imposed spiral magnetic fields. The azimuthal component of this field is generated by an axial current inside the inner cylinder, and may be slightly stronger than the axial field. We obtain an instability beyond the Rayleigh line, for Reynolds numbers of order 1000 and Hartmann numbers of order 10, and independent of the (small) magnetic Prandtl number. For experiments with R_out = 2 R_in = 10 cm and Omega_out = 0.27 Omega_in, the instability appears for liquid sodium for axial fields of ~20 Gauss and axial currents of \~1200 A. For gallium the numbers are ~50 Gauss and ~3200 A. The vertical cell size is about twice the cell size known for nonmagnetic experiments.

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arXiv2005

Three-dimensional stability of the solar tachocline

The three-dimensional, hydrodynamic stability of the solar tachocline is investigated based on a rotation profile as a function of both latitude and radius. By varying the amplitude of the latitudinal differential rotation, we find linear stability limits at various Reynolds numbers by numerical computations. We repeated the computations with different latitudinal and radial dependences of the angular velocity. The stability limits are all higher than those previously found from two-dimensional approximations and higher than the shear expected in the Sun. It is concluded that any part of the tachocline which is radiative is hydrodynamically stable against small perturbations.

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arXiv2005

Differential rotation on the lower main sequence

We compute the differential rotation of main sequence stars of the spectral types F, G, K, and M by solving the equation of motion and the equation of convective heat transport in a mean-field formulation. For each spectral type the rotation rate is varied to study the dependence of the surface shear on this parameter. The resulting rotation patterns are all solar-type. The horizontal shear turns out to depend strongly on the effective temperature and only weakly on the rotation rate. The meridional flow depends more strongly on the rotation rate and has different directions in the cases of very slow and very fast rotation, respectively.

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arXiv2005

Anti-solar differential rotation

The differential rotation of anti-solar type detected by observations for several stars may result from a fast meridional flow. The sufficiently intensive meridional circulation may be caused by large-scale thermal inhomogeneities or, perhaps, by tidal forcing from a companion star. First results of simulations of the anti-solar rotation of a giant star with magnetically induced thermal inhomogeneities are presented. Perspectives for observational check of the theory are discussed.

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arXiv2005

A numerical MHD model for the solar tachocline

There are successful approaches to explain the formation of the tachocline by a poloidal magnetic field in the solar core. We present here the first MHD simulations of the solar tachocline which self-consistently include the meridional circulation. We show that the meridional flow significantly changes the shape and the characteristics of the tachocline. We find that after the inclusion of the meridional circulation, a tachocline can be formed even when the poloidal field lines are crossing the boundary between the radiative zone and the convection zone. We also discuss the effects of the magnetic Prandtl number as well as of the magnetic Reynolds number on the properties of the tachocline. The tachocline is much thinner for higher magnetic Reynolds numbers and/or lower magnetic Prandtl numbers. We expect that a poloidal magnetic seed field of around 1 G will be sufficient to produce the tachocline of the Sun. However, the model requires the initial magnetic field to be in a narrow range for satisfying tachocline solutions. The simulations including a stable temperature gradient produce a shallower as well as slower meridional circulation than the ones without it, as desired from the Lithium abundance at the solar surface.

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arXiv2005

The influence of the Hall effect on the global stability of cool protostellar disks

The influence of the Hall effect on the global stability of cool Kepler disks under the influence of an axial magnetic field is considered. For sufficiently large magnetic Reynolds numbers Rm the magnetorotational instability (MRI) exists in a finite interval of magnetic field amplitudes, $B$_{min} < $B$ < $B$_{max}. For Kepler disks the pure MRI needs both rather high Rm (representing the needed electrical conductivity) as well as $B$_{min} of order 0.1 G. The magnetic field pattern resulting from our global and linear calculations is of quadrupolar parity. For magnetic fields $antiparallel$ to the rotation axis the Hall effect reduces the minimum magnetic Reynolds number by about one order of magnitude. The $B$_{min}, however, is even (sightly) increased (see Fig. 6). For magnetic fields $parallel$ to the rotation axis the Hall effect drives its own instability without the action of the Lorentz force. The corresponding critical magnetic Reynolds number proves to be larger with Hall effect (Rm ~ 10) than without Hall effect (Rm ~ 7) so that the Hall effect for parallel fields even disturbs the formation of MHD-instability in cool protoplanetary disks. If the disk is supercritical then the main result of the Hall effect for positive fields is the strong reduction of the minimum magnetic field amplitude which is necessary to start the instability. Observations must show whether in star-forming regions the rotation axis and the magnetic field orientation are correlated or are anticorrelated. If the magnetic fields are high enough then our model predicts the dominance of fields antiparallel to the rotation axis.

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arXiv2005

Stability of density-stratified viscous Taylor-Couette flows

The stability of density-stratified viscous Taylor-Couette flows is considered using the Boussinesq approximation but without any use of the short-wave approximation. The flows which are unstable after the Rayleigh criterion (\hat μ<\hat η^2, with \hat μ=Ω_{out}/Ω_{in} and \hat η= R_{in}/R_{out}) now develop overstable axisymmetric Taylor vortices. For the considered wide-gap container we find the nonaxisymmetric modes as the most unstable ones. The nonaxisymmetric modes are unstable also beyond the Rayleigh line. For such modes the instability condition seems simply to be \hatμ<1 as stressed by Yavneh, McWilliams & Molemaker (2001). However, we never found unstable modes for too flat rotation laws fulfilling the condition \hat μ>\hat η. The Reynolds numbers rapidly grow to very high values if this limit is approached (see Figs. 3 and 4). Also striking is that the marginal stability lines for the higher $m$ do less and less enter the region beyond the Rayleigh line so that we might have to consider the stratorotational instability as a 'low-$m$ instability'. The applicability of these results to the stability problem of accretion disks with their strong stratification and fast rotation is shortly discussed.

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arXiv2004

Geodynamo alpha-effect derived from box simulations of rotating magnetoconvection

The equations for fully compressible rotating magnetoconvection are numerically solved in a Cartesian box assuming conditions roughly suitable for the geodynamo. The mean electromotive force describing the generation of mean magnetic flux by convective turbulence in the rotating fluid is directly calculated from the simulations, and the corresponding alpha-coefficients are derived. Due to the very weak density stratification the alpha-effect changes its sign in the middle of the box. It is positive at the top and negative at the bottom of the convection zone. For strong magnetic fields we also find a clear downward advection of the mean magnetic field. Both of the simulated effects have been predicted by quasi-linear computations (Soward, 1979; Kitchatinov and Ruediger, 1992). Finally, the possible connection of the obtained profiles of the EMF with mean-field models of oscillating alpha^2-dynamos is discussed.

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arXiv2004

Differential rotation of main sequence F stars

The differential rotation of a 1.2 $M_\odot$ zero age MS star (spectral type F8) is computed and the results are compared with those from a similar model of the Sun. The rotation pattern is determined by solving the Reynolds equation including the convective energy transport. The latter is anisotropic due to the Coriolis force causing a horizontal temperature gradient of ~ 7 K between the poles and the equator. Comparison of the transport mechanisms of angular momentum (the eddy viscosity, the $Λ$-effect and the meridional flow) shows that for the F star the $Λ$-effect is the most powerful transporter for rotation periods of 7 d or less. In the limit of very fast rotation the $Λ$-effect is balanced by the meridional flow alone and the rotation is nearly rigid. The rotation pattern found for the F star is very similar to the solar rotation law, but the horizontal shear is about twice the solar value. As a function of the rotation period, the total equator-pole difference of the angular velocity has a (slight) maximum at a period of 7 d and (slowly) vanishes in both the limiting cases of very fast and very slow rotation. A comparison of the solar models with those for the F-type star shows a much stronger dependence of the differential surface rotation on the stellar luminosity rather than on the rotation rate.

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arXiv2004

The eddy heat-flux in rotating turbulent convection

The three components of the heat-flux vector $F =ρC_p are numerically computed for a stratified rotating turbulent convection using the NIRVANA code in a flat box. The latitudinal component $F_θ$ proves to be negative (positive) in the northern (southern) hemisphere so that the heat always flows towards the poles. As a surprise, the radial heat-flux $F_r$ peaks at the equator rather than at the poles (Taylor numbers O(10^6)). The same behavior is observed for the radial turbulence intensity $ $ which for \emph{free} turbulence is also believed to peak at the poles (see Eq. (19) below). As we can show, however, the consequences of this unexpected result (also obtained by Kaepylae, Korpi and Tuominen 2004) for the theory of differential rotation are small as mainly the $F_θ$ is responsible to solve the `Taylor number puzzle'. In all our simulations the azimuthal component $F_ϕ$ proves to be negative so that the rotating turbulence produces an westwards directed azimuthal heat-flux which should be observable. Fluctuations with higher temperature are expected to be anticorrelated with their own angular velocity fluctuations. We find this rotation-induced result as understandable as the $F_ϕ$ is closely related to the radial Λ-effect which is known to be also negative in stratified and rapidly rotating convection zones.

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arXiv2002

Magnetoconvection and dynamo coefficients: II. Field-direction dependent pumping of magnetic field

We study the pumping of magnetic flux in three-dimensional compressible magnetoconvection in the context of stellar dynamos. The simulation domain represents a rectangular section from the lower part of a stellar convection zone plus the underlying stably stratified layer, with a total depth of up to five pressure scale heights. Once convection has attained a statistically stationary state, a magnetic field is introduced. The magnetic field is subsequently modified by the convective motions, and the resulting pumping effects are isolated by calculating various coefficients of the expansion of the electromotive force, uxb, in terms of components of the mean magnetic field. The dependence of the pumping effects on rotation, latitude and other parameters is studied. First numerical evidence is found for the existence of pumping effects in the horizontal directions, unless the rotation axis coincides with the vertical axis, as is the case on the poles. Evidence is found that the pumping effects act differently on different components of the mean magnetic field. Latitudinal pumping is mainly equatorward for toroidal field, and can be poleward for poloidal field. Longitudinal pumping is mainly retrograde for the radial field but prograde for the latitudinal field. The pumping effect in the vertical direction is found to be dominated by the diamagnetic effect, equivalent to a predominating downward advection with a maximum speed in the turbulent case of about 10 percent of the rms convective velocity. Where possible, an attempt is made to identify the physical origin of the effect. Finally, some consequences of the results for stellar dynamos are discussed.

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arXiv2002

Parity properties of an advection-dominated solar $α^2\Om$-dynamo

We have developed a high-precision code which solves the kinematic dynamo problem both for given rotation law and meridional flow in the case of a low eddy diffusivity of the order of $10^{11}$ cm$^2$/s known from the sunspot decay. All our models work with an \alf-effect which is positive (negative) in the northern (southern) hemisphere. It is concentrated in radial layers located either at the top or at the bottom of the convection zone. We have also considered an \alf-effect uniformly distributed in all the convection zone. In the present paper the main attention is focused on i) the parity of the solution, ii) the form of the butterfly diagram and iii) the phase relation of the resulting field components. If the helioseismologically derived internal solar rotation law is considered, a model without meridional flow of high magnetic Reynolds number (corresponding to low eddy diffusivity) fails in all the three issues in comparison with the observations. However, a meridional flow with equatorial drift at the bottom of the convection zone of few meters by second can indeed enforce the equatorward migration of the toroidal magnetic field belts similar to the observed butterfly diagram but, the solution has only a dipolar parity if the (positive) \alf-effect is located at the base of the convection zone rather than at the top. We can, therefore, confirm the main results of a similar study by Dikpati & Gilman (2001).

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arXiv2001

The stability of axisymmetric Taylor-Couette flow in hydromagnetics

The linear marginal instability of an axisymmetric MHD Taylor-Couette flow of infinite vertical extension is considered. The dependence of the flow stability on magnetic Prandtl number, Pm, and gap-width between rotating cylinders is investigated. There is an unstability for flows with resting outer cylinder even without a magnetic field. Nevertheless, there are solutions with smaller critical Reynolds numbers for certain (weak) magnetic fields. These solutions, however, exist for not too small Pm or large enough gap. For hydrodynamically stable flow, we found that a magnetic field amplitude always exsits where the critical Reynolds number is minimal. In all calculated cases the minimal critical Reynolds numbers are running with 1/Pm for small Pm and the critical Reynolds numbers exceed value of 10^6 for Pm of sodium (10^{-5}) or gallium (10^{-6}).

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