Anisotropic hydrodynamic turbulence in accretion disks
^{1} Institut für Astronomie und Astrophysik, Universität Tübingen, Auf der Morgenstelle 10, 72076 Tübingen, Germany
email: moritz.stoll@unituebingen.de; wilhelm.kley@unituebingen.de
^{2} UniversitätsSternwarte, LudwigMaximiliansUniversität München, Scheinerstr. 1, 81679 München, Germany
email: picogna@usm.lmu.de
Received: 9 December 2016
Accepted: 1 February 2017
Recently, the vertical shear instability (VSI) has become an attractive purely hydrodynamic candidate for the anomalous angular momentum transport required for weakly ionized accretion disks. In direct threedimensional numerical simulations of VSI turbulence in disks, a meridional circulation pattern was observed that is opposite to the usual viscous flow behavior. Here, we investigate whether this feature can possibly be explained by an anisotropy of the VSI turbulence. Using threedimensional hydrodynamical simulations, we calculate the turbulent Reynolds stresses relevant for angular momentum transport for a representative section of a disk. We find that the vertical stress is significantly stronger than the radial stress. Using our results in viscous disk simulations with different viscosity coefficients for the radial and vertical direction, we find good agreement with the VSI turbulence for the stresses and meridional flow; this provides additional evidence for the anisotropy. The results are important with respect to the transport of small embedded particles in disks.
Key words: accretion, accretion disks / turbulence
© ESO, 2017
1. Introduction
The exact origin of the driving mechanism of accretion disks is still not fully understood. To accrete matter onto the central object, the matter needs to lose its angular momentum, and because molecular viscosity is by many orders of magnitudes too small to facilitate the required angular transport, it has been suggested that disks are driven by turbulence. The discovery of a linear magnetorotational instability (MRI) for rotating flows with a negative angular velocity gradient has led to the suggestion that accretion disks are driven by magnetohydrodynamical (MHD) turbulence (Balbus & Hawley 1998). However, the MRI only works efficiently for wellionized media, for example, in disks around compact objects, but for lower ionization levels the nonideal MHD effects become stronger and the operability of the MRI questionable. In particular for the cool and lowionized regions, socalled dead zones with very low turbulent activity have been predicted (Gammie 1996).
Hence, other alternatives are sought for. In the past years the purely hydrodynamical vertical shear instability (VSI) has attracted some attention because the only requirement is a vertical shear in the angular velocity profile, which is in fact a natural consequence of a radial temperature gradient in the disk, for example, induced by irradiation from the central object. Through numerical simulations and linear analysis it has been shown that the VSI operates efficiently for vertically isothermal disks (Nelson et al. 2013) as well as for fully radiative disks that include stellar irradiation (Stoll & Kley 2014). This makes the VSI a promising candidate to bring at least some life back into the dead zones. For many astrophysical applications it is useful to parameterize the turbulence and describe the angular momentum transport by an effective viscous prescription, for example, the wellknown ansatz by Shakura & Sunyaev (1973) where the uncertainties of the turbulence are summarized in one constant parameter α (Balbus & Papaloizou 1999). Such an approach using one parameter is applicable for an isotropic turbulence, and useful when the interest is in the overall radial evolution of the disk. To analyze the internal flow field of the disk, which is important for the motion of embedded small particles, it is necessary to take possible nonisotropy effects into account.
Here, we demonstrate that the flow reversal found in recent VSIturbulent disks (Stoll & Kley 2016) can in fact be traced back to the intrinsic anisotropy of the VSIturbulence. Using multidimensional hydrodynamical simulations, we calculate the effective radial and vertical transport coefficients and use them in viscous disk simulations.
2. Model setup
We use the pluto code (Mignone et al. 2007) for our simulations, where we model a section of a locally isothermal accretion disk. For the direct turbulent simulations we use a full 3D setup and spherical coordinates (R, θ, φ), while for comparison laminar viscous simulations (αdisk), we use a 2D axisymmetric setup and cylindrical coordinates (r,z). The model parameters are given in Table 1.
Model parameter: domain size and grid resolution.
Even though some of the simulations are performed in spherical coordinates, the results are analyzed in cylindrical coordinates. The initial disk is axisymmetric and extends from 0.4 r_{0} to 2.5 r_{0}, where r_{0} = 5.2 au. The initial density profile is given by vertical hydrostatic equilibrium (1)where ρ_{0} is the gas midplane density at r = r_{0}, and p = −1.5. In our locally isothermal approximation the temperature of the disk is a function of the cylindrical radius only, (2)where we choose q = −1, which causes the disk aspect ratio to be constant and T_{0} such that H/r = h = 0.05. The pressure is given by , where c_{s} is the isothermal sound speed with c_{s} ∝ r^{− 1/2}. The gas moves initially with the angular velocity given by the Keplerian value, corrected by the pressure support (Nelson et al. 2013) (3)with , and the meridional flow (u_{r},u_{z}) is set to zero. At the inner and outer boundary we use reflecting boundaries. To increase numerical stability for the turbulent runs, we damp the variables ρ,u_{r},u_{z} to the initial values on a timescale of half a local orbit following the recipe by de ValBorro et al. (2006), with a damping applied at the inner boundary from 0.4−0.5 r_{0} and at the outer boundary from 2.3−2.5 r_{0}. At the vertical boundaries we use reflective boundaries when the flow is directed inward and zero gradient otherwise. The VSI model is inviscid, and for the αdisk model the kinematic viscosity is given by ν = 2/3αc_{s}H, with a constant α = 5 × 10^{4}, which matches the outcome of VSI model.
3. Disk structure
We compare the structure of the VSI unstable disk to viscous disks described by an αparameter, and study the main differences. The VSI disk is evolved to a quasiequilibrium state before the analysis is performed. We focus in particular on the flow field and stress tensor, and refer to Nelson et al. (2013) and Stoll & Kley (2014, 2016) for an analysis of the turbulent flow structure.
While the density distributions of the viscous and turbulent disks in equilibrium are very similar due to the necessary pressure equilibrium, there is an important difference in the meridional flow within the disk in particular for the radial velocity. We show the azimuthally averaged radial velocity u_{r} at r = r_{0} as a function of the vertical distance for the turbulent and the standard viscous disk in Fig. 1. For the turbulent disk we averaged the velocity in time over 50 orbits and in space around r_{0} in the region (0.8−1.25)r_{0}. For better visibility we rescaled the viscous case by a factor of 200. Obviously, the two radial velocity profiles have an opposite behavior. The standard viscous disk using a single (isotropic) value of α shows the typical outflow in the midplane that has been predicted analytically by Urpin (1984) and was later shown in fully timedependent numerical simulations (Kley & Lin 1992). This behavior of u_{r}(z) can be derived from the equilibrium angular momentum equation that contains the vertical disk structure (Urpin 1984). In spite of the outwardly directed flow in the midplane, the total vertically integrated mass flow is nevertheless directed inward in case of accreting disks (Kley & Lin 1992).
In contrast, the mean flow field for the turbulent flow (labeled 3D VSI and shown also with a dotted line for a model with double resolution in all directions) is fully reversed; it is not only negative in the midplane and positive in the corona, but also much stronger, as indicated by the different scaling of the curves in Fig. 1. This special feature of the meridional flow field in the VSI case has been found for isothermal as well as radiative disks in Stoll & Kley (2016), but was not analyzed with respect to anisotropic turbulence. From the direct comparison to the viscous case, it is clear that with a standard shear viscosity prescription using a constant αvalue or a constant kinematic viscosity, no agreement can be obtained because this will always lead to an inverted parabolic type of profile (Jacquet 2013). This raises the general question whether the VSI turbulence in disks can be described by a standard NavierStokes approach to model the angular momentum diffusion. In Sect. 4 we show that we obtain a good match of a fully turbulent and viscous flow for a nonanisotropic turbulent viscosity where the radial and vertical parts enter with a different strength (see curve 2D anisotropic stress), which might be expected for the clearly nonisotropic character of the flow structure in VSI turbulence (Stoll & Kley 2014).
Fig. 1
Radial velocity averaged over 50 orbits. We compare the disk with alphaviscosity (α = 5 × 10^{4}, blue curve) to a disk with active VSI (red curve), a disk with active VSI and doubled resolution (red dotted curve) and a viscous disk with anisotropic stress similar to the VSI disk (green curve, details see Sect. 4). For the turbulent disk the velocity has been azimuthally averaged. The profile shown is in units of sound speed c_{s0} and at r = r_{0}. The viscous case has been rescaled to better visualize the difference. 

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To analyze the effect of the turbulence with respect to angular momentum transport in the disk, it is necessary to calculate the turbulent stresses of the VSI disk. For the overall mass flow in accretion disks, which is driven by outward angular momentum transport, the rφcomponent of the Reynolds stress tensor, R, is the most important component because it is generated by the strong shear in the azimuthal velocity. In the case of VSI turbulent disks, it is clear that the vertical dependence of the turbulent stresses (zφcomponent) may be of importance as well. Hence, from our simulations we calculate the following turbulent Reynolds stresses (4)where u_{i} with i in (r,z) denote the radial and vertical flow velocity (u_{r},u_{z}) and δu_{φ} is the deviation of the azimuthal velocity, u_{φ} = rΩ, from unperturbed equilibrium, as given by Eq. (3). For the later analysis it is beneficial that the stresses are calculated in cylindrical coordinates (r,z), see Sect. 4. Since we are interested in particular in the vertical dependence of the stresses, R_{i,φ} is calculated by averaging over the full azimuth (2π), over a small radial range around a reference radius, and over time. Here, we timeaverage from orbit 80 to orbit 200 using a series of over 60 snap shots and spaceaverage in radius from 0.75−1.35 r_{0}.
The results of this averaging procedure are shown in Fig. 2. The solid curves refer to the specific stresses R_{i,φ}(z) /ρ(r_{0},z) (i = r,z) in units of , where ρ(r_{0},z) is the equilibrium density distribution, given by Eq. (1), and c_{s0} is the sound speed, both at the reference radius r_{0}.
Fig. 2
Specific stress tensor (stress per density) in units of . The solid lines represent the Reynolds stress (R) of the VSI simulation and the dotted lines refer to the viscous stress tensor (S) using α = 5 × 10^{4}. The S_{zφ} line was rescaled by a factor of 650 to match to the VSI model. The dotted line in the upper panel has a constant value of 5 × 10^{4}. 

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We compare it to the viscous shear stress prescription (see Eq. (6) with ν = ν_{r} = ν_{z}) using α = 5 × 10^{4} (dotted lines), which is close to the average of the rφcomponent of the specific VSI stress, 4 × 10^{4}. We rescaled the zφcomponent of the viscous shear stress by a factor of 650 to match the value from the VSI stress. From this large rescaling factor it is immediately clear that R_{zφ} is far larger than expected from an isotropic viscous shear prescription. We note that the deviation of the vertical R_{rφ}/ρprofile from the constant S_{rφ}/ρprofile is not important for our argument, which is why for simplicity we chose a constant α. For the angular momentum transport only the vertical average of this stress component plays a role. In our case, the very large zφcomponent of the stress dominates the meridional flow and the influence of R_{rφ} is small.
4. Anisotropic viscosity of the VSI turbulence
From our numerical studies of the VSI turbulence, in particular the vertical component of the Reynolds stress tensor, we can infer that the turbulence is nonisotropic. Even though we have integrated the hydrodynamical equations using spherical coordinates, we calculated and display R_{iφ} in cylindrical coordinates because this is simpler to analyze, as we explain in the following. In our approach we investigate whether the turbulent Reynolds stresses, R, can be modeled by a viscous ansatz where R is replaced by the standard viscous stress tensor, S, with an effective turbulent eddy viscosity as introduced by Boussinesq. In cylindrical coordinates the change in angular momentum is given by the following evolution equation: (5)For an axisymmetric flow, that is, when ∂/∂φ vanishes, the vector S_{φ} (the φrow of the viscous stress tensor) is given by (Tassoul 1978) (6)Axisymmetry is expected for accretion disk flows, and we found this in our simulations. In Eq. (6) we allowed for the option of an anisotropic viscosity by splitting the kinematic viscosity into two components ν_{r} and ν_{z}, where ν_{r} refers to the radial part, which typically is the main contribution in accretion disks in driving the angular momentum transport and mass accretion. The ν_{z} part connects to the vertical variation of the angular velocity Ω and has commonly been assumed to be on the same order as ν_{r}. Indeed, using ν_{z} = ν_{r} and performing viscous axisymmetric, twodimensional simulations, we find the typical meridional flow field in disks with outflow in the midplane and inflow in upper layers of the disk, as shown in Fig. 1 by the curve labeled “isotropic stress”, as found in classic studies (Urpin 1984; Kley & Lin 1992). The outflow in the midplane can easily be derived by an analysis of the radial flow that can be obtained from the angular momentum equation (see also Fromang et al. 2011; Jacquet 2013). From Eq. (5) we find for the equilibrium state that (7)Expanding Eq. (3) around the midplane (small z), we find (8)where q and p are the exponents in the radial power laws of the density and temperature, respectively, and h = H/r denotes the relative scale height of the disk. Using this relation for Ω(r,z), we find (9)and then, neglecting terms of order z^{2}/r^{2}(10)Combining this with the S_{zφ} relation, we find (11)This is plotted in the lower panel in Fig. 2 using ν_{z} = 650ν_{r}, which demonstrates that the linear dependence of the specific S_{zφ}stress is a direct consequence of Eq. (11). From Eq. (7) we find for the relation determining the sign of u_{r} in the midplane the following relation: (12)where for the last step we assumed that the viscosity has an αtype behavior with and ρ ∝ r^{p} and . We note that the direction of flow in the disk midplane can be influenced by the slopes (p,q) in the disk stratification (Fromang et al. 2011; Philippov & Rafikov 2017). From the above relation we find directly that for our disk with slopes q = −1 and p = −3/2 that (13)For isotropic turbulence with α_{r} = α_{z} we therefore have outflow in the disk midplane. For the turning point we find that α_{z} must be larger than 1.5α_{r}. Upon increasing α_{z} over α_{r}, the midplane radial velocity becomes more and more negative, and the entire vertical flow profile eventually reverses. In our numerical simulations of viscous disks using different values for ν_{z} we could indeed find the observed flow reversal for moderate values of ν_{z}/ν_{r}. By increasing ν_{z} further, we found that the VSI turbulence can be modeled by an anisotropic eddy viscosity with ν_{z} over two magnitudes larger than ν_{r} (650 for our chosen parameter, as shown in Fig. 2).
In performing the comparison simulations, we initially tried to use the same spherical coordinate system that we used for the turbulent VSI simulations by just increasing ν_{θ} over ν_{R} in the corresponding components of the stress tensor in spherical coordinates. However, this did not lead to the expected results, in particular, the inversion of the parabola of u_{r}(z). The results displayed in Fig. 1 were therefore obtained using a cylindrical coordinate system. Because the usage of a spherical coordinate system is beneficial in disk simulations, the equations need to be transformed from r,z to R,θ.
This means we need to transform the viscous part, ∇·(rS_{φ}), to spherical coordinates. The transformation equations are (14)and the components of the stress tensor transform according to The derivatives of Ω transform then as Using Eq. (6) in Eqs. (15) and (16) and substituting this into Eqs. (17) and (18), we obtain for the stress tensor components in spherical coordinates As can be inferred from these equations, the relatively simple anisotropic relation in cylindrical coordinates leads to complex coupled equations in spherical coordinates with cross terms in the derivatives for Ω. For the isotropic case we can set ν_{r} = ν_{z} = ν and obtain the standard relations for the stress tensor components in Rθcoordinates (Tassoul 1978). Now it becomes clear why merely increasing the θ part of the viscosity in Rθcoordinates did not yield the correct answer when compared to the VSI case. Using the full viscosity terms as described in Eqs. (19) and (20) in the numerical simulations yields the correct behavior. However, this comes with a serious drawback because in this case the numerical integration required much smaller time steps for numerical stability than the cylindrical simulation with the same viscosity coefficients. Performing multidimensional simulations of viscous disks mimicking the nonisotropic behavior of the VSI turbulence in Rθcoordinates therefore requires a considerable numerical effort. One solution
to this problem may be the usage of an implicit solver for the viscous terms.
5. Conclusions
From direct threedimensional simulations of locally isothermal accretion disks we observed that the eddies introduced by the VSI generate stresses that are strongly anisotropic. Specifically, we found that the vertical zφcomponent of the Reynolds stress is enhanced by a factor of 650 over the standard rφpart. By performing viscous disk simulations using a nonisotropic viscosity with α_{z} highly enlarged over α_{r}, we could obtain the same flow reversal as seen in the VSI disk, which verifies the nonisotropy of the viscosity. Hence, the reversal of the radial flow profile compared to the usual αmodel is a clear consequence of the anisotropy. This will have an effect on the dust migration processes (Stoll & Kley 2016) that need to be contrasted to the outward drift in the midplane viscous models (Takeuchi & Lin 2002). From this we can conclude that we need to be careful with turbulence models imposed on accretions disks when we adopt viscous models to describe them.
The meridional circulation of MRIturbulent disks has been analyzed by Fromang et al. (2011), who found a similar mean flow dynamics in the disk but did not attribute it to a nonisotropic turbulence (with large S_{zφ}) but rather to a radial variation in the magnitude of the viscosity. However, their turbulent R_{zφ} profile (in Fig. 5) indicates that it may be enhanced over the standard viscous value as well, which could also be a reason for the flow reversal.
Even though the analysis is performed for simplicity for a locally isothermal disk, our results are quite general as simulations for fully radiative disks show the same behavior although they have different radial and vertical temperature profiles. For this purpose, we reanalyzed our radiative simulations in Stoll & Kley (2016) and found a similar anisotropy. Concerning numerical resolution, simulations with double resolution show the same results as shown in Fig. 1. Nevertheless, further exploration needs to be done in order to check how the anisotropy factor varies for different disk parameters and to explore the possibility of anisotropic stresses in MRI models.
Acknowledgments
Moritz Stoll received financial support from the Landesgraduiertenförderung of the state of BadenWürttemberg and through the German Research Foundation (DFG) grant KL 650/16. G. Picogna acknowledges the support through DFGgrant KL 650/21 within the collaborative research program “The first 10 Million Years of the Solar System”. Some simulations were performed on the bwGRiD cluster in Tübingen, funded by the state of BadenWürttemberg and the DFG. We thank Roman Rafikov for providing us with a preprint and very useful discussions.
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All Tables
All Figures
Fig. 1
Radial velocity averaged over 50 orbits. We compare the disk with alphaviscosity (α = 5 × 10^{4}, blue curve) to a disk with active VSI (red curve), a disk with active VSI and doubled resolution (red dotted curve) and a viscous disk with anisotropic stress similar to the VSI disk (green curve, details see Sect. 4). For the turbulent disk the velocity has been azimuthally averaged. The profile shown is in units of sound speed c_{s0} and at r = r_{0}. The viscous case has been rescaled to better visualize the difference. 

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In the text 
Fig. 2
Specific stress tensor (stress per density) in units of . The solid lines represent the Reynolds stress (R) of the VSI simulation and the dotted lines refer to the viscous stress tensor (S) using α = 5 × 10^{4}. The S_{zφ} line was rescaled by a factor of 650 to match to the VSI model. The dotted line in the upper panel has a constant value of 5 × 10^{4}. 

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In the text 