Two types of axisymmetric helical magnetorotational instability in rotating flows with positive shear
Summary (3 min read)
Introduction
- This is a repository copy of Two types of axisymmetric helical magnetorotational instability in rotating flows with positive shear.
- Version: Accepted Version Article: Mamatsashvili, G, Stefani, F, Hollerbach, R et al. (1 more author) (2019) Two types of axisymmetric helical magnetorotational instability in rotating flows with positive shear.
- These conditions are indeed satisfied in the solar tachocline, where this new instability can possibly play an important role in its dynamics and magnetic activity.
II. MAIN EQUATIONS
- Consider a flow between two coaxial cylinders at inner, ri, and outer, ro, radii, rotating, respectively, with angular velocities Ωi and Ωo in the cylindrical coordinates (r, φ, z).
- The pressure associated with this base flow and maintaining its rotation is denoted as P0.
- The imposed background helical magnetic field B0 = (0, B0φ(r), B0z) consists of a radially varying, current-free azimuthal component, B0φ(r) = βB0zro/r, and a constant axial component, B0z , where the constant parameter β characterizes field’s helicity.
- There is instability in the flow, if the real part of any eigenvalue, or growth rate is positive, Re(γ) > 0, for any of the eigennmodes.
III. WKB ANALYSIS
- The authors use a radially local WKB approximation, where the radial dependence of the perturbations is assumed to be of the form ∝ exp(ikrr) with kr being the radial wavenumber.
- Figure 1(a) shows the growth rate, Re(γ), as a function of the re-scaled axial wavenumber, as determined from a numerical solution of Eq. (4) at finite but very small Pm = 10−6, together with solution (5) in the inductionless limit, for fixed Ha∗ and Re∗.
- Energy is drawn from the background flow rΩ(r) to the growing perturbations due to the coupling between meridional circulation and azimuthal field perturbations brought about by the imposed azimuthal field, a mechanism also underlying HMRI at negative shear [6, 29].
- To explore the behavior of type 2 Super-HMRI further, the authors first vary α as well as the re-scaled Hartmann and Reynolds numbers.
- Note that while the authors have only presented the Ro = 1.5 case in order to demonstrate the behavior of the instability with Pm, other values of Rossby number yield qualitatively similar behavior and scalings of γm, Ha ∗ m, Re ∗ m.
IV. GLOBAL ANALYSIS
- After the radially local WKB analysis, the authors now investigate type 2 Super-HMRI in the global case.
- Hence, the main equations are the same as those in that paper and are obtained by linearizing Eqs. (1)-(3) about the above equilibrium, with the only difference being that now the imposed rotation profile Ω(r) increases with radius corresponding to outer cylinder rotating faster than the inner one (super-rotation).
- The boundary conditions are no-slip for the velocity and either perfectly conducting or insulating for the magnetic field.
- The global 1D analysis serves two main purposes.
- First, to compare with the results of the above WKB analysis in the regime where the latter holds, i.e., at high β ≫ 10 and a small gap width between the cylinders, δ ≡ ro − ri ≪ ro, when the equilibrium quantities do not change much with radius across the gap.
A. Narrow-gap case
- One of the main difficulties when comparing local and global analysis of HMRI and AMRI in a magnetic TC flow is that the local Rossby number, which defines these instabilities and to which they are therefore sensitive [19, 23, 24], varies with radius, even in the narrow gap case.
- This implies that actually the WKB regime is better fulfilled at large Pm and those higher kz , at which the instability reaches a maximum growth, and hence specific boundary conditions do not affect its growth and frequency.
- This indicates that type 2 Super-HMRI, like HMRI at negative , is a genuine instability intrinsic to the flow, tapping free energy of differential rotation , and is not induced/driven by the radial boundaries on the confining rotating cylinders, although it can still be modified by these boundaries.
B. Wide-gap case
- Having explored type 2 Super-HMRI in the local and narrow-gap global cases, the authors now look for it in the case of a wide gap.
- As seen in Fig. 4, qualitatively the expected scalings with β are still followed, with Ha and Re (or S and Rm) as well as kzm increasing with β.
- By contrast, the local WKB analysis better applies in the narrow gap case, η̂ → 1, because the eigenfunctions vary mostly only over the gap width (Figs. 8-10), which is much less than ro and hence the radial variation of the equilibrium quantities are small across this distance.
- A more comprehensive global linear analysis of this instability, exploring the dependence of its growth rate on the flow parameters (η̂, β, Re,Ha, Pm), will be presented elsewhere.
V. SUMMARY AND DISCUSSION
- The authors have uncovered and analyzed a novel type of double-diffusive axisymmetric HMRI, labelled type 2 Super-HMRI, which exists in rotational flows with radially increasing angular velocity, or positive shear of arbitrary steepness threaded by a helical magnetic field – a configuration where magnetorotational instabilities were previously unknown.
- This will also allow us to make comparison with theoretical results.
A. Applicability to the solar tachocline
- MRI has already been discussed in relation to the solar tachocline in several studies [17, 36–39], showing that it can arise at middle and high latitudes, where the shear of the differential rotation is negative.
- This new double-diffusive type 2 Super-HMRI, on the other hand, may arise and potentially have important implications for the dynamics and magnetic activity of the low latitude, near-equatorial region of the solar tachocline, since necessary conditions for the development of this instability can be realized there.
- It seen from this figure that the largest growth rate is ∼ 10−3, or in dimensional variables ∼ 10−3Ωo, and therefore the corresponding growth time is ∼ 103Ω−1o .
Acknowledgments
- This project has received funding from the European Union’s Horizon 2020 research and innovation pro- gramme under the Marie Sk lodowska – Curie Grant Agreement No. 795158 and the ERC Advanced Grant Agreement No. 787544 as well as from the Shota Rustaveli National Science Foundation of Georgia (SRNSFG, grant No. FR17-107).
- GM acknowledges support from the Alexander von Humboldt Foundation .
- The authors thank both anonymous referees for constructive criticism which has led to an extended version of this paper and much improved the presentation of their main results. [1].
- Actually the selected value of kr0 when comparing local WKB and global dispersion curves is still somewhat arbitrary, since it is not generally possible to get an exact matching between the characteristic radial length of the global eigenfunctions and radial wavenumber of WKB solutions/harmonics.
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Frequently Asked Questions (17)
Q2. What are the future works in this paper?
This promising result of the global stability analysis can, in turn, be a basis for future efforts aiming at the detection of this instability and thereby providing an experimental evidence for its existence. Building on the findings of this first study, future work will explore in greater detail the parameter space and the effect of boundary conditions on type 2 Super-HMRI, which are more relevant to those present in TC flow experiments.
Q3. What is the mechanism underlying the imposed azimuthal field?
Energy is drawn from the background flow rΩ(r) to the growing perturbations due to the coupling between meridional circulation and azimuthal field perturbations brought about by the imposed azimuthal field, a mechanism also underlying HMRI at negative shear [6, 29].
Q4. What is the imposed background helical magnetic field?
The imposed background helical magnetic field B0 = (0, B0φ(r), B0z) consists of a radially varying, current-free azimuthal component, B0φ(r) = βB0zro/r, and a constant axial component, B0z , where the constant parameter β characterizes field’s helicity.
Q5. What is the basic condition for the local WKB approximation to hold?
A basic condition for the local WKB approximation to hold is that the radial wavelength, λr, of the perturbations must be much smaller than the characteristic radial size, ro, of the system over which the equilibrium quantities vary, i.e., λr ≪ ro.
Q6. What is the criterion for the flow stability of a magnetic field?
Since the authors focus on positive Rossby numbers, Ro > 0, or positive shear, the flow is generally stable both hydrodynamically, according to Rayleigh’s criterion (but see Ref. [13]), as well as against SMRI with a purely axial field (β = 0) [24–26].
Q7. How does the growth rate of a radial wavenumber change with the boundary conditions?
depending on Ha and Re, conducting boundaries can lead either to increase or decrease of the growth rate compared to its WKB value, whereas insulating boundaries alwaysreduce the growth rate about three times compared to those for the conducting ones for fixed Hartmann and Reynolds numbers.
Q8. What is the flow stability of a positive shear cylinder?
Since the authors are primarily interested in the flow stability in the case of positive shear, or so-called “super-rotation” [15, 16], the inner cylinder is assumed to rotate slower than the outer one, Ωi < Ωo, inducing an azimuthal nonuniform flow U0 = (0, rΩ(r), 0) between the cylinders with radially increasing angular velocity, dΩ/dr > 0, and hence positive Rossby number, Ro > 0.
Q9. What is the radial dependence of the perturbations?
In this section, the authors use a radially local WKB approximation, where the radial dependence of the perturbations is assumed to be of the form ∝ exp(ikrr) with kr being the radial wavenumber.
Q10. What is the reason for the differences in the growth rates between the local and global wide gap cases?
Another reason for the differences in the growth rates between the local and the global wide gap cases is that a finite distance between the cylinders also excludes (cuts off) very small radial wavenumbers (α → 1), which correspond to larger growth rates at β ∼ 1 in the WKB analysis (see Fig. 1(b)).
Q11. What is the primary goal of the calculations?
As noted above, in this subsection, the primary goal of these calculations is to identify this new instability in a TC flow setup commonly employed in lab experiments, which in the present case has a radially increasing angular velocity (positive shear) profile.
Q12. How does the dependence on parameter in Eq. (4) work?
Regarding the dependence on β parameter in Eq. (4), it is readily seen that, as long as β 6= 0, it enters the coefficients of these dispersion relations through the re-scaled wavenumbers, Hartmann, Lundquist and Reynolds numbers, k∗z ≡ kz/β, k∗ ≡ k/β, Ha∗ ≡ Ha/β, S∗ ≡ S/β, Re∗ ≡ Re/β2, Rm∗ ≡ Rm/β2, in terms of which the authors carry out the following WKB analysis.
Q13. What is the type of instability that is found in Eq. (4)?
type 2 Super-HMRI represents a new, dissipation-induced instability mode at positive shear, which appears to require the presence of both finite viscosity and resistivity.
Q14. What is the inverse of the inductionless limit?
This latter branch is basically an extension of the more familiar HMRI operating at negative shear, which in the inductionless limit also satisfies Eq. (5), but at Ro < RoLLL, where RoLLL = 2(1 − √2) ≈ −0.83 is the lower Liu limit [19, 24, 27].
Q15. What is the axial current required to achieve large in the wide gap?
The authors take β ∼ 1 in these calculations for the wide-gap, since it is rather costly to achieve large β in experiments due to very high axial currents required.
Q16. What is the maximum growth rate for a given Pm?
In particular, the maximum growth rate, γm, occurs for (Ha ∗ m, Re ∗m) ≈ (700, 9 · 104) when Pm is small (Fig. 1(c)), but for orders of magnitude smaller (Ha∗m, Re ∗m) = (2.54, 0.23) when Pm is large (Fig. 2(c))
Q17. What is the main reason why the WKB approach is questionable?
the authors will see in the global linear analysis below that this mode of instability is in fact not restricted only to large β and can even exist at smaller β ∼ 1, but in this case the WKB approach is questionable and should be applied with caution.