6 July 2019

Most flows in nature and engineering are turbulent because of their large velocities and spatial scales. Laboratory experiments of rotating quasi-Keplerian flows, for which the angular velocity decreases radially but the angular momentum increases, are however laminar at Reynolds numbers exceeding one million. This is in apparent contradiction to direct numerical simulations showing that in these experiments turbulence transition is triggered by the axial boundaries. We here show numerically that as the Reynolds number increases turbulence becomes progressively confined to the boundary layers and the flow in the bulk fully relaminarizes. Our findings support that turbulence is unlikely to occur in isothermal constant density quasi-Keplerian flows.

Boundary-layer turbulence in experiments of quasi-Keplerian flows] Boundary-layer turbulence in experiments of quasi-Keplerian flows Jose M. Lopez and Marc Avila] JOSEM.LOPEZ, and MARCAVILA

1 Introduction

Understanding the origin of turbulence in accretion disks is a long-standing problem in astrophysics (Ji & Balbus 2013). The simplest model for the flow of gas in an accretion disk consists of an isothermal incompressible constant density fluid rotating with a Keplerian angular velocity , where is the distance to the accreting central object. Despite the hydrodynamic stability of such flows to small disturbances (Rayleigh 1917), the possibility of a nonlinear transition to turbulence via finite-amplitude disturbances is not precluded. However, this has not been demonstrated and so several mechanisms capable of destabilizing Keplerian flows have been proposed in the literature (see Turner et al. 2014, for a recent review). Prominent amongst these is the magnetorotational instability (MRI, see Balbus & Hawley 1998; Balbus 2003), which can drive vigorous turbulence and transport angular momentum at rates required for accretion to occur. However, the MRI operates in ionized disks only and so it does not apply to cool protostellar disks. There are many mechanisms that might give rise to turbulence in the absence of magnetic fields: baroclinic instabilities (Klahr & Bodenheimer 2003; Johnson & Gammie 2006; Petersen et al. 2007), instabilities driven by radial (Goldreich & Schubert 1967; Fricke 1968; Urpin & Brandenburg 1998) or axial stratification (Shalybkov & Rüdiger 2005; Dubrulle et al. 2005b; Marcus et al. 2015), crossflow instabilities (Kerswell 2015), convective instabilities (Lin & Papaloizou 1980; Ryu & Goodman 1992) or self-gravitation (Toomre 1964; Lin & Pringle 1987). Nevertheless, their applicability to accretion disks is still under investigation. Whereas there is an understanding of the underlying instability mechanisms, their non-linear evolution and saturated state have still to be studied in realistic disk simulations with the proper radiation transport and analysing the effect of the boundary conditions.

In general, the lack of observational evidence and the computational limitations in simulating the extreme parameter values governing the dynamics of accretion disks makes them a particularly difficult object to study (see e.g. Miesch et al. 2015). This has motivated the development of laboratory experiments capturing the essential physics at play. Quasi-Keplerian flows, for which the angular velocity decreases radially, whereas the angular momentum increases, can in principle be realized in laboratory experiments of fluids between two concentric rotating cylinders (Taylor–Couette flow). If the cylinders are assumed to be infinite in length the basic laminar flow is purely azimuthal


where () and () are the angular velocity and radius of the inner (outer) cylinder. Provided that but then the basic Couette flow (1) is quasi-Keplerian. Despite the apparent simplicity of this model, laboratory realizations of quasi-Keplerian velocity profiles are fraught with difficulty. In practice, the viscous interaction between fluid and end-plates confining the fluid in the axial direction results in secondary flows, also known as Ekman circulation (EC). EC can extend deep into the bulk flow and cause the azimuthal velocity to significantly deviate from the theoretical profile (1) as the rotation speeds increase (Richard & Zahn 1999; Hollerbach & Fournier 2004).

Pioneering experiments of quasi-Keplerian flows were conducted by Ji et al. (2006), who used a short height-to-gap aspect ratio and end plates split into two independently rotating rings. Ji et al. (2006) carefully adjusted the rotation speed of the rings so as to minimize EC and measured Reynolds stresses in the bulk. They concluded that the bulk flow was laminar despite reaching Reynolds numbers of up to . These results were questioned by Paoletti & Lathrop (2011), who used a tall apparatus with end plates attached to the outer cylinder. Paoletti & Lathrop (2011) split the inner cylinder vertically in three sections and measured the torque on the central section so as to reduce the effect of the end plates in their measurements. However, Avila (2012) performed direct numerical simulations reproducing the precise geometry of Ji et al. (2006) and Paoletti & Lathrop (2011) and showed that in both setups strong EC render the flows turbulent at Reynolds numbers as low as . Although his simulations were consistent with the turbulent flows observed by Paoletti & Lathrop (2011), as confirmed by subsequent experiments (Nordsiek et al. 2015), they were in apparent contradiction with the laminar flows observed by Ji et al. (2006).

More recently, Edlund & Ji (2014) attributed this discrepancy to the large gap in Reynolds numbers between simulations and experiments. They directly measured velocity profiles in a new experimental setup and showed that if the end plates are rotated within a certain range of velocities, hereafter referred to as optimal boundary conditions, quasi-Keplerian Couette flow (1) is obtained and remains stable even when subject to strong disturbances.

We here perform direct numerical simulations of experimental quasi-Keplerian flows for Reynolds numbers up to . We show that as the Reynolds number increases, turbulence becomes progressively confined to thin boundary layers at the end plates. As a result laminar quasi-Keplerian profiles are realized in the bulk of the experiment. We provide a detailed picture of the relaminarisation process and the role of the boundary conditions for two distinct configurations studied by Edlund & Ji (2015). Our results bridge the gap between experiments and previous simulations and support the experimental conclusion that constant density isothermal quasi-Keplerian Taylor–Couette flows are stable.

2 Specification of the problem and numerical methods

A fluid of kinematic viscosity is contained in the annular gap between two vertical concentric cylinders of length and radii and . The subindex () denotes the inner (outer) cylinder and is the gap width. Differential rotation is generated by rotating the cylinders at independent angular velocities and . The shear Reynolds number, , and the rotation number, , were chosen as control parameters


where and are the shear and rotation speed of the basic Couette flow (1) evaluated at the mean geometric radius . The rotation number allows for a clear distinction between cyclonic () and anticyclonic () flows. It has been widely used to characterize different rotation regimes of the Taylor–Couette experiments and to compare results for different geometries (Dubrulle et al. 2005a; Ravelet et al. 2010; Paoletti et al. 2012).

In astrophysics is used to characterise the rotation law. The flow is quasi-Keplerian if () is chosen within the range (). In the simulations presented in this paper, () was chosen, corresponding to the experiments of Ji et al. (2006) and simulations of Avila (2012), and close to the value chosen by Edlund & Ji (2014). Their apparatus is axially bounded by two horizontal plates which rotate differentially with respect to the cylinders. These end plates can be further split into several independently rotating rings whose angular velocities can be adjusted to best approximate (1). The geometry of their apparatus is fully specified by two dimensionless parameters: the radius ratio, , and the length-to-gap aspect ratio, .

Different configurations of this apparatus differ from one another in the number of rings into which the end plates are split. Here, we study in detail two configurations, the so-called HTX and wide ring (WR), in which only one ring rotates differentially with respect to the cylinders. In the HTX configuration (dashed line in figure 1 ) the end plates are split in three rings. The inner and outer rings are attached to the cylinders, whereas the central ring rotates at an angular velocity intermediate to those of the cylinders. In the WR configuration (solid line in figure 1 ) there is a single ring that spans the entire annulus but also rotates independently. The dot-dashed line in figure 1 illustrates the boundary conditions of Ji et al. (2006), who designed their device to study the magnetorotational instability by using electrically conducting fluids and an imposed axial magnetic field. We will refer to this configuration as MRI.

Figure 1: Rotation speed of the end plates () normalised by the rotation speed of the inner cylinder () in the WR, HTX and MRI configurations. Torque () on the cylinders and end plates in the the WR configuration as a function of . is normalised by the torque of the Couette profile (1) (). The optimal rotation range is enclosed in a rectangular box. Same as in for the HTX configuration. In both and torques were computed at .

2.1 Numerical method

The Navier–Stokes equations have been solved in cylindrical coordinates using a second order time-splitting method (Hughes & Randriamampianina 1998; Mercader et al. 2010). The spatial discretization is via a Galerkin-Fourier expansion in and Chebyshev collocation in and . Hereafter the radial , azimuthal and axial velocities are normalized with respect to the characteristic velocity used in the definition of the shear Reynolds number (2). The code used is a parallelized version of a spectral solver that has been widely tested (Avila et al. 2008; Lopez & Marques 2015; Lopez et al. 2015). Details of the parallelization strategy can be found in Shi et al. (2015).

In the WR and HTX configurations there are discontinuities in the angular velocity at the junctions where elements rotating at different speeds meet. For an accurate use of spectral techniques these discontinuities must be regularised (see Lopez & Shen (1998)). In the WR configuration this is accomplished through the introduction of two exponential functions in the form


whereas in the HTX configuration two hyperbolic tangent functions are used


where and are the radial locations at which the central ring meets the outer and inner rings respectively. In both cases was used.

The numerical resolution was carefully chosen in order to meet several requirements. First, we checked that the total angular momentum flux through cylinders and end plates vanished in the statistically stationary regime. Second, we gradually increased the number of collocation points until converged values of the torque at the inner and outer cylinders were obtained. Finally, we checked the spectral convergence of the code using the infinity norm of the spectral coefficients of the computed solutions, defined as for the radial direction, and analogously for the axial and azimuthal directions. An example of spatial convergence is illustrated in figure 2, which shows , with , of the radial velocity for a solution corresponding to the HTX configuration at . This solution was computed with and Chebyshev axial points in and , and Fourier modes in . In all simulations the trailing coefficients of the spectral expansion were at least four orders of magnitude smaller than the leading coefficients. Table 1 shows the spatial resolution corresponding to the largest simulated for each configuration. The reader is referred to Brauckmann & Eckhardt (2013) for a comprehensive analysis on the suitability of these convergence criteria for Taylor–Couette flows at large Reynolds numbers.

Figure 2: Convergence of the spectral coefficients of the radial velocity in the three spatial directions using the infinity norm. It corresponds to a simulation of the HTX configuration at . This solution has been computed with Chebyshev radial points, Fourier modes and Chebyshev axial points.
WR 128 256 544 47630
HTX 392 642 224 32180
MRI 192 192 288 12874
Table 1: Maximum spatial resolution and for each configuration. , and indicate the number of spectral modes in the radial, azimuthal and axial directions, respectively.

2.2 Optimal boundary conditions

Following Edlund & Ji (2015), we here determine the optimal rotation speed of the end plates from a balance of the angular momentum fluxes (torque) through the boundaries of the apparatus. In particular, optimal rotation is identified when the torque at the end plates () becomes zero, so that the torque on the cylinders has the same magnitude but opposite sign, , as in the infinite-cylinder idealization. Figures 1 and show the torque across the cylinders and end plates as a function of for solutions computed at in both configurations. In agreement with Edlund & Ji (2015), in both cases there exist a narrow range of for which is approximately fulfilled (rectangular box in figures 1 and ). For our simulations we chose (HTX) and (WR). Note that the torque in the WR configuration is substantially larger than in the HTX setup. The reason for this will be discussed in §3, along with the description of the secondary flows in both setups.

3 Basic flow and transition to turbulence

3.1 Wide ring

Figure 3 shows that in the WR configuration the secondary EC cells extend over the entire annulus. Near the end plates, the flow is deflected radially towards the cylinders leading to two Ekman vortices with opposite sense of circulation. The size and intensity of these vortices change with and it is only under optimal boundary conditions that these have nearly equal size and strength (). When the fluid reaches the cylinders it is transported from the end plates to the mid-plane over Stewartson boundary layers. As a result, two strong radial jets emerge from the cylinders and displace the flow towards mid-gap. The circulation cycle is then closed by two vertical cells that transport the fluid back to the end plates.

These large-scale secondary flows lead to linear instabilities that manifest themselves at the equatorial region (Avila et al. 2008; Avila 2012), and cause a transition to turbulence at low values of . Figure 4 shows, through isosurfaces of the radial velocity , the location of the most unstable mode at the onset of instability. Note that the axisymmetric part of has been subtracted to facilitate visualization. The flow pattern emerging from this primary transition, which takes place at , is a rotating wave with azimuthal wave number . As is further increased, the flow undergoes secondary instabilities leading to either rotating waves with different or quasi-periodic states, and becomes eventually turbulent at . Figure 4 shows isosurfaces of for a turbulent state computed at . Interestingly, the turbulence does not extend towards the end plates but remains concentrated around the mid-plane.

Figure 3: Meridional sections showing color maps of the radial (left panel) and axial (right panel) velocities in the WR and HTX configurations. The solutions depicted correspond in both cases to laminar flow computed at . In all figures shown in this paper, dark (light) regions indicate zones of positive (negative) velocities. There are contours equally distributed in , and , for the WR and HTX configurations respectively.

3.2 Htx

Figure 3 shows that in the HTX configuration the secondary EC is mainly confined to the vicinity of the end plates. Because of the split end plates, the radial flow along them is arranged in four alternating outward-inward vortices which direct the flow towards the junctions between the rings. The pair of vortices located at the outermost part of the end plates are significantly larger and more intense () than those arising near the inner cylinder (). Significant axial transport of fluid towards the mid-plane occurs only in a narrow region around mid-gap. However, the flow does not reach the mid-plane, as it is recirculated towards the inner cylinder by a strong radial inflow that arise at an approximately intermediate distance between the end plates and the equatorial region. Finally, the flow is pushed back towards the end plates by axial velocities arising in the regions near the cylinders. A comparison with the WR configuration reveals that the substantial difference in torque shown in section 2.2 is caused by the influence of the Stewartson boundary layers that form at the cylinders in the WR configuration. These produce strong azimuthal velocity gradients near the cylinders, which result in a significant increase of the torque as compared with that in the HTX configuration.

The meridional circulation in the HTX configuration becomes unstable at . The instability results in a rotating wave with localised at the end plates (see figure 4 ), and the flow becomes quickly chaotic as is increased (). Nevertheless, the turbulence remains primarily localised near the upper and lower third of the experiment (see figure 4 ), so that the zonal flow at the equatorial region is barely affected by the secondary flows and nearly matches a quasi-Keplerian velocity profile, see §4.2.

Figure 4: and show isosurfaces of the radial velocity of the leading eigenmodes near the onset of instability. The axisymmetric component has been subtracted to facilitate visualization of the spatial structure of the unstable mode. Equatorial rotating wave with computed at in the WR configuration, Rotating wave with localised near the end plates for in the HTX configuration. and show isosurfaces of the radial velocity for turbulent states computed at in the WR and HTX configurations. There are isosurfaces equally distributed across and in the WR and HTX configurations respectively.

4 Dynamics at high Reynolds numbers

As the rotation of the cylinders is increased the spatial arrangement of the secondary flows undergo significant changes in both configurations, which alter the structure of the resulting turbulence. While this transition occurs smoothly with increasing , we here distinguish between low and high Reynolds numbers using as an approximate threshold, beyond which the changes described in this section begin to become apparent.

4.1 Wide ring

Figure 5 shows the structure of the time-averaged secondary flow for the WR configuration at . Here the radial jets that emanate from the cylinders at the equatorial region do not extend across the entire gap, but remain localised in regions closer to the cylinders. The gradual displacement of these jets towards the cylinders as increases is accompanied by the emergence of two pairs of radial flow cells on top and bottom of them. These radial cells recirculate the flow towards the cylinders, so that the vertical transport of fluid from the equator towards the end plates that closes the Ekman circulation cycle is also confined to the vicinity of the cylinders. As a result, the radial and axial velocities are nearly zero over the central region of the gap and the flow becomes essentially azimuthal in the bulk, resulting in vanishing Reynolds stresses.

The turbulent dynamics of this system is confined to the region in which the radial equatorial jets penetrate into the bulk flow. Hence as increases and the secondary flows occupy regions closer to the cylinders, significant turbulent fluctuations are only found in the vicinity of the cylinders. Figure 6 clearly illustrates the progressive localisation of the turbulence near the cylinders as increases. Interestingly, turbulent structures occur mainly near the inner cylinder, which could be related to the large curvature of the apparatus ().

Figure 7 shows the mean azimuthal velocity for . With the exception of the zones near the cylinders, where the flow is obviously affected by the turbulence, it is observed that is nearly independent of the axial coordinate. This is confirmed in figure 7 , where is shown at three different axial locations. Although these profiles collapse together, they differ substantially from the desired quasi-Keplerian velocity profile (1), shown as a (black) solid line in figure 7 . Interestingly, despite vanishing fluctuations (and hence Reynolds stresses) in the bulk, the profile is far from ideal because of the effect of the global EC.

Figure 5: Meridional sections showing color maps of the mean radial (left panel) and axial (right panel) velocities in the WR and HTX configurations. The solutions depicted were computed at in and in . There are contours equally distributed in , and , for the WR and HTX configurations respectively.

Figure 6: Evolution of the isosurfaces of the radial velocity with in both configurations. There are isosurfaces corresponding to in both cases. Note that plots corresponding to the WR configuration are slightly tilted to better illustrate the gradual displacement of the turbulence towards the cylinders.

4.2 Htx

Figure 5 shows the structure of the time-averaged secondary meridional flow for the HTX configuration at . As increases both radial and axial velocities are progressively confined to the end plates, resulting in an increasingly larger region where the flow remains nearly purely azimuthal. There is a fraction of the secondary flow generated at the end plates that is transported to the equator over a boundary layer at the inner cylinder. The formation of this boundary layer leads to the emergence of two large-scale circulation cells, which are progressively confined to the inner cylinder as is increased. These cells are similar to but significantly weaker than those in the WR configuration. Turbulent fluctuations are also progressively confined to the end plates as increases (see figure 6 ). Some fluctuations caused by the large-scale recirculation flow may also occur in the vicinity of the inner cylinder. However, given their low intensity, it can be stated that the flow remains nearly laminar when sufficiently far from the end plates.

As seen in figure 7 , the mean azimuthal velocity is only significantly affected by the secondary flows in the vicinity of the end plates. Hence, negligible differences were found when measuring radial profiles of the mean azimuthal velocity in the bulk at different axial locations (see figure 7 ). Despite large-scale secondary flows develop at the inner cylinder, unlike for the WR configuration, these are not sufficiently strong as to significantly modify the azimuthal velocity. As a result, the azimuthal velocity profiles in this configuration closely approximate the desired quasi-Keplerian Couette flow (1). It should be noted that Edlund & Ji (2014) reported velocity profiles with a small but noticiable deviations from (1) near the inner cylinder. Such deviations suggest that, while the turbulence at the inner cylinder does not affect the bulk flow in our simulations, its influence might not be entirely negligible in experiments at larger .

Figure 7: and show color maps and contours illustrating the mean azimuthal velocity in the WR and HTX configurations respectively, whereas radial profiles of computed at three different axial locations are shown in WR and HTX. In both cases the solution depicted corresponds to the maximum achieved in our simulations, in and , and in and . There are contours equally distributed across the full range of . The (black) shows the quasi-Keplerian velocity profile (1) that would be achieved The horizontal lines superimposed upon figure indicate the axial locations at which the azimuthal velocity profiles have been computed.

4.3 Dynamics of the Mri configuration

Avila (2012) performed direct numerical simulations of the MRI configuration of Ji et al. (2006) up to , for which turbulence was found to fill the entire domain. Here we extend the range of Reynolds numbers by a factor of two. First of all, we note that the rotation speeds of the end-plate rings used by Ji et al. (2006) are not optimal and result in large torque at the end plates. At low , the meridional circulation resembles that of the WR configuration (see figure 1 in Avila (2012)), with a strong radial jet located at the equatorial region. However, unlike the WR, the radial flow at the end plates is entirely inward, and so there is a single large-scale circulation cell in the upper and lower half of the experiment As in the WR configuration the large scale circulation cells and turbulent motions cluster here progressively near the inner cylinder (see figures 8 and ), leaving a nearly azimuthal and laminar flow in the remaining part of the gap.

Figures 8 and show the time-averaged azimuthal velocity and radial profiles of at respectively. Here is also nearly uniform in the axial direction, but differs from the theoretical Couette flow (1). Hence we conclude that although Ji et al. (2006) measured negligible Reynolds stresses in the bulk of their experiment, their flows were strongly turbulent in thin boundary layers at the cylinders. Interestingly, in the bulk the profiles are in fact quasi-Keplerian yet substantially shifted with respect to Couette flow because of the sharp drop at the cylinder boundary layers. Similar velocity profiles for this configuration were reported in the numerical simulations of  Obabko et al. (2008) and experiments of Schartman et al. (2012), who speculated that the deviation in the profiles near the inner cylinder might be caused by the existence of turbulent Stewartson boundary layers.

Figure 8: , and show meridional sections illustrating the mean radial, axial and azimuthal velocities in the MRI configuration for a solution computed at . contours equally distributed across , and have been added. Radial profiles of computed at the same axial locations as in figure 7.

5 Discussion and conclusions

We have performed direct numerical simulations of the flow in a Taylor-Couette device that Edlund & Ji (2014) specifically designed to infer the hydrodynamic stability of constant-density Keplerian flows. A first interesting observation is that the occurrence of turbulence at low appears to be a robust feature of quasi-Keplerian Taylor–Couette flows. Nevertheless, turbulence manifests itself differently depending on axial boundary conditions. In the WR configuration, as well as in the HTX and MRI configurations if the boundary conditions are not optimal, as in Ji et al. (2006), the end plates drive a large-scale EC which gives rise to strongly turbulent boundary layers at the cylinders. In contrast, when the HTX configuration is operated under optimal boundary conditions, the EC and associated turbulence is localised near the end plates.

As increases turbulence localises to thin boundary layers, whereas the flow in the bulk becomes nearly azimuthal and axially uniform. The progressive relaminarisation of the bulk flow observed in these configurations does not however imply that they are all adequate to infer the stability of astrophysical flows. As reported in Edlund & Ji (2015), the azimuthal velocity profiles achieved in the WR configuration differ substantially from a quasi-Keplerian profile, even in their optimal regime of operation, whereas laminar Couette profiles can be realized in the HTX configuration with optimal boundary conditions. Leclercq et al. (2016) showed that quasi-Keplerian profiles can also be achieved in experiments if stable stratification is added near the end plates. However, this method becomes impractical for the large Reynolds numbers investigated in the Princeton experiments.

It is remarkable that in spite of the nearly one order of magnitude gap in Reynolds numbers between our simulations and the experiments of Edlund & Ji (2015), the azimuthal velocity profiles are indistinguishable. This suggests that, despite the turbulent boundary layers, the velocity profiles exhibit self-similar behaviour, in agreement with the observations Edlund & Ji (2015). Taken together, these results show that isothermal constant density quasi-Keplerian Taylor–Couette flows are stable at least up to . Noteworthy, for and the energy of disturbances imposed to the laminar flow can be transiently amplified up to a factor of (see eq. (5.1) in Maretzke et al. 2014). Hence it seems that for quasi-Keplerian flows linear transient growth is a poor indicator of turbulence transition.

Our results highlight that experiments of astrophysical flows cannot only rely on measuring velocity fluctuations alone, because vanishing Reynolds stresses do not imply quasi-Keplerian velocity profiles. Similarly, torque measurements are inadequate because they cannot be used to infer the level of turbulence in the bulk, which may be laminar despite highly turbulent boundary layers.

We remark that the experiments simulated here were performed with a constant density fluid, whereas in accretion disks the gas is strongly stratified in the axial and radial directions. Hence the results shown here apply to barotropic gases only. For stratified quasi-Keplerian flows several instabilities have been reported. Examples are the strato-rotational instability (Molemaker et al. 2001; Le Bars & Le Gal 2007), the radiative instability (Le Dizès & Riedinger 2010; Riedinger et al. 2011), the zombie vortex instability (Marcus et al. 2015; Lesur & Latter 2016), the vertical shear instability (Urpin & Brandenburg 1998; Nelson et al. 2013) and the subcritical global instability (Klahr & Bodenheimer 2003; Johnson & Gammie 2006; Petersen et al. 2007). The ability to realize quasi-Keplerian velocity profiles in experiments at large Reynolds numbers opens up avenues for new experimental investigations of some of these instabilities and their underlying mechanisms. Candidates are the vertical shear instability or subcritical global instability, which could be addressed with experiments of radially stratified Taylor–Couette flows including thermal relaxation, or the zombie vortex instability, which could be studied in a Taylor–Couette setup subject to strong stable stratification in the vertical direction. Nevertheless, additional issues related to the interplay between end plates and stratification must be first addressed (Lopez et al. 2015).

We are grateful to red Española de Supercomputación (RES) and the Regionales Rechenzentrum Erlangen (RRZE) for the computational resources provided.

  • Avila (2012) Avila, M. 2012 Stability and angular-momentum transport of fluid flows between corotating cylinders. Phys. Rev. Lett. 108.
  • Avila et al. (2008) Avila, M., Grimes, M., Lopez, J. M. & Marques, F. 2008 Global endwall effects on centrifugally stable flows. Phys. Fluids 20, 104104.
  • Balbus (2003) Balbus, S. A. 2003 Enhanced angular momentum transport in accretion disks. Annual Review of Astronomy and Astrophysics 41 (1), 555–597.
  • Balbus & Hawley (1998) Balbus, S. A. & Hawley, J. F. 1998 Instability, turbulence, and enhanced transport in accretion disks. Rev. Mod. Phys. 70, 1–53.
  • Brauckmann & Eckhardt (2013) Brauckmann, H. J. & Eckhardt, B. 2013 Direct numerical simulations of local and global torque in taylor–couette flow up to re= 30 000. Journal of Fluid Mechanics 718, 398–427.
  • Dubrulle et al. (2005a) Dubrulle, B., Dauchot, O., Daviaud, F., Longaretti, P.-Y., Richard, D. & Zahn, J.-P. 2005a Stability and turbulent transport in taylor couette flow from analysis of experimental data. Physics of Fluids 17 (9).
  • Dubrulle et al. (2005b) Dubrulle, B., Marié, L., Normand, C., Richard, D., Hersant, F. & Zahn 2005b A hydrodynamic shear instability in stratified disks. Astronomy & Astrophysics 429, 1–13.
  • Edlund & Ji (2014) Edlund, E. M. & Ji, H. 2014 Nonlinear stability of laboratory quasi-keplerian flows. Phys. Rev. E 89, 021004.
  • Edlund & Ji (2015) Edlund, E. M. & Ji, H. 2015 Reynolds number scaling of the influence of boundary layers on the global behavior of laboratory quasi-keplerian flows. Phys. Rev. E 92, 043005.
  • Fricke (1968) Fricke, K. 1968 Instabilität stationärer Rotation in Sternen. Zeitschrift für Astrophysik 68, 317.
  • Goldreich & Schubert (1967) Goldreich, P. & Schubert, G. 1967 Differential Rotation in Stars. Astrophys. J. 150, 571.
  • Hollerbach & Fournier (2004) Hollerbach, R. & Fournier, A. 2004 End-effects in rapidly rotating cylindrical taylor-couette flow. In MHD Couette Flows: Experiments and Models, , vol. 733, pp. 114–121. AIP Conference Proceedings.
  • Hughes & Randriamampianina (1998) Hughes, S. & Randriamampianina, A. 1998 An improved projection scheme applied to pseudospectral methods for the incompressible Navier-Stokes equations. Intnl J. Num. Meth. Fluids 28, 501–521.
  • Ji & Balbus (2013) Ji, H. & Balbus, S. 2013 Angular momentum transport in astrophysics and in the lab. Physics Today 66 (8), 27–33.
  • Ji et al. (2006) Ji, H., Burin, M., Schartman, E. & Goodman, J. 2006 Hydrodynamic turbulence cannot transport angular momentum effectively in astrophysical disks. Nature 444 (7117), 343–346.
  • Johnson & Gammie (2006) Johnson, B. M. & Gammie, C. F. 2006 Nonlinear stability of thin, radially stratified disks. The Astrophysical Journal 636 (1), 63.
  • Kerswell (2015) Kerswell, R. 2015 Instability driven by boundary inflow across shear: a way to circumvent rayleigh’s stability criterion in accretion disks? Journal of Fluid Mechanics 784, 619–663.
  • Klahr & Bodenheimer (2003) Klahr, H. & Bodenheimer, P. 2003 Turbulence in accretion disks: Vorticity generation and angular momentum transport via the global baroclinic instability. The Astrophysical Journal 582 (2), 869.
  • Le Bars & Le Gal (2007) Le Bars, M. & Le Gal, P. 2007 Experimental analysis of the stratorotational instability in a cylindrical couette flow. Physical review letters 99 (6), 064502.
  • Le Dizès & Riedinger (2010) Le Dizès, S. & Riedinger, X. 2010 The strato-rotational instability of taylor–couette and keplerian flows. Journal of Fluid Mechanics 660, 147–161.
  • Leclercq et al. (2016) Leclercq, C., Partridge, J. L., Augier, P., Dalziel, S. B. & Kerswell, R. R. 2016 Using stratification to mitigate end effects in quasi-keplerian taylor–couette flow. Journal of Fluid Mechanics 791, 608–630.
  • Lesur & Latter (2016) Lesur, G. & Latter, H. 2016 On the survival of zombie vortices in protoplanetary discs. Monthly Notices of the Royal Astronomical Society 462, 4549–4554.
  • Lin & Papaloizou (1980) Lin, D. N. C. & Papaloizou, J. 1980 On the structure and evolution of the primordial solar nebula. Monthly Notices of the Royal Astronomical Society 191 (1), 37–48.
  • Lin & Pringle (1987) Lin, D. N. C. & Pringle, J. E. 1987 A viscosity prescription for a self-gravitating accretion disc. Monthly Notices of the Royal Astronomical Society 225 (3), 607–613.
  • Lopez & Marques (2015) Lopez, J. M. & Marques, F. 2015 Dynamics of axially localized states in taylor-couette flows. Phys. Rev. E 91, 053011.
  • Lopez et al. (2015) Lopez, J. M., Marques, F. & Avila, M. 2015 Conductive and convective heat transfer in fluid flows between differentially heated and rotating cylinders. International Journal of Heat and Mass Transfer 90, 959 – 967.
  • Lopez & Shen (1998) Lopez, J. M. & Shen, J. 1998 An efficient spectral-projection method for the Navier-Stokes equations in cylindrical geometries I. Axisymmetric cases. J. Comput. Phys. 139, 308–326.
  • Marcus et al. (2015) Marcus, P., Pei, S., Jiang, C., Barranco, J., Hassanzadeh, P. & Lecoanet, D. 2015 Zombie vortex instability. i. a purely hydrodynamic instability to resurrect the dead zones of protoplanetary disks. The Astrophysical Journal 808 (1), 87.
  • Maretzke et al. (2014) Maretzke, S., Hof, B. & Avila, M. 2014 Transient growth in linearly stable taylor-couette flows. J. Fluid Mech. 742, 254–290.
  • Mercader et al. (2010) Mercader, I., Batiste, O. & Alonso, A. 2010 An efficient spectral code for incompressible flows in cylindrical geometries. Computers & Fluids 39, 215–224.
  • Miesch et al. (2015) Miesch, M., Matthaeus, W., Brandenburg, A., Petrosyan, A., Pouquet, A., Cambon, C., Jenko, F., Uzdensky, D., Stone, J., Tobias, S., Toomre, J. & Velli, M. 2015 Large-eddy simulations of magnetohydrodynamic turbulence in heliophysics and astrophysics. Space Science Reviews 194 (1), 97–137.
  • Molemaker et al. (2001) Molemaker, M. J., McWilliams, J. C. & Yavneh, I. 2001 Instability and equilibration of centrifugally stable stratified taylor-couette flow. Physical review letters 86 (23), 5270.
  • Nelson et al. (2013) Nelson, R. P., Gressel, O. & Umurhan, O. M. 2013 Linear and non-linear evolution of the vertical shear instability in accretion discs. Monthly Notices of the Royal Astronomical Society p. stt1475.
  • Nordsiek et al. (2015) Nordsiek, F., Huisman, S. G., van der Veen, R. C. A., Sun, C., Lohse, D. & Lathrop, D. P. 2015 Azimuthal velocity profiles in rayleigh-stable taylor–couette flow and implied axial angular momentum transport. Journal of Fluid Mechanics 774, 342–362.
  • Obabko et al. (2008) Obabko, A., Cattaneo, F. & Fischer, P. 2008 The influence of horizontal boundaries on ekman circulation and angular momentum transport in a cylindrical annulus. Physica Scripta T132, 014029.
  • Paoletti et al. (2012) Paoletti, M., van Gils, D. P., Dubrulle, B., Sun, C., Lohse, D. & Lathrop, D. 2012 Angular momentum transport and turbulence in laboratory models of keplerian flows. Astronomy & Astrophysics 547, A64.
  • Paoletti & Lathrop (2011) Paoletti, M. S. & Lathrop, D. P. 2011 Angular momentum transport in turbulent flow between independently rotating cylinders. Physical review letters 106 (2), 024501.
  • Petersen et al. (2007) Petersen, M., Julien, K. & Stewart, G. 2007 Baroclinic vorticity production in protoplanetary disks. The Astrophysical Journal 658, 1236–1251.
  • Ravelet et al. (2010) Ravelet, F., Delfos, R. & Westerweel, J. 2010 Influence of global rotation and reynolds number on the large-scale features of a turbulent taylor–couette flow. Physics of Fluids 22 (5).
  • Rayleigh (1917) Rayleigh, L. 1917 On the dynamics of revolving fluids. Proc. Roy. Soc. Lond. A 93 (648), 148–154.
  • Richard & Zahn (1999) Richard, D. & Zahn, J.-P. 1999 Turbulence in differentially rotating flows. what can be learned from the couette-taylor experiment. Astronomy & Astrophysics 347, 734–738.
  • Riedinger et al. (2011) Riedinger, X., Le Dizès, S. & Meunier, P. 2011 Radiative instability of the flow around a rotating cylinder in a stratified fluid. Journal of Fluid Mechanics 672, 130–146.
  • Ryu & Goodman (1992) Ryu, D. & Goodman, J. 1992 Convective instability in differentially rotating disks. Astrophys. J. 388, 438–450.
  • Schartman et al. (2012) Schartman, E., Ji, H., Burin, M. J. & Goodman, J. 2012 Stability of quasi-keplerian shear flow in a laboratory experiment. Astronomy & Astrophysics 543, A94.
  • Shalybkov & Rüdiger (2005) Shalybkov, D. & Rüdiger, G. 2005 Stability of density-stratified viscous taylor-couette flows. AA 438 (2), 411–417.
  • Shi et al. (2015) Shi, L., Rampp, M., Hof, B. & Avila, M. 2015 A hybrid mpi-openmp parallel implementation for pseudospectral simulations with application to taylor–couette flow. Computers & Fluids 106, 1 – 11.
  • Toomre (1964) Toomre, A. 1964 On the gravitational stability of a disk of stars. The Astrophysical Journal 139, 1217–1238.
  • Turner et al. (2014) Turner, N. J., Fromang, S., Gammie, C., Klahr, H., Lesur, G., Wardle, M. & Bai, X. N. 2014 Transport and accretion in planet-forming disks. Arizona University press .
  • Urpin & Brandenburg (1998) Urpin, V. & Brandenburg, A. 1998 Magnetic and vertical shear instabilities in accretion discs. Monthly Notices of the Royal Astronomical Society 294, 399.
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description