2.1 Basic equations and closure models

Our equations are obtained as follows. A small patch of an accretion disc, co-orbiting with a fiducial point $R_{0}$ in the mid-plane of the unperturbed disc at an angular velocity $\unicode[STIX]{x1D734}=\unicode[STIX]{x1D6FA}\hat{\boldsymbol{z}}$ , is represented in Cartesian coordinates with the $x$ and $y$ directions corresponding to the radial and azimuthal directions, respectively. Differential rotation is accounted for by including the Coriolis force and by imposing a background linear shear flow, $\boldsymbol{U}_{0}=-Sx\hat{\boldsymbol{y}}$ , where $S\equiv -\text{d}\unicode[STIX]{x1D6FA}/\text{d}\ln R_{0}>0$ is the shear frequency; Keplerian rotation yields $S=(3/2)\unicode[STIX]{x1D6FA}$ . The evolutionary equations for the first three moments of the plasma distribution function are then (Chew, Goldberger & Low Reference Chew, Goldberger and Low1956; Kulsrud Reference Kulsrud, Rosenbluth and Sagdeev1983; Schekochihin et al. Reference Schekochihin, Cowley, Rincon and Rosin2010),

(2.1) $$\begin{eqnarray}\displaystyle & \displaystyle \frac{\text{d}\unicode[STIX]{x1D70C}}{\text{d}t}=-\unicode[STIX]{x1D70C}\unicode[STIX]{x1D735}\boldsymbol{\cdot }\boldsymbol{u}, & \displaystyle\end{eqnarray}$$

(2.2) $$\begin{eqnarray}\displaystyle & \displaystyle \unicode[STIX]{x1D70C}\left(\frac{\text{d}\boldsymbol{u}}{\text{d}t}+2\unicode[STIX]{x1D6FA}\hat{\boldsymbol{z}}\times \boldsymbol{u}-2S\unicode[STIX]{x1D6FA}x\hat{\boldsymbol{x}}\right)=-\unicode[STIX]{x1D735}\left(p_{\bot }+\frac{B^{2}}{8\unicode[STIX]{x03C0}}\right)+\unicode[STIX]{x1D735}\boldsymbol{\cdot }\left[\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\left(\frac{B^{2}}{4\unicode[STIX]{x03C0}}+\unicode[STIX]{x0394}p\right)\right], & \displaystyle\end{eqnarray}$$

(2.3) $$\begin{eqnarray}\displaystyle & \displaystyle \frac{\text{d}\boldsymbol{B}}{\text{d}t}=\boldsymbol{B}\boldsymbol{\cdot }\unicode[STIX]{x1D735}\boldsymbol{u}-\boldsymbol{B}\unicode[STIX]{x1D735}\boldsymbol{\cdot }\boldsymbol{u}, & \displaystyle\end{eqnarray}$$

(2.4) $$\begin{eqnarray}\displaystyle & \displaystyle \frac{\text{d}p_{\bot }}{\text{d}t}=-\unicode[STIX]{x1D735}\boldsymbol{\cdot }(q_{\bot }\hat{\boldsymbol{b}})-q_{\bot }\unicode[STIX]{x1D735}\boldsymbol{\cdot }\hat{\boldsymbol{b}}+p_{\bot }\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}-2p_{\bot }\unicode[STIX]{x1D735}\boldsymbol{\cdot }\boldsymbol{u}-\unicode[STIX]{x1D708}_{c}\unicode[STIX]{x0394}p, & \displaystyle\end{eqnarray}$$

(2.5) $$\begin{eqnarray}\displaystyle & \displaystyle \frac{\text{d}p_{\Vert }}{\text{d}t}=-\unicode[STIX]{x1D735}\boldsymbol{\cdot }(q_{\Vert }\hat{\boldsymbol{b}})+2q_{\bot }\unicode[STIX]{x1D735}\boldsymbol{\cdot }\hat{\boldsymbol{b}}-2p_{\Vert }\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}-p_{\Vert }\unicode[STIX]{x1D735}\boldsymbol{\cdot }\boldsymbol{u}+2\unicode[STIX]{x1D708}_{c}\unicode[STIX]{x0394}p, & \displaystyle\end{eqnarray}$$

where $\text{d}/\text{d}t\equiv \unicode[STIX]{x2202}/\unicode[STIX]{x2202}t+\boldsymbol{u}\boldsymbol{\cdot }\unicode[STIX]{x1D735}$ is the convective derivative. The velocity $\boldsymbol{u}$ in (2.1)–(2.5) includes both the background shear flow $\boldsymbol{U}_{0}$ and perturbations on top of this $\unicode[STIX]{x1D6FF}\boldsymbol{u}$ (e.g. the MRI). The other symbols have their usual meanings: $\unicode[STIX]{x1D70C}$ is the mass density, $\boldsymbol{B}$ is the magnetic field, $\unicode[STIX]{x1D708}_{c}$ is the particle collision frequency, while $B\equiv |\boldsymbol{B}|$ and $\hat{\boldsymbol{b}}\equiv \boldsymbol{B}/B$ denote the magnetic-field strength and direction (note that $\unicode[STIX]{x1D735}\boldsymbol{\cdot }(\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}B^{2})$ is simply $\boldsymbol{B}\boldsymbol{\cdot }\unicode[STIX]{x1D735}\boldsymbol{B}$ ). The pressures perpendicular and parallel to $\hat{\boldsymbol{b}}$ are $p_{\bot }$ and $p_{\Vert }$ respectively, while $q_{\bot }$ and $q_{\Vert }$ denote the fluxes of perpendicular and parallel heat in the direction parallel to $\hat{\boldsymbol{b}}$ . Note that $p_{\bot }$ and $p_{\Vert }$ in (2.2) should in principle be summed over both particle species (with separate pressures for each species), while $\unicode[STIX]{x1D70C}$ and $\boldsymbol{u}$ in (2.1)–(2.3) are the ion density and flow velocity. For simplicity, in this work we solve only the ion pressure equations (i.e. $p_{\bot }=p_{\bot ,i}$ , $p_{\Vert }=p_{\Vert ,i}$ ), which is justified in the limit of cold electrons (as expected in RIAFs, e.g. Sharma et al. Reference Sharma, Quataert, Hammett and Stone2007). We have also neglected non-ideal corrections to the induction equation (2.3) (e.g. the Hall term), which is appropriate given our neglect of finite Larmor radius (FLR) effects in (2.2) (we will, however, include a hyper-resistivity term in equation (2.3) for numerical reasons; see § 2.2). For convenience, we define the dimensionless anisotropy $\unicode[STIX]{x1D6E5}\equiv \unicode[STIX]{x0394}p/p_{0}$ , where $p_{0}=(p_{\bot }+2p_{\Vert })/3$ is the total thermal pressure, as well as the ratio of thermal to magnetic pressure $\unicode[STIX]{x1D6FD}\equiv 8\unicode[STIX]{x03C0}p_{0}/B^{2}$ , the Alfvén speed $v_{A}=B/\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}}$ and its $\hat{\boldsymbol{z}}$ component $v_{Az}=B_{z}/\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}}$ , the sound speed $c_{s}=\sqrt{p_{0}/\unicode[STIX]{x1D70C}}$ and the parallel sound speed $c_{s\Vert }=\sqrt{p_{\Vert }/\unicode[STIX]{x1D70C}}$ . The double-dot notation used in (2.4)–(2.5) and throughout this work is $\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}\equiv \sum _{i,j}b_{i}b_{j}\unicode[STIX]{x2202}_{i}u_{j}$ .

In their present form, equations (2.1)–(2.5) are not closed, due to the presence of the unspecified heat fluxes, $q_{\bot }$ and $q_{\Vert }$ . These must be either specified using a closure scheme, neglected or solved for using the full kinetic equations. In this work we consider three closures for $q_{\bot }$ and $q_{\Vert }$ (or equivalently, three approximations to (2.4)–(2.5)). These will be seen to lead to quite different behaviour in solutions of (2.1)–(2.5). They are:

Collisionless Landau-fluid closure. Landau-fluid (LF) closures have been used extensively in the fusion community (Hammett & Perkins Reference Hammett and Perkins1990; Hammett, Dorland & Perkins Reference Hammett, Dorland and Perkins1992; Snyder, Hammett & Dorland Reference Snyder, Hammett and Dorland1997) and, to a lesser degree, for astrophysical applications (Reference Sharma, Hammett, Quataert and StoneS06; Sharma et al. Reference Sharma, Quataert, Hammett and Stone2007). They are particularly well suited for modelling collisionless ( $\unicode[STIX]{x1D708}_{c}=0$ ) plasmas. In the LF closure, the heat fluxes,

(2.6) $$\begin{eqnarray}\displaystyle & \displaystyle q_{\bot }=-\frac{2c_{s\Vert }^{2}}{\sqrt{2\unicode[STIX]{x03C0}}c_{s\Vert }|k_{\Vert }|+\unicode[STIX]{x1D708}_{c}}\left[\unicode[STIX]{x1D70C}\unicode[STIX]{x1D735}_{\Vert }\left(\frac{p_{\bot }}{\unicode[STIX]{x1D70C}}\right)-p_{\bot }\left(1-\frac{p_{\bot }}{p_{\Vert }}\right)\frac{\unicode[STIX]{x1D735}_{\Vert }B}{B}\right], & \displaystyle\end{eqnarray}$$

(2.7) $$\begin{eqnarray}\displaystyle & \displaystyle q_{\Vert }=-\frac{8c_{s\Vert }^{2}}{\sqrt{8\unicode[STIX]{x03C0}}c_{s\Vert }|k_{\Vert }|+(3\unicode[STIX]{x03C0}-8)\unicode[STIX]{x1D708}_{c}}\,\unicode[STIX]{x1D70C}\unicode[STIX]{x1D735}_{\Vert }\left(\frac{p_{\Vert }}{\unicode[STIX]{x1D70C}}\right), & \displaystyle\end{eqnarray}$$

are constructed to replicate the effects of linear Landau damping. Here $\unicode[STIX]{x1D735}_{\Vert }\equiv \hat{\boldsymbol{b}}\boldsymbol{\cdot }\unicode[STIX]{x1D735}$ denotes the gradient parallel to the field and $|k_{\Vert }|$ denotes the wavenumber parallel to the field, which must be considered as an operator because it appears in the denominator of (2.6)–(2.7). The forms of the heat fluxes in (2.6)–(2.7) accurately reproduce the true kinetic growth rates and frequencies for a variety of large-scale (MHD) modes, including the MRI (Reference Quataert, Dorland and HammettQ02; Sharma et al. Reference Sharma, Hammett and Quataert2003). We refer the reader to Snyder et al. (Reference Snyder, Hammett and Dorland1997) and Reference Sharma, Hammett, Quataert and StoneS06 for more information.

Weakly collisional ‘Braginskii’ closure. In the Braginskii regime, $|\unicode[STIX]{x1D735}\boldsymbol{u}|\ll \unicode[STIX]{x1D708}_{c}$ (Braginskii Reference Braginskii1965), the pressure anisotropy is strongly influenced by collisional relaxation. We thus neglect $\text{d}_{t}p_{\bot }$ and $\text{d}_{t}p_{\Vert }$ in (2.4)–(2.5) and balance the double-adiabatic production of pressure anisotropy (the $\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}$ and $\unicode[STIX]{x1D735}\boldsymbol{\cdot }\boldsymbol{u}$ terms) against its collisional relaxation (the $\unicode[STIX]{x1D708}_{c}\unicode[STIX]{x0394}p$ terms) to find

(2.8) $$\begin{eqnarray}\unicode[STIX]{x1D6E5}\approx \frac{1}{\unicode[STIX]{x1D708}_{c}}\left(\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}-\frac{1}{3}\unicode[STIX]{x1D735}\boldsymbol{\cdot }\boldsymbol{u}\right)=\frac{1}{\unicode[STIX]{x1D708}_{c}}\frac{\text{d}}{\text{d}t}\ln \frac{B}{\unicode[STIX]{x1D70C}^{2/3}},\end{eqnarray}$$

where we have also used the fact that $\unicode[STIX]{x1D708}_{c}/|\unicode[STIX]{x1D735}\boldsymbol{u}|\gg 1$ implies $\unicode[STIX]{x0394}p\ll p_{0}$ . (For $\unicode[STIX]{x1D6FD}\gg 1$ , the $\unicode[STIX]{x1D735}\boldsymbol{\cdot }\boldsymbol{u}$ term can also be neglected.) When inserted into the momentum equation (2.2), equation (2.8) has the form of an anisotropic viscous stress, and is thus referred to as ‘Braginskii viscosity’ (or Braginskii MHD for the full set of equations). Note that we have neglected heat fluxes in arriving at (2.8), a simplification that is rigorously obtained if $\unicode[STIX]{x1D708}_{c}/|\unicode[STIX]{x1D735}\boldsymbol{u}|\gg \unicode[STIX]{x1D6FD}^{1/2}$ (the ‘high-collisionality’ regime). On the other hand, if $\unicode[STIX]{x1D708}_{c}/|\unicode[STIX]{x1D735}\boldsymbol{u}|\ll \unicode[STIX]{x1D6FD}^{1/2}$ (the ‘moderate-collisionality’ regime), the heat fluxes are strong over the time scales of the motion (Mikhailovskii & Tsypin Reference Mikhailovskii and Tsypin1971), and their contribution to the (ion) pressure anisotropy must be retained. (See § B.4 for further discussion.) In this case, there is no simple closure that can be devised (e.g. see appendix B of Squire, Schekochihin & Quataert Reference Squire, Schekochihin and Quataert2017) and it is usually easier to consider the full LF system.

Double-adiabatic closure. The double-adiabatic, or Chew–Goldberger–Low (CGL), closure (Chew et al. Reference Chew, Goldberger and Low1956) simply involves setting $q_{\bot }=q_{\Vert }=0$ . This approximation is far from justified for subsonic motions in the high- $\unicode[STIX]{x1D6FD}$ plasmas considered here; however, the closure is useful for comparison with the LF closure by virtue of its relative simplicity. It has also been employed in a variety of previous computational studies (e.g. Reference Sharma, Hammett, Quataert and StoneS06; Kowal, Falceta-Gonçalves & Lazarian Reference Kowal, Falceta-Gonçalves and Lazarian2011, Santos-Lima et al. Reference Santos-Lima, de Gouveia Dal Pino, Kowal, Falceta-Gonçalves, Lazarian and Nakwacki2014), and so it is worthwhile to diagnose the model’s successes and limitations.

An important caveat for each of these approximations to (2.4)–(2.5) relates to plasma microinstabilities. For our purposes, given the focus of this work on the high- $\unicode[STIX]{x1D6FD}$ regime, the most significant of these are the firehose instability (Rosenbluth Reference Rosenbluth1956; Chandrasekhar, Kaufman & Watson Reference Chandrasekhar, Kaufman and Watson1958; Parker Reference Parker1958; Yoon, Wu & de Assis Reference Yoon, Wu and de Assis1993), which is excited if

(2.9) $$\begin{eqnarray}\unicode[STIX]{x1D6E5}\lesssim -\frac{2}{\unicode[STIX]{x1D6FD}},\end{eqnarray}$$

and the mirror instability (Hasegawa Reference Hasegawa1969; Southwood & Kivelson Reference Southwood and Kivelson1993; Hellinger Reference Hellinger2007), which is excited if

(2.10) $$\begin{eqnarray}\unicode[STIX]{x1D6E5}\gtrsim \frac{1}{\unicode[STIX]{x1D6FD}}.\end{eqnarray}$$

(There are corrections to these $\unicode[STIX]{x1D6FD}$ -dependent thresholds that arise from particle resonances and depend on the specific form of the distribution function; see, e.g. Klein & Howes Reference Klein and Howes2015.) Important aspects of these instabilities (e.g. their regularization at small scales or particle scattering in their nonlinear evolution) are not captured by the closures we employ here, and kinetic calculations are needed to correctly understand their saturation. There have been a variety of recent works in this vein (Hellinger & Trávníček Reference Hellinger and Trávníček2008; Schekochihin et al. Reference Schekochihin, Cowley, Kulsrud, Rosin and Heinemann2008; Rosin et al. Reference Rosin, Schekochihin, Rincon and Cowley2011; Kunz, Schekochihin & Stone Reference Kunz, Schekochihin and Stone2014a ; Hellinger et al. Reference Hellinger, Matteini, Landi, Verdini, Franci and Trávníček2015; Rincon, Schekochihin & Cowley Reference Rincon, Schekochihin and Cowley2015; Riquelme, Quataert & Verscharen Reference Riquelme, Quataert and Verscharen2015; Sironi & Narayan Reference Sironi and Narayan2015; Melville, Schekochihin & Kunz Reference Melville, Schekochihin and Kunz2016; Riquelme, Quataert & Verscharen Reference Riquelme, Quataert and Verscharen2016), which have shown that these microinstabilities generally act to pin the pressure anisotropy at the marginal stability limits. Interestingly, when $\unicode[STIX]{x1D6E5}$ is driven beyond the stability boundaries, the microinstabilities achieve this in two stages: first, while the microscale fluctuations are growing secularly, by increasing (if $\text{d}_{t}B<0$ ) or decreasing (if $\text{d}_{t}B>0$ ) the magnetic-field strength $B$ (in other words, the small-scale fluctuations contribute to $B$ ); second, as the instabilities saturate, by enhancing the scattering of particles and thus increasing $\unicode[STIX]{x1D708}_{c}$ in (2.4)–(2.5). While the time for the firehose instability at moderate $\unicode[STIX]{x1D6FD}$ to saturate is essentially set by gyro-scale physics, and so might be considered as instantaneous in a fluid model, the mirror instability saturates on a time scales comparable to the turnover time of the large-scale motions driving the anisotropy (see § 6.3 and Kunz et al. Reference Kunz, Schekochihin and Stone2014a , Rincon et al. Reference Rincon, Schekochihin and Cowley2015, Riquelme et al. Reference Riquelme, Quataert and Verscharen2015, Melville et al. Reference Melville, Schekochihin and Kunz2016). We also note that there are also various other kinetic instabilities that could be important, for instance, the ion-cyclotron instability, or electron instabilities. We do not consider these in detail because the mirror and firehose instabilities are thought to be the most relevant to the high- $\unicode[STIX]{x1D6FD}$ , ion-dominated regime that is the focus of this work (see § 5 for further discussion).

In practice, because the primary effect in both the secular and scattering regimes is to limit $\unicode[STIX]{x1D6E5}$ at the threshold boundaries, we model these effects as a ‘hard-wall’ limit on $\unicode[STIX]{x1D6E5}$ , following prior work (Reference Sharma, Hammett, Quataert and StoneS06; Sharma et al. Reference Sharma, Quataert, Hammett and Stone2007, Santos-Lima et al. Reference Santos-Lima, de Gouveia Dal Pino, Kowal, Falceta-Gonçalves, Lazarian and Nakwacki2014, Chandra et al. Reference Chandra, Gammie, Foucart and Quataert2015, Foucart et al. Reference Foucart, Chandra, Gammie and Quataert2015). This simply limits $\unicode[STIX]{x1D6E5}$ to $1/\unicode[STIX]{x1D6FD}$ or $-2/\unicode[STIX]{x1D6FD}$ if the dynamics drives $\unicode[STIX]{x1D6E5}$ across these boundaries.Footnote ³ One should, however, be careful with this simple ‘limiter’ method not to inadvertently remove interesting physics from the model. For instance, the parallel firehose instability is destabilized at the same point $\unicode[STIX]{x1D6E5}=-2/\unicode[STIX]{x1D6FD}$ as where the magnetic tension is nullified by $\unicode[STIX]{x0394}p$ (indeed, this is the cause of the instability), which can have a strong influence on the largest scales (Squire, Quataert & Schekochihin Reference Squire, Quataert and Schekochihin2016; Squire et al. Reference Squire, Schekochihin and Quataert2017) and is captured in even our simplest 1-D models. For this reason, in considering azimuthal-field KMRI modes, we have run calculations both with and without a firehose limiter, seeing very similar dynamics in each case. Finally, we note that with finite scale separations between $\unicode[STIX]{x1D6FA}_{i}$ and $S$ , as is the case in numerical simulations (Riquelme et al. Reference Riquelme, Quataert, Sharma and Spitkovsky2012; Hoshino Reference Hoshino2015; Kunz et al. Reference Kunz, Stone and Quataert2016), there can be significant overshoot of the pressure anisotropy beyond the limits (2.9) and (2.10) (Kunz et al. Reference Kunz, Schekochihin and Stone2014a ). This overshoot may be important for the large-scale evolution (see § 3) but is probably not representative of what happens in real systems, which usually have a very large dynamic range between $\unicode[STIX]{x1D6FA}_{i}$ and $S$ . These effects are discussed in detail in § 6.

2.2 Computational methods

A number of different numerical methods are used to solve (2.1)–(2.7). For investigating the 1-D evolution of a channel mode, we use a pseudo-spectral method, with standard dealiasing and hyper-diffusion operators used to remove the energy just above the grid scale. A very similar numerical method, albeit on a 3-D Fourier grid, is used for the studies of parasitic modes. For studies of the fully nonlinear 3-D evolution, we use a modified version of the finite-difference code Zeus, as described in Reference Sharma, Hammett, Quataert and StoneS06. For simulations in the weakly collisional regime, we solve the full LF system (2.1)–(2.7), so as to correctly capture the effects of the heat fluxes in the moderate- and high-collisionality regimes (see § B.4).

A few words are needed regarding the numerical treatment of heat fluxes in the LF model (2.6)–(2.7). In particular, the $1/|k_{\Vert }|$ operator is numerically awkward, because it is not diagonal in either Fourier space or real space. We thus use the prescription of Reference Sharma, Hammett, Quataert and StoneS06 and replace this by a pre-chosen $k_{L}$ for the Zeus implementation and the parasitic-mode studies, while for the 1-D collisionless calculations we use $1/|k_{\Vert }|=1/|k_{z}|$ (once the mode reaches larger amplitude this may somewhat underestimate the heat fluxes, since $k_{\Vert }<k_{z}$ if the field lines are not straight). Following Reference Sharma, Hammett, Quataert and StoneS06, we have checked that varying the choice of $k_{L}$ within a reasonable range, or using the choice $|k_{\Vert }|=|k_{z}|$ , does not significantly affect the dynamics.

We use the methods detailed in appendix A3 of Reference Sharma, Hammett, Quataert and StoneS06 to limit the pressure anisotropy: $\unicode[STIX]{x1D708}_{c}$ is instantaneously increased in (2.4)–(2.5) whenever $\unicode[STIX]{x1D6E5}$ passes the limits (2.9) or (2.10). We do not make any distinction between the ‘secular growth’ and ‘particle scattering’ phases of microinstability evolution with this method (see discussion above, around (2.10), and § 6.3), and more study is needed to better understand the successes and limitations of this simple limiter approach.

2.3 General comparison of kinetic models

Before commencing with our analysis of the KMRI, we highlight in this section some of the key similarities and differences between the LF, Braginskii and CGL models, as well as that of standard MHD.

First, irrespective of the closure details, the general effect of pressure anisotropy is to modify the Lorentz force, either by enhancing ( $\unicode[STIX]{x0394}p>0$ ) or reducing ( $\unicode[STIX]{x0394}p<0$ ) the effective magnetic tension (see (2.2)). The same relative pressure anisotropy $\unicode[STIX]{x1D6E5}=\unicode[STIX]{x0394}p/p_{0}$ will thus have a greater dynamical effect as $\unicode[STIX]{x1D6FD}$ increases, because $p_{0}$ increases compared to $B$ . In contrast, the generation of $\unicode[STIX]{x1D6E5}$ in a changing magnetic field,

(2.11) $$\begin{eqnarray}\frac{\text{d}\unicode[STIX]{x1D6E5}}{\text{d}t}\sim \hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}\sim \frac{\text{d}\ln B}{\text{d}t}\end{eqnarray}$$

(or $\unicode[STIX]{x1D6E5}\sim \unicode[STIX]{x1D708}_{c}^{-1}\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}$ for Braginskii), does not depend on $\unicode[STIX]{x1D6FD}$ . Thus, the dynamics of higher- $\unicode[STIX]{x1D6FD}$ plasmas is in general more strongly influenced by self-generated pressure anisotropies than is the dynamics of lower- $\unicode[STIX]{x1D6FD}$ plasmas.

Secondly, the spatial form of $\unicode[STIX]{x0394}p$ generated in a given time-dependent $B$ differs significantly between the LF, CGL and Braginskii models. This $\unicode[STIX]{x0394}p$ is important for the nonlinear behaviour of the collisionless MRI. The influence of a spatially constant $\unicode[STIX]{x1D6E5}$ can be considered from an essentially linear standpoint: it simply acts to enhance or reduce the Lorentz force by the factor $(1+\unicode[STIX]{x1D6FD}\unicode[STIX]{x1D6E5}/2)$ . In contrast, when the spatial variation in $\unicode[STIX]{x1D6E5}$ is similar to its magnitude, its effect is inherently nonlinear. For the same reason, detailed conclusions about the expected change in the spatial shape of an MRI mode due to pressure anisotropy do depend on the regime of interest (and model) – for example, collisionless versus Braginskii (Squire et al. Reference Squire, Quataert and Schekochihin2016), or low versus high $\unicode[STIX]{x1D6FD}$ – rather than being generic consequences of any self-generated pressure anisotropy. For our purposes, one can consider high-collisionality Braginskii MHD (equation (2.8)) as the limiting model that develops large spatial variation in $\unicode[STIX]{x1D6E5}$ (since $\unicode[STIX]{x1D6E5}$ is tied directly to $\text{d}_{t}B$ ), while the high- $\unicode[STIX]{x1D6FD}$ limit of the LF model is the opposite, developing large $\unicode[STIX]{x1D6E5}$ with very little spatial variation.Footnote ⁴ This is because collisions generically act to reduce the magnitude of $\unicode[STIX]{x1D6E5}$ without affecting the spatial variation in $p_{\bot }$ and $p_{\Vert }$ , whereas heat fluxes act to reduce spatial variation in $p_{\bot }$ and $p_{\Vert }$ without affecting the spatial average of $\unicode[STIX]{x1D6E5}$ .

This last statement warrants further explanation, given the complexity of (2.4)–(2.7). The effect of the LF heat fluxes (2.6)–(2.7) can be clarified if we assume $\unicode[STIX]{x1D708}_{c}=0$ and $\unicode[STIX]{x0394}p\ll p_{0}$ (the latter is always valid at high $\unicode[STIX]{x1D6FD}$ ), so that

(2.12a,b ) $$\begin{eqnarray}q_{\Vert }\approx -\sqrt{\frac{8}{\unicode[STIX]{x03C0}}}\unicode[STIX]{x1D70C}c_{s}\frac{\unicode[STIX]{x1D735}_{\Vert }}{|k_{\Vert }|}\left(\frac{p_{\Vert }}{\unicode[STIX]{x1D70C}}\right),\quad q_{\bot }\approx -\sqrt{\frac{2}{\unicode[STIX]{x03C0}}}\unicode[STIX]{x1D70C}c_{s}\frac{\unicode[STIX]{x1D735}_{\Vert }}{|k_{\Vert }|}\left(\frac{p_{\bot }}{\unicode[STIX]{x1D70C}}\right).\end{eqnarray}$$

Then, assuming $\hat{\boldsymbol{b}}\boldsymbol{\cdot }\unicode[STIX]{x1D735}q_{\bot ,\Vert }\gg q_{\bot ,\Vert }\unicode[STIX]{x1D735}\boldsymbol{\cdot }\hat{\boldsymbol{b}}$ , which is valid when the perturbation to the background field is small (i.e. when the field lines are nearly straight), the contribution to the $p_{\bot }$ and $p_{\Vert }$ evolution equations has the form $\unicode[STIX]{x2202}_{t}p_{\bot }\sim -\unicode[STIX]{x1D70C}c_{s}|k_{\Vert }|(p_{\bot }/\unicode[STIX]{x1D70C})$ and $\unicode[STIX]{x2202}_{t}p_{\Vert }\sim -\unicode[STIX]{x1D70C}c_{s}|k_{\Vert }|(p_{\Vert }/\unicode[STIX]{x1D70C})$ , respectively. These terms, which model the effect of Landau damping (Snyder et al. Reference Snyder, Hammett and Dorland1997), act as a ‘scale-independent’ diffusion of $p_{\bot }$ and $p_{\Vert }$ , damping inhomogeneitiesFootnote ⁵ over the sound-wave time scale $|k_{\Vert }|c_{s}$ . This is important because $|k_{\Vert }|c_{s}\sim \unicode[STIX]{x1D6FD}^{1/2}\unicode[STIX]{x1D6FE}_{\text{MRI}}$ (where $\unicode[STIX]{x1D6FE}_{\text{MRI}}$ is the MRI growth rate), showing that for $\unicode[STIX]{x1D6FD}\gg 1$ , the heat fluxes will rapidly erase spatial variation in $\unicode[STIX]{x0394}p$ on the time scale that the MRI grows. As a result, the spatial variation in $\unicode[STIX]{x0394}p$ will be dwarfed by its mean; i.e. $\unicode[STIX]{x0394}p$ will be nearly spatially constant. A more thorough discussion of these ideas is given in appendix B, where we solve explicitly for the $\unicode[STIX]{x0394}p$ that arises in an exponentially growing, spatially varying magnetic perturbation. This shows that the double-adiabatic model for $p_{\bot ,\Vert }$ generates a $\unicode[STIX]{x0394}p$ with spatial variation of the order of its mean, while the addition of LF heat fluxes decreases the spatial variation of $\unicode[STIX]{x0394}p$ by a factor $\unicode[STIX]{x1D6FD}^{1/2}$ while leaving the mean $\unicode[STIX]{x0394}p$ unchanged.

3.1 Linear KMRI

Before discussing any nonlinear effects, it is helpful to first review aspects of the linear KMRI. We consider only the simplest case of purely vertical wavenumbers $k_{z}\neq 0$ , $k_{x}=k_{y}=0$ ; i.e. $(\boldsymbol{k}\Vert \boldsymbol{B}\Vert \unicode[STIX]{x1D734})$ . This choice is motivated by the stabilizing influence of a non-zero radial wavenumber $k_{x}$ (see discussion in § 4 of Reference Quataert, Dorland and HammettQ02), meaning that $k_{x}=0$ modes should dominate if growing from small amplitudes, while treating $k_{y}\neq 0$ modes requires a global and/or time-dependent method (Balbus & Hawley Reference Balbus and Hawley1992; Johnson Reference Johnson2007; Squire & Bhattacharjee Reference Squire and Bhattacharjee2014a ). We also neglect the possibility of a radial background magnetic field since this leads to a time-dependent background azimuthal field. More thorough discussion and detailed derivations can be found in Reference Quataert, Dorland and HammettQ02; Sharma et al. (Reference Sharma, Hammett and Quataert2003), Balbus (Reference Balbus2004), Rosin & Mestel (Reference Rosin and Mestel2012), Heinemann & Quataert (Reference Heinemann and Quataert2014), Quataert et al. (Reference Quataert, Heinemann and Spitkovsky2015), as well in appendix A, where we derive properties of the KMRI in a mixed-vertical–azimuthal field.

Figure 1.

Dimensionless linear growth rate $\unicode[STIX]{x1D6FE}/\unicode[STIX]{x1D6FA}$ of the KMRI at $\unicode[STIX]{x1D6FD}_{0z}=8\unicode[STIX]{x03C0}p_{0}/B_{0z}^{2}=400$ and $S/\unicode[STIX]{x1D6FA}=3/2$ , plotted as a function of dimensionless vertical wavenumber $k_{z}v_{Az}/\unicode[STIX]{x1D6FA}$ (with $k_{x}=k_{y}=0$ ). The solid blue curve shows the case with a purely vertical $\boldsymbol{B}_{0}$ and no background pressure anisotropy $\unicode[STIX]{x1D6E5}_{0}$ , for which the dispersion relation is identical to the standard MRI. The orange dashed line shows the case with $B_{0y}=0$ and $\unicode[STIX]{x1D6E5}_{0}=1/\unicode[STIX]{x1D6FD}_{0}$ , which is approximately the anisotropy at which the mirror limit is first reached in the growing mode. Finally, the green dotted line shows the growth rate in the case with an azimuthal field $B_{0y}=B_{0z}$ (with $\unicode[STIX]{x1D6FD}_{0z}=400$ , $\unicode[STIX]{x1D6FD}_{0}=200$ ), where the growth rate is strongly enhanced compared to the MHD MRI (which is unaffected by the azimuthal field for $k_{x}=k_{y}=0$ ).

We linearize (2.1)–(2.7) with $\unicode[STIX]{x1D708}_{c}=0$ and $S/\unicode[STIX]{x1D6FA}=3/2$ , then insert the Fourier ansatz $\unicode[STIX]{x1D6FF}f(z,t)=\unicode[STIX]{x1D6FF}f\text{e}^{\text{i}kz-\text{i}\unicode[STIX]{x1D714}t}$ for each variable ( $f=\unicode[STIX]{x1D70C}$ , $\boldsymbol{u}$ , $\boldsymbol{B}$ etc.). Solution of the resulting polynomial equation for $\unicode[STIX]{x1D714}$ yields the linear KMRI growth rates, $\unicode[STIX]{x1D6FE}/\unicode[STIX]{x1D6FA}=\text{Im}(\unicode[STIX]{x1D714})/\unicode[STIX]{x1D6FA}$ , as shown in figure 1 for several relevant cases. For the case of purely vertical field and no background pressure anisotropy (solid line), the KMRI dispersion relation is identical to the collisional MRI. This occurs because when $\boldsymbol{B}_{0}=B_{0}\hat{\boldsymbol{z}}$ the MRI does not linearly perturb the pressure (because $\unicode[STIX]{x2202}_{z}(\boldsymbol{B}_{0}\boldsymbol{\cdot }\unicode[STIX]{x1D6FF}\boldsymbol{B})=0$ ), and thus is ignorant of the equation of state. With a non-zero radial wavenumber $k_{x}\neq 0$ , this is no longer the case (since then $\unicode[STIX]{x1D6FF}B_{z}\neq 0$ ), and the growth rate is lower than for the standard MRI.

The addition of a background positive pressure anisotropy, $\unicode[STIX]{x1D6E5}_{0}>0$ , shifts the MRI to larger wavelengths (smaller $k$ ; dashed curve in figure 1). This is because the anisotropic-pressure stress in the momentum equation has a form identical to that of the Lorentz force (see (2.2)). Thus the only difference in comparison to the standard MRI dispersion relation is the replacement of $kv_{A}$ with $kv_{A}(1+\unicode[STIX]{x1D6FD}_{0}\unicode[STIX]{x1D6E5}_{0}/2)^{1/2}$ , which decreases the wavenumber that maximizes $\unicode[STIX]{x1D6FE}$ from ${\sim}\!\unicode[STIX]{x1D6FA}v_{A}^{-1}$ to ${\sim}\!\unicode[STIX]{x1D6FA}v_{A}^{-1}(1+\unicode[STIX]{x1D6FD}_{0}\unicode[STIX]{x1D6E5}_{0}/2)^{-1/2}$ , while keeping the maximum itself constant. This is relevant to the nonlinear behaviour of the KMRI, since the mode generates a pressure anisotropy as it evolves.

Finally, the addition of a background azimuthal field causes the KMRI dispersion relation to differ significantly from that of the standard MRI (Reference Quataert, Dorland and HammettQ02; Balbus Reference Balbus2004; dotted curve in figure 1), increasing the growth rate and moving the instability to larger wavelengths. This differs from the standard (MHD) MRI, which is unaffected by $B_{0y}\neq 0$ when $k_{y}=0$ . Due to the different physical processes that lead to the large growth rates at low $k$ , this instability is also known as the magnetoviscous instability (MVI; Balbus Reference Balbus2004). Unlike the standard MRI, the growth mechanism relies on the azimuthal pressure force $\hat{\boldsymbol{b}}_{0}\hat{\boldsymbol{b}}_{0}\unicode[STIX]{x1D6FF}\unicode[STIX]{x0394}p$ , which is destabilizing and dominates over the magnetic tension by a factor of $\unicode[STIX]{x1D6FD}_{0}^{1/2}$ (see Reference Quataert, Dorland and HammettQ02). As shown in appendix A, for $\unicode[STIX]{x1D6FD}_{0}\gg 1$ the KMRI growth rate approaches $\unicode[STIX]{x1D6FE}=(2S\unicode[STIX]{x1D6FA})^{1/2}$ , with a maximum growth rate at wavenumber $k_{\text{max}}v_{Az}/\unicode[STIX]{x1D6FA}\approx 1.8\,\unicode[STIX]{x1D6FD}_{0z}^{-1/6}$ when $B_{0y}\approx B_{0z}$ and $S/\unicode[STIX]{x1D6FA}=3/2$ (see (A 2)). In this fastest-growing mode, the relative amplitudes of the various components are $\unicode[STIX]{x1D6FD}_{0}^{-2/3}\unicode[STIX]{x1D6FF}B_{x}/B_{0}\sim \unicode[STIX]{x1D6FD}_{0}^{-1/3}\unicode[STIX]{x1D6FF}B_{y}/B_{0}\sim \unicode[STIX]{x1D6FD}_{0}^{-5/6}\unicode[STIX]{x1D6FF}u_{x}/v_{A}\sim \unicode[STIX]{x1D6FD}_{0}^{-5/6}\unicode[STIX]{x1D6FF}u_{y}/v_{A}\sim \unicode[STIX]{x1D6FF}p_{\bot ,\Vert }/p_{0}$ (unlike the standard MRI, where $\unicode[STIX]{x1D6FF}B_{x}/B_{0}\sim \unicode[STIX]{x1D6FF}B_{y}/B_{0}\sim \unicode[STIX]{x1D6FF}u_{x}/v_{A}\sim \unicode[STIX]{x1D6FF}u_{y}/v_{A}$ ). While we shall use these scalings below in our discussion of the nonlinear behaviour of MRI modes, we caution that they only apply at rather high $\unicode[STIX]{x1D6FD}_{0}$ , a problem that is exacerbated if $B_{0y}/B_{0z}\neq 1$ . At more moderate $\unicode[STIX]{x1D6FD}_{0}$ , as feasible for simulations, $k_{\text{max}}$ tends towards its value for the standard MRI, $k_{\text{max}}v_{Az}/\unicode[STIX]{x1D6FA}\approx 1$ (see figure 7). It is also worth noting that the dispersion relation, $\unicode[STIX]{x1D6FE}(k)$ , varies only slowly around $k=k_{\text{max}}$ (see e.g. dotted curve in figure 1). This implies that, if starting from random initial conditions, a long time would be required before the fastest-growing mode dominates, suggesting that when nonlinear effects become important there will likely still be several modes of similar amplitudes. With these caveats duly noted, in our discussion of nonlinear effects below (§ 3.3), we will consider only the fastest-growing KMRI mode (i.e. set $k=k_{\text{max}}$ ) and use the above scalings, rather than keep $k$ arbitrary.

Figure 2.

The structure of a kinetic MRI mode evolving in a vertical background field $B_{0z}$ in various regimes, as computed from the 1-D LF model (with $\unicode[STIX]{x1D708}_{c}\neq 0$ in panel c). We take $\unicode[STIX]{x1D6FD}_{0}=337$ in a domain with $\unicode[STIX]{x1D6FA}L_{z}/c_{s}=1$ , such that the peak of the MRI dispersion relation (i.e. the maximum $\unicode[STIX]{x1D6FE}$ ) is at $k=2\times 2\unicode[STIX]{x03C0}/L_{z}$ (each panel shows only half of a scale height). Each plot illustrates $\unicode[STIX]{x1D6FF}B_{x}$ (blue solid line), $\unicode[STIX]{x1D6FF}B_{y}$ (red dashed line), $\unicode[STIX]{x1D6FF}u_{x}$ (yellow dot-dashed line) and $\unicode[STIX]{x1D6FF}u_{y}$ (purple dotted line). The various panels show: (a) the linear KMRI mode (this is the initial conditions for each simulation), which is identical in structure to an MHD MRI mode at these parameters; (b) the collisionless MRI mode when $\unicode[STIX]{x0394}p$ reaches the mirror limit ( $\unicode[STIX]{x1D6FF}B\sim \unicode[STIX]{x1D6FD}^{-1/2}B_{0z}\approx 0.015$ ), which remains very nearly sinusoidal because the heat fluxes make $\unicode[STIX]{x0394}p$ spatially uniform; (c) a mode in the high-collisionality Braginskii regime (with $\unicode[STIX]{x1D708}_{c}/S=\unicode[STIX]{x1D6FD}_{0}^{3/4}$ ) when $\unicode[STIX]{x0394}p$ reaches the mirror limit (at $\unicode[STIX]{x1D6FF}B\sim (\unicode[STIX]{x1D708}_{c}/S)^{1/2}\unicode[STIX]{x1D6FD}^{-1/2}B_{0z}\approx 0.13$ ), which is non-sinusoidal because of the $O(1)$ spatial variation in $\unicode[STIX]{x0394}p$ ; (d) the MRI mode at very large amplitudes, when compressibility becomes important. The structure of this final compressible stage of evolution is the same across all models, including standard (collisional) MHD.

3.2 Nonlinear KMRI: vertical magnetic field

In this section, we consider the nonlinear evolution of the MRI in a vertical background field. In this case the linear dispersion relation is identical to that obtained in ideal MHD. However, we shall show that the modes are (modestly) nonlinearly modified by the pressure anisotropy at low amplitudes $\unicode[STIX]{x1D6FF}B\sim \unicode[STIX]{x1D6FD}^{-1/2}B_{0}$ . To do so, we first describe the evolution of a truly collisionless mode using the LF closure with $\unicode[STIX]{x1D708}_{c}=0$ (§ 3.2.1), and then examine the weakly collisional Braginskii case in § 3.2.2.

3.2.1 Collisionless (LF) regime

A maximally unstable MRI mode satisfies

(3.1a ) $$\begin{eqnarray}\displaystyle & \displaystyle \unicode[STIX]{x1D6FF}u_{x}=\unicode[STIX]{x1D6FF}u_{y}=-\sqrt{\frac{3}{5}}\frac{\unicode[STIX]{x1D6FF}B_{0}}{\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}}}\text{e}^{\unicode[STIX]{x1D6FE}t}\sin (kz), & \displaystyle\end{eqnarray}$$

(3.1b ) $$\begin{eqnarray}\displaystyle & \displaystyle -\unicode[STIX]{x1D6FF}B_{x}=\unicode[STIX]{x1D6FF}B_{y}=\unicode[STIX]{x1D6FF}B_{0}\text{e}^{\unicode[STIX]{x1D6FE}t}\cos (kz), & \displaystyle\end{eqnarray}$$

where $\unicode[STIX]{x1D6FE}=S/2$ is the growth rate and $\unicode[STIX]{x1D6FF}B_{0}$ is the initial mode amplitude. Because of the opposing signs between $\unicode[STIX]{x1D6FF}B_{x}\unicode[STIX]{x1D6FF}u_{x}$ and $\unicode[STIX]{x1D6FF}B_{y}\unicode[STIX]{x1D6FF}u_{y}$ in the mode, only $-S\hat{b}_{x}\hat{b}_{y}$ contributes to $\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}\approx -S\unicode[STIX]{x1D6FF}B_{x}\unicode[STIX]{x1D6FF}B_{y}/B_{0z}^{2}$ . As shown in § B.3, at high $\unicode[STIX]{x1D6FD}$ in a collisionless plasma (using the LF closure), the mean of the pressure anisotropy dominates over its spatial variation by a factor of $\unicode[STIX]{x1D6FD}^{1/2}$ (see (B 21)–(B 24)), and $\unicode[STIX]{x1D6E5}$ is approximately spatially constant:

(3.2) $$\begin{eqnarray}\unicode[STIX]{x1D6E5}\sim \frac{3}{2}\frac{\unicode[STIX]{x1D6FF}B_{0}^{2}}{B_{0z}^{2}}\text{e}^{2\unicode[STIX]{x1D6FE}t}.\end{eqnarray}$$

The mirror threshold is reached at $\unicode[STIX]{x1D6E5}=1/\unicode[STIX]{x1D6FD}$ , when $\unicode[STIX]{x1D6FF}B/B_{0z}\sim \unicode[STIX]{x1D6FD}_{0}^{-1/2}$ . As discussed in § 3.1, a positive pressure anisotropy modifies the MRI mode by effectively increasing the magnetic tension, and the mode will be stabilized if $kv_{A}\sqrt{1+\unicode[STIX]{x0394}(t)\unicode[STIX]{x1D6FD}_{0}/2}\geqslant \sqrt{2S\unicode[STIX]{x1D6FA}}$ . Fortunately, for a mode near the peak growth rate, $kv_{A}=\sqrt{S(\unicode[STIX]{x1D6FA}-S/4)}$ , this stabilization does not occur, because the fast-growing mirror fluctuations limit $\sqrt{1+\unicode[STIX]{x0394}(t)\unicode[STIX]{x1D6FD}_{0}/2}$ to values at or below $\sqrt{3/2}$ . As shown in figure 2(b), this pressure anisotropy causes a rather minor modification to the shape of the MRI mode because $\unicode[STIX]{x0394}p$ is almost spatially constant, decreasing $u_{x}$ and $B_{y}$ relative to $u_{y}$ and $B_{x}$ in the same way as for an MHD MRI mode that is not at the fastest-growing wavelength.Footnote ⁶

As the mode continues to evolve to larger amplitudes $\unicode[STIX]{x1D6FF}B/B_{0z}\gtrsim \unicode[STIX]{x1D6FD}_{0}^{-1/2}$ , the pressure anisotropy remains limited by mirror fluctuations. Leaving aside, for the moment, questions related to how the mode disrupts and becomes turbulent, there are two other amplitudes of interest: (i) when the mode amplitude surpasses the background field at $\unicode[STIX]{x1D6FF}B/B_{0z}\sim 1$ , and (ii) when compressibility becomes important at $\unicode[STIX]{x1D6FF}B/B_{0z}\sim \unicode[STIX]{x1D6FD}_{0}^{1/2}$ ( $\unicode[STIX]{x1D6FF}u\sim c_{s}$ ). Interestingly, if the pressure anisotropy is efficiently limited by mirror fluctuations, $\unicode[STIX]{x0394}p=B^{2}/8\unicode[STIX]{x03C0}$ , then the pressure anisotropy nonlinearity has little effect:

(3.3) $$\begin{eqnarray}\unicode[STIX]{x1D735}\boldsymbol{\cdot }(\unicode[STIX]{x0394}p\hat{\boldsymbol{b}}\hat{\boldsymbol{b}})=\frac{\unicode[STIX]{x1D735}\boldsymbol{\cdot }(B^{2}\hat{\boldsymbol{b}}\hat{\boldsymbol{b}})}{8\unicode[STIX]{x03C0}}=\frac{\boldsymbol{B}\boldsymbol{\cdot }\unicode[STIX]{x1D735}\boldsymbol{B}}{8\unicode[STIX]{x03C0}}=\frac{\boldsymbol{B}_{0}\boldsymbol{\cdot }\unicode[STIX]{x1D735}\unicode[STIX]{x1D6FF}\boldsymbol{B}+\unicode[STIX]{x1D6FF}\boldsymbol{B}\boldsymbol{\cdot }\unicode[STIX]{x1D735}\unicode[STIX]{x1D6FF}\boldsymbol{B}}{8\unicode[STIX]{x03C0}}=\frac{\boldsymbol{B}_{0}\boldsymbol{\cdot }\unicode[STIX]{x1D735}\unicode[STIX]{x1D6FF}\boldsymbol{B}}{8\unicode[STIX]{x03C0}},\end{eqnarray}$$

since $\unicode[STIX]{x1D6FF}\boldsymbol{B}\boldsymbol{\cdot }\unicode[STIX]{x1D735}\unicode[STIX]{x1D6FF}\boldsymbol{B}\approx 0$ for an MRI channel mode (Goodman & Xu Reference Goodman and Xu1994). Thus, once $\unicode[STIX]{x1D6FF}B_{x}\sim \unicode[STIX]{x1D6FF}B_{y}\gtrsim B_{0}$ , the effect of the pressure-anisotropy nonlinearity on the mode remains identical to when $\unicode[STIX]{x1D6FF}B_{x}\sim \unicode[STIX]{x1D6FF}B_{y}\lesssim B_{0}$ , even though the pressure anisotropy has a large ( $\unicode[STIX]{x0394}p\sim \unicode[STIX]{x1D6FF}B^{2}$ ) variation in space (i.e. the change is simply a modified magnetic tension, as shown in figure 2 b). In other words, because $\unicode[STIX]{x0394}p\propto B^{2}$ , there is no significant change to the mode as the mode amplitude surpasses the background field strength.

The final phase of evolution, once $\unicode[STIX]{x1D6FF}B\sim \unicode[STIX]{x1D6FD}^{1/2}B_{0}$ (i.e. $\unicode[STIX]{x1D6FF}u\sim c_{s}$ ), is then very similar to standard MHD, and the mode develops a rather distinctive shape, which we illustrate in figure 2(d). Because the nonlinearity is dominated at this point in the evolution by inhomogeneities in the density, this mode shape appears generically in all of the models studied here (including compressible MHD) across a wide range of parameters (cf. Latter et al. Reference Latter, Lesaffre and Balbus2009).

3.2.2 Weakly collisional (Braginskii) regime

In the Braginskii regime, which is valid for $\overline{\unicode[STIX]{x1D708}}_{c}\equiv \unicode[STIX]{x1D708}_{c}/S\sim \unicode[STIX]{x1D708}_{c}/\unicode[STIX]{x1D6FE}\gg 1$ and is relevant (i.e. represents a potentially significant correction to standard MHD) when $\overline{\unicode[STIX]{x1D708}}_{c}\ll \unicode[STIX]{x1D6FD}_{0}$ , there are two subregimes. In the moderate-collisionality regime, $\overline{\unicode[STIX]{x1D708}}_{c}\ll \unicode[STIX]{x1D6FD}_{0}^{1/2}$ , the heat fluxes play a very significant role and smooth the pressure anisotropy spatially, as occurs in the collisionless case described in § 3.2.1. In the high-collisionality regime, $\overline{\unicode[STIX]{x1D708}}_{c}\gg \unicode[STIX]{x1D6FD}_{0}^{1/2}$ , the heat fluxes are sub-dominant and do not play a significant dynamical role, leading to $\unicode[STIX]{x0394}p$ profiles that vary significantly in space. For more information, see § B.4 and appendix B of Squire et al. (Reference Squire, Schekochihin and Quataert2017).

In the moderate-collisionality regime, up to $\overline{\unicode[STIX]{x1D708}}_{c}\lesssim \unicode[STIX]{x1D6FD}_{0}^{1/2}$ , the behaviour of the mode at amplitudes $\unicode[STIX]{x1D6FF}B\lesssim (\unicode[STIX]{x1D6FD}_{0}/\overline{\unicode[STIX]{x1D708}}_{c})^{1/2}B_{0}$ (see below) is effectively identical to the collisionless regime discussed in § 3.2.1. In particular, the pressure anisotropy that develops from the growing mode with $\unicode[STIX]{x1D6FF}B\ll B_{0}$ is

(3.4) $$\begin{eqnarray}\unicode[STIX]{x1D6E5}\approx \frac{1}{\unicode[STIX]{x1D708}_{c}}\langle \hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\boldsymbol{ : }\unicode[STIX]{x1D735}\boldsymbol{u}\rangle \sim \frac{S}{\unicode[STIX]{x1D708}_{c}}\frac{\unicode[STIX]{x1D6FF}B_{0}^{2}}{B_{0z}^{2}}\,\text{e}^{2\unicode[STIX]{x1D6FE}t}=\frac{1}{\overline{\unicode[STIX]{x1D708}}_{c}}\frac{\unicode[STIX]{x1D6FF}B_{0}^{2}}{B_{0z}^{2}}\,\text{e}^{2\unicode[STIX]{x1D6FE}t},\end{eqnarray}$$

because the heat fluxes are smoothing $\unicode[STIX]{x0394}p$ faster than it is being created (by some factor between $\unicode[STIX]{x1D6FD}_{0}^{1/2}$ and $1$ , depending on $\overline{\unicode[STIX]{x1D708}}_{c}\,\unicode[STIX]{x1D6FD}_{0}^{-1/2}$ ; see Squire et al. Reference Squire, Schekochihin and Quataert2017). Thus, by the time that $\unicode[STIX]{x0394}p$ reaches the mirror limit (i.e. when $\unicode[STIX]{x1D6FF}B\sim (\overline{\unicode[STIX]{x1D708}}_{c}/\unicode[STIX]{x1D6FD}_{0})^{1/2}B_{0}$ ), it is nearly smooth in space, implying that the same conclusions reached in the collisionless limit also apply here. The same is then true as the mode continues growing to $\unicode[STIX]{x1D6FF}B\gtrsim B_{0}$ (but $\unicode[STIX]{x1D6FF}B\lesssim (\unicode[STIX]{x1D6FD}_{0}/\overline{\unicode[STIX]{x1D708}}_{c})^{1/2}B_{0}$ ); it forces $\unicode[STIX]{x0394}p$ to the mirror limit everywhere in space, implying the mode is not strongly affected by the pressure-anisotropy nonlinearity (see (3.3)).

In the high-collisionality regime, $\overline{\unicode[STIX]{x1D708}}_{c}\gg \unicode[STIX]{x1D6FD}_{0}^{1/2}$ , the heat fluxes do not significantly smooth spatial variation in $\unicode[STIX]{x0394}p$ and we must modify various aspects of the conclusions from the previous section. The pressure anisotropy that develops from the growing mode (for $\unicode[STIX]{x1D6FF}B\ll B_{0}$ ) is now spatially inhomogeneous:

(3.5) $$\begin{eqnarray}\unicode[STIX]{x1D6E5}=\frac{1}{\unicode[STIX]{x1D708}_{c}}\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}\sim \frac{1}{\overline{\unicode[STIX]{x1D708}}_{c}}\frac{\unicode[STIX]{x1D6FF}B_{0}^{2}}{B_{0z}^{2}}\,\text{e}^{2\unicode[STIX]{x1D6FE}t}\cos ^{2}(kz).\end{eqnarray}$$

This implies that, as the pressure anisotropy first reaches the mirror limit in some regions of space (near the antinodes of the mode, where $\text{d}_{t}\text{ln}~B$ is largest), it also changes the shape of the mode, viz., it couples different Fourier components of $\unicode[STIX]{x1D6FF}\boldsymbol{B}$ and $\unicode[STIX]{x1D6FF}\boldsymbol{u}$ . This causes minor modifications to the shape of the mode, which are shown in figure 2(c) for $\overline{\unicode[STIX]{x1D708}}_{c}=\unicode[STIX]{x1D6FD}_{0}^{3/4}$ (i.e. in the middle of the high-collisionality regime; the shape changes at other $\overline{\unicode[STIX]{x1D708}}_{c}$ and $\unicode[STIX]{x1D6FD}_{0}$ are generally similar to this). As the mode grows further, $\unicode[STIX]{x0394}p$ becomes limited by the mirror instability ( $\unicode[STIX]{x0394}p\propto B_{0}^{2}+\unicode[STIX]{x1D6FF}B^{2}$ ) across a larger region of space, implying (by the arguments above) that the mode regains its sinusoidal shape (albeit briefly, see next paragraph).

There is one final effect, not included in the collisionless discussion, which occurs in both the moderate-collisionality and high-collisionality Braginskii regimes at large mode amplitudes, $\unicode[STIX]{x1D6FF}B\gtrsim (\unicode[STIX]{x1D6FD}_{0}/\overline{\unicode[STIX]{x1D708}}_{c})^{1/2}B_{0}$ . The difference compared to the collisionless case arises because, in the Braginskii regime, $\unicode[STIX]{x0394}p$ is proportional to the current value of $\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}$ rather than to its time history. Once $\unicode[STIX]{x1D6FF}B\gtrsim B_{0}$ , this value $\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\,\boldsymbol{ : }\,\unicode[STIX]{x1D735}\boldsymbol{u}\approx -S\unicode[STIX]{x1D6FF}B_{x}\unicode[STIX]{x1D6FF}B_{y}/\unicode[STIX]{x1D6FF}B^{2}$ becomes constant in time, despite the fact that $B^{2}\approx \unicode[STIX]{x1D6FF}B^{2}$ is growing. Thus, $\unicode[STIX]{x0394}p$ moves back below the mirror limit when $\unicode[STIX]{x1D6FF}B^{2}\gtrsim p_{0}/\overline{\unicode[STIX]{x1D708}}_{c}$ , viz., when $\unicode[STIX]{x1D6FF}B\gtrsim (\unicode[STIX]{x1D6FD}_{0}/\overline{\unicode[STIX]{x1D708}}_{c})^{1/2}B_{0}$ . This occurs before compressibility affects the mode (at $\unicode[STIX]{x1D6FF}B\sim \unicode[STIX]{x1D6FD}_{0}^{1/2}B_{0}$ ), and causes the pressure anisotropy to vary in space, which in turn modifies the shape of the mode. These modifications are very minor, even at very high $\unicode[STIX]{x1D6FD}_{0}\sim 10^{5}$ and high $\overline{\unicode[STIX]{x1D708}}_{c}$ (not shown), and so it seems unlikely that they should modify mode saturation in three dimensions in any significant way. As the amplitude approaches $\unicode[STIX]{x1D6FF}B\sim \unicode[STIX]{x1D6FD}_{0}^{1/2}B_{0}$ , the mode is affected by compressibility in exactly the same way as is the collisionless (or MHD) MRI (see figure 2 d).

Figure 3.

(a) Energy evolution of each component of the growing KMRI mode in a mixed-azimuthal–vertical field with $B_{0y}=B_{0z}$ , at $\unicode[STIX]{x1D6FD}_{0}=5000$ ( $\unicode[STIX]{x1D6FD}_{0z}=10\,000$ ) in a domain such that $\unicode[STIX]{x1D6FA}L_{z}/c_{s}=1$ . We show $\unicode[STIX]{x1D6FF}B_{x}$ (solid purple line; $E_{\text{MRI}}=\int \text{d}z\,\unicode[STIX]{x1D6FF}B_{x}^{2}/8\unicode[STIX]{x03C0}$ ), $\unicode[STIX]{x1D6FF}B_{y}$ (solid green line; $E_{\text{MRI}}=\int \text{d}z\,\unicode[STIX]{x1D6FF}B_{y}^{2}/8\unicode[STIX]{x03C0}$ ), $\unicode[STIX]{x1D6FF}u_{x}$ (dashed blue line; $E_{\text{MRI}}=\int \text{d}z\,\unicode[STIX]{x1D70C}\unicode[STIX]{x1D6FF}u_{x}^{2}/2$ ), and $\unicode[STIX]{x1D6FF}u_{y}$ (dashed red line; $E_{\text{MRI}}=\int \text{d}z\,\unicode[STIX]{x1D70C}\unicode[STIX]{x1D6FF}u_{y}^{2}/2$ ). The calculation, which uses the 1-D LF model (2.1)–(2.7) with $\unicode[STIX]{x1D708}_{c}=0$ , is initialized with random Fourier amplitudes, scaled by $k^{-2}$ (initial phase of evolution not shown for clarity). For comparison, we also show the thermal energy (yellow dot-dashed line) and the energy of the background magnetic field (grey dot-dashed line). Following the linear phase with large growth rate (Region 1), the linearly perturbed pressure anisotropy reaches the mirror and firehose limits when $\unicode[STIX]{x1D6FF}B_{y}\sim \unicode[STIX]{x1D6FD}_{0}^{-2/3}B_{0y}$ , $\unicode[STIX]{x1D6FF}B_{x}\sim \unicode[STIX]{x1D6FD}_{0}^{-1/3}B_{0y}$ . There follows a transition phase (Region 2) in which the perturbed pressure anisotropy can no longer contribute to the instability and the mode moves to the much shorter wavelengths characteristic of the standard MRI. Then, once $\unicode[STIX]{x1D6FF}B_{y}>B_{0y}$ , the mode grows similarly to the vertical-field KMRI (Region 3) with $\unicode[STIX]{x1D6E5}$ at the mirror limit, until finally it is affected by compressibility in the same way as illustrated in figure 2(d) (Region 4). (b) Spatial structure of the azimuthal-field KMRI mode at a variety of times corresponding to ‘ $\times$ ’ markers in panel (a), which are chosen to illustrate the different phases of evolution. At each time, offset on the vertical axis for clarity with times listed in units of $\unicode[STIX]{x03A9}^{-1}$ , we show $\unicode[STIX]{x1D6FF}B_{x}/\max (\unicode[STIX]{x1D6FF}B)$ with solid lines, $\unicode[STIX]{x1D6FF}B_{y}/\max (\unicode[STIX]{x1D6FF}B)$ with dashed lines, and $\unicode[STIX]{x0394}p/\max (|\unicode[STIX]{x0394}p|)$ with dotted lines (the grey lines show $0$ to more clearly separate each curve). The mode transitions (around $t\approx 16~\unicode[STIX]{x03A9}^{-1}$ ) from structures characteristic of the azimuthal-field KMRI with $\unicode[STIX]{x0394}p$ both positive and negative, to those characteristic of the MHD-like vertical-field MRI, with the pressure anisotropy everywhere positive and at the mirror limit. Although less clean than the single-mode case studied in figure 2, the structures at very late times ( $t=24$ ) are again affected by compressibility in the same way (cf., $\unicode[STIX]{x1D6FF}B_{x}$ and $\unicode[STIX]{x1D6FF}B_{y}$ with those shown in figure 2 d).

3.3 Nonlinear KMRI: azimuthal–vertical magnetic field

In this section, we consider the effect of an additional background azimuthal magnetic field. We focus mainly on the collisionless KMRI (LF model; § 3.3.1), briefly mentioning the Braginskii version (for which the conclusions are similar) in § 3.3.2. As shown in figure 1, the MRI (or MVI) under such conditions is significantly different from the vertical background field case, growing fastest at long wavelengths $k_{\text{max}}v_{Az}/\unicode[STIX]{x1D6FA}\ll 1$ with growth rates exceeding $S/2$ . This situation is arguably more relevant astrophysically than is the pure vertical-field case: at high $\unicode[STIX]{x1D6FD}_{0}$ , even small azimuthal fields significantly modify the dispersion relation (see appendix A).

3.3.1 Collisionless (LF) regime

As with the vertical-field KMRI, nonlinear effects become important in the collisionless case at very low amplitudes, specifically when $\unicode[STIX]{x1D6FF}B_{y}\sim \unicode[STIX]{x1D6FD}_{0}^{-2/3}B_{0}$ (or when $\unicode[STIX]{x1D6FF}B_{x}\sim \unicode[STIX]{x1D6FD}_{0}^{-1/3}B_{0}$ , see (A 4)–(A 7)). Once the perturbed field becomes larger than the background field, the magnetic field is dominated by the mode itself and the instability again becomes similar to the MHD MRI (or, equivalently, the vertical-field KMRI at large amplitudes).

We now describe how such a mode transitions through four distinct stages in its nonlinear evolution, which is illustrated schematically in figure 3. Let us consider each stage of evolution separately, assuming $B_{0y}\approx B_{0z}=B_{0}/\sqrt{2}$ for the sake of simplicity:

(1) Linear evolution. Unlike in the vertical-field case, the KMRI mode linearly produces a pressure anisotropy,

(3.6) $$\begin{eqnarray}\unicode[STIX]{x1D6E5}\approx \sqrt{2\unicode[STIX]{x03C0}}\frac{1}{c_{s}k}\frac{\unicode[STIX]{x2202}_{t}\unicode[STIX]{x1D6FF}B_{y}}{B_{0}}\approx \sqrt{2\unicode[STIX]{x03C0}}\frac{\unicode[STIX]{x1D6FE}}{c_{s}k}\frac{\unicode[STIX]{x1D6FF}B_{y}}{B_{0}},\end{eqnarray}$$

because $\unicode[STIX]{x1D6FF}\boldsymbol{B}\boldsymbol{\cdot }\boldsymbol{B}_{0}=\unicode[STIX]{x1D6FF}B_{y}B_{0y}\neq 0$ (here we have set $B_{0y}\approx B_{0z}$ ; see Reference Quataert, Dorland and HammettQ02 and appendix A). This implies that, as the mode evolves, it pushes the plasma towards both the mirror limit, in regions where $\unicode[STIX]{x1D6FF}\boldsymbol{B}\boldsymbol{\cdot }\boldsymbol{B}_{0}>0$ (i.e. $\unicode[STIX]{x1D6FF}B_{y}B_{0y}>0$ ), and the firehose limit, in regions where $\unicode[STIX]{x1D6FF}\boldsymbol{B}\boldsymbol{\cdot }\boldsymbol{B}_{0}<0$ ( $\unicode[STIX]{x1D6FF}B_{y}B_{0y}<0$ ). Note that the factor $\unicode[STIX]{x1D6FE}/(c_{s}k)^{-1}\sim \unicode[STIX]{x1D6FD}_{0}^{-1/2}(v_{A}k/\unicode[STIX]{x1D6FE})^{-1}$ in (3.6) arises due to the smoothing effect of the heat fluxes and reduces $\unicode[STIX]{x1D6E5}$ significantly (for example, in the CGL model where $q_{\bot }=q_{\Vert }=0$ , $\unicode[STIX]{x1D6E5}\approx 3\unicode[STIX]{x1D6FF}B_{y}/B_{0}$ is much larger than (3.6)). The linear phase ends as $\unicode[STIX]{x1D6E5}$ approaches the microinstability limits $|\unicode[STIX]{x1D6E5}|\sim \unicode[STIX]{x1D6FD}^{-1}$ and becomes flattened by growing mirror and firehose fluctuations. Assuming the mode grows at the scale that maximizes the growth rate, $k_{\text{max}}v_{A}/\unicode[STIX]{x1D6FA}\sim \unicode[STIX]{x1D6FD}_{0}^{-1/6}$ (see (A 2) and figure 7), these limits are reached when $\unicode[STIX]{x1D6FF}B_{y}\sim \unicode[STIX]{x1D6FD}^{-2/3}B_{0}$ , or when $\unicode[STIX]{x1D6FF}B_{x}\sim \unicode[STIX]{x1D6FD}^{-1/3}B_{0}$ (since $\unicode[STIX]{x1D6FF}B_{x}\sim \unicode[STIX]{x1D6FD}_{0}^{1/3}\unicode[STIX]{x1D6FF}B_{y}$ for these fastest-growing modes; see (A 4)–(A 7)). At this point, the perturbation of $B$ due to $\unicode[STIX]{x1D6FF}B_{x}$ is similar to that due to $\unicode[STIX]{x1D6FF}B_{y}$ , meaning that both components contribute to the pressure anisotropy.Footnote ⁷

(2) Pressure anisotropy limited, with $\unicode[STIX]{x1D6FF}B_{y}<B_{0y}$ . In the limit that the mirror and firehose fluctuations efficiently constrain the growing $|\unicode[STIX]{x1D6E5}|$ , the pressure profile will develop a step function profile in space between the mirror limit, $\unicode[STIX]{x1D6E5}\approx 1/\unicode[STIX]{x1D6FD}$ , and the firehose limit $\unicode[STIX]{x1D6E5}\approx -2/\unicode[STIX]{x1D6FD}$ (see figure 3 b at $t=12.5~\unicode[STIX]{x03A9}^{-1}$ ). A key effect of these limits is that they suppress the influence of the $\unicode[STIX]{x1D6FF}p_{\bot }$ and $\unicode[STIX]{x1D6FF}p_{\Vert }$ perturbations on the mode evolution. Without such pressure perturbations, the MRI reverts back to standard, MHD-like behaviour characteristic of the vertical-field MRI (this can be seen, for example, by artificially suppressing $\unicode[STIX]{x1D6FF}p_{\bot ,\Vert }$ perturbations in a calculation of the $B_{0y}\neq 0$ KMRI dispersion relation). Specifically, the growth rate approaches zero for $kv_{A}\lesssim \unicode[STIX]{x1D6FA}$ and peaks at smaller scales $kv_{A}\sim \unicode[STIX]{x1D6FA}$ . Thus, the long-wavelength linear modes are significantly stabilized (i.e. $\unicode[STIX]{x1D6FE}$ at low $k$ is small) and the mode moves to shorter wavelengths. Such behaviour is expected intuitively because the azimuthal pressure force, which is the cause of the enhanced low- $k$ linear growth rate (Reference Quataert, Dorland and HammettQ02; Balbus Reference Balbus2004), is limited by the mirror and firehose fluctuations. Because the standard MRI grows with the perturbed energies in approximate equipartition, $\unicode[STIX]{x1D6FF}B_{y}$ must ‘catch up’ to $\unicode[STIX]{x1D6FF}B_{x}$ , and both of these must catch up to the velocity perturbations (which grow linearly with $\unicode[STIX]{x1D6FF}u_{x}\sim \unicode[STIX]{x1D6FF}u_{y}\sim \unicode[STIX]{x1D6FD}_{0}^{1/2}\unicode[STIX]{x1D6FF}B_{y}$ ) during this phase of evolution (in other words, $\unicode[STIX]{x1D6FF}\boldsymbol{u}$ grows more slowly than $\unicode[STIX]{x1D6FF}\boldsymbol{B}$ ). This picture is confirmed by 1-D numerical calculations, with the growth of $\unicode[STIX]{x1D6FF}\boldsymbol{u}$ decreasing significantly as shorter wavelengths take over; see figure 3(a), Region 2. We also see smaller-scale perturbations growing on top of the longer-wavelength mode in figure 3(b) at $t\unicode[STIX]{x1D6FA}=12.5$ (e.g. around $z=0.2$ and $z=0.85$ ), particularly in those regions at the firehose limit where the MRI preferentially grows at smaller scales because $\unicode[STIX]{x0394}p<0$ . Note that the mode cannot be stabilized completely during this phase because the MRI growth rate on a background $\unicode[STIX]{x0394}p$ , though small, is non-zero as $k\rightarrow 0$ .

3. $\unicode[STIX]{x1D6FF}B_{y}>B_{0y}$ . As the amplitude of $\unicode[STIX]{x1D6FF}B$ grows larger than the background $B_{0y}$ field, the mode enters a second phase of nonlinear evolution. With the field-line direction dominated by the perturbation, the presence of a background $B_{0y}$ loses its dynamical importance and the mode behaves similarly to the vertical-field case, growing at $kv_{A}\sim \unicode[STIX]{x1D6FA}$ . In addition, because the magnitude of the magnetic field is now growing everywhere in space, $\unicode[STIX]{x1D6E5}$ becomes everywhere positive and will be limited only by the mirror instability; see figure 3(b) at $t=21~\unicode[STIX]{x03A9}^{-1}$ . As with the vertical-field MRI, when the perturbation amplitude dominates the total $B$ , the pressure anisotropy $\unicode[STIX]{x0394}p\approx (\unicode[STIX]{x1D6FF}B_{x}^{2}+\unicode[STIX]{x1D6FF}B_{y}^{2})/8\unicode[STIX]{x03C0}$ does not cause significant nonlinear modifications, because $\unicode[STIX]{x1D6FF}\boldsymbol{B}\boldsymbol{\cdot }\unicode[STIX]{x1D735}\unicode[STIX]{x1D6FF}\boldsymbol{B}=0$ for an MRI channel mode.

4. Compressibility effects. There is no 1-D mechanism to halt the growth of the mode until $\unicode[STIX]{x1D6FF}u$ approaches the sound speed ( $\unicode[STIX]{x1D6FF}B_{x}\sim \unicode[STIX]{x1D6FF}B_{y}\sim \unicode[STIX]{x1D6FD}^{1/2}B_{0}$ ). Thus, the mode behaves similarly to the vertical-field MRI, with large variations in $\unicode[STIX]{x1D70C}$ . The profiles that develop have the same characteristic shape as those seen in figure 2(d) (cf., figure 3 b at $t\unicode[STIX]{x1D6FA}=24$ ).

Each of the four stages discussed above can be seen in the mode energy evolution, shown in figure 3(a). In contrast to the calculation of the vertical-field MRI evolution (figure 2), we begin from random large-scale initial conditions at much higher $\unicode[STIX]{x1D6FD}_{0}=5000$ (with $B_{0y}=B_{0z}$ ), so as to clearly distinguish between the different regions of evolution and allow the smaller scale modes to grow after $\unicode[STIX]{x1D6E5}$ reaches the microinstability limits. While the details of the process described above will be modified depending on a variety of factors – e.g. the mode wavelength in comparison to the domain, the spectrum of the initial conditions, and the value of $B_{0y}/B_{0z}$ – the basic concepts and phases of evolution should be generally applicable. It is also worth noting that, at the large values of $\unicode[STIX]{x1D6FD}$ for which our arguments are most applicable, the mode will likely collapse into turbulence before the final nonlinear stage where compressibility is important (see § 4).

3.3.2 Weakly collisional (Braginskii) regime

As with the vertical-field MRI in the Braginskii regime (§ 3.2.2), there are two different Braginskii sub-regimes: (i) if $\overline{\unicode[STIX]{x1D708}}_{c}\equiv \unicode[STIX]{x1D708}_{c}/S\ll \unicode[STIX]{x1D6FD}^{1/2}$ , the instability grows at a similar rate to the collisionless instability (and the heat fluxes play an important dynamical role), or (ii) if $\overline{\unicode[STIX]{x1D708}}_{c}~\gg \unicode[STIX]{x1D6FD}^{1/2}$ , the growth rate of the MVI is reduced, reaching the collisional (standard MHD) regime when $\overline{\unicode[STIX]{x1D708}}_{c}\sim \unicode[STIX]{x1D6FD}$ (see figures 1–3 of Sharma et al. Reference Sharma, Hammett and Quataert2003). To understand this latter point – that the Braginskii MRI becomes MHD-like when $\overline{\unicode[STIX]{x1D708}}_{c}\gtrsim \unicode[STIX]{x1D6FD}$ – we compare the Lorentz force, $\boldsymbol{B}_{0}\boldsymbol{\cdot }\unicode[STIX]{x1D735}\unicode[STIX]{x1D6FF}\boldsymbol{B}=\unicode[STIX]{x1D735}\boldsymbol{\cdot }(\boldsymbol{B}_{0}\unicode[STIX]{x1D6FF}\boldsymbol{B})$ , to the pressure-anisotropy force $\unicode[STIX]{x1D735}\boldsymbol{\cdot }(\hat{\boldsymbol{b}}\hat{\boldsymbol{b}}\unicode[STIX]{x0394}p)$ that arises from the (linear) $\unicode[STIX]{x0394}p$ induced by the KMRI mode,

(3.7) $$\begin{eqnarray}\unicode[STIX]{x0394}p\sim \frac{p_{0}}{\unicode[STIX]{x1D708}_{c}}\frac{1}{B}\frac{\text{d}B}{\text{d}t}\sim \frac{p_{0}}{\unicode[STIX]{x1D708}_{c}}\frac{1}{B_{0}}\frac{\text{d}\unicode[STIX]{x1D6FF}B}{\text{d}t}\sim \frac{\unicode[STIX]{x1D6FD}}{\unicode[STIX]{x1D708}_{c}}\,\unicode[STIX]{x1D6FE}B_{0}\unicode[STIX]{x1D6FF}B(t),\end{eqnarray}$$

where $B_{0}^{2}=B_{0y}^{2}+B_{0z}^{2}$ and we have assumed $B_{0y}\sim B_{0z}$ . Note that we have neglected the heat fluxes in (3.7), which act to reduce $\unicode[STIX]{x0394}p$ (see (3.6)), as is appropriate for the high-collisionality regime (see § B.4). We see from (3.7) that the pressure-anisotropy stress is larger than the Lorentz force (and thus important for the mode’s evolution) only if $\overline{\unicode[STIX]{x1D708}}_{c}\lesssim \unicode[STIX]{x1D6FD}$ , as expected (Sharma et al. Reference Sharma, Hammett and Quataert2003).

Numerical experiments (not shown) have revealed that, in the moderate-collisionality regime $\overline{\unicode[STIX]{x1D708}}_{c}\equiv \unicode[STIX]{x1D708}_{c}/S\ll \unicode[STIX]{x1D6FD}^{1/2}$ , the Braginskii KMRI behaves similarly to a truly collisionless mode (this should be expected based on the arguments above and in § 3.2.2). As described in § 3.2.2, at very large amplitudes, $\unicode[STIX]{x1D6FF}B>B_{0}$ (Region 3), the evolution differs from a collisionless mode once $\unicode[STIX]{x1D6FF}B\gtrsim (\unicode[STIX]{x1D6FD}_{0}/\overline{\unicode[STIX]{x1D708}}_{c})^{1/2}B_{0}$ (the growing mode can no longer sustain $\unicode[STIX]{x0394}p$ at the mirror limit). In the high-collisionality regime, $\overline{\unicode[STIX]{x1D708}}_{c}\gtrsim \unicode[STIX]{x1D6FD}^{1/2}$ , the linear mode itself transitions back to the standard MHD MRI, and much of the discussion above loses its relevance. In particular, the most-unstable mode moves to larger scales as $\overline{\unicode[STIX]{x1D708}}_{c}$ increases (see figure 2b of Sharma et al. Reference Sharma, Hammett and Quataert2003). This implies that the sudden reduction in the scale of the mode when $\unicode[STIX]{x0394}p\sim B^{2}$ (see figure 3 b between $t\approx 12.5$ and $t\approx 21$ ) is much less relevant. The mode causes $\unicode[STIX]{x0394}p$ to reach the mirror and firehose limit at some amplitude $\unicode[STIX]{x1D6FF}B\lesssim B_{0}$ (with the exact point depending on $\overline{\unicode[STIX]{x1D708}}_{c}/\unicode[STIX]{x1D6FD}$ ) and then transition to the behaviour discussed in § 3.2.2 once $\unicode[STIX]{x1D6FF}B\gtrsim B_{0}$ .

3.4 General discussion of 1-D nonlinearities

With the diverse assortment of nonlinear effects outlined in the previous sections, it seems prudent to conclude with a discussion of some overarching ideas. As is generally the case in high- $\unicode[STIX]{x1D6FD}$ collisionless plasma dynamics (e.g. Schekochihin & Cowley Reference Schekochihin and Cowley2006; Squire et al. Reference Squire, Quataert and Schekochihin2016), nonlinearity can be important for perturbation amplitudes far below what one might naively expect. For the MRI in the collisionless regime, this occurs a factor of ${\sim}\unicode[STIX]{x1D6FD}_{0}$ (or ${\sim}\unicode[STIX]{x1D6FD}_{0}^{7/6}$ for $\unicode[STIX]{x1D6FF}B_{y}$ with $B_{0y}\neq 0$ ) below where nonlinear effects become important in standard MHD. However, we have also seen that, in all cases considered, the KMRI (or MVI) always reverts to MHD-like evolution at large amplitudes due to the anisotropy-limiting response of the mirror and firehose instabilities (e.g. Kunz et al. Reference Kunz, Schekochihin and Stone2014a ). This behaviour has also been seen in fully kinetic 2-D simulations (Riquelme et al. Reference Riquelme, Quataert, Sharma and Spitkovsky2012). More specifically, this arises because of the form of the pressure anisotropy, viz.  $\unicode[STIX]{x0394}p=B^{2}/8\unicode[STIX]{x03C0}$ , when it is limited at the mirror threshold. If $B$ is dominated by the mode itself ( $B^{2}\approx \unicode[STIX]{x1D6FF}B^{2}$ ), then the anisotropic stress in the momentum equation (2.2),

(3.8) $$\begin{eqnarray}\unicode[STIX]{x1D735}\boldsymbol{\cdot }(\unicode[STIX]{x0394}p\hat{\boldsymbol{b}}\hat{\boldsymbol{b}})=\frac{1}{8\unicode[STIX]{x03C0}}\unicode[STIX]{x1D735}\boldsymbol{\cdot }(B^{2}\hat{\boldsymbol{b}}\hat{\boldsymbol{b}})\approx \frac{1}{8\unicode[STIX]{x03C0}}\unicode[STIX]{x1D6FF}\boldsymbol{B}\boldsymbol{\cdot }\unicode[STIX]{x1D735}\unicode[STIX]{x1D6FF}\boldsymbol{B},\end{eqnarray}$$

acts like an additional Lorentz force, which is zero for the MRI channel mode (Goodman & Xu Reference Goodman and Xu1994). This implies that the pressure-anisotropy effects that are critical to the difference between the KMRI and the MRI in linear theory become unimportant once $\unicode[STIX]{x1D6FF}B\gtrsim B_{0}$ . Due to this, a large-amplitude collisionless KMRI channel mode is an approximate nonlinear solution (of the LF equations), as in MHD, until its amplitude approaches the sound speed (there is a minor complication in the Braginskii regime; see § 3.2.2). Thus, the effect of compressibility on the large-amplitude mode structure – if this occurs before breakdown into turbulence – looks nearly identical in the MHD and kinetic models, with either a Braginskii or LF closure, and with or without azimuthal fields (this structure is shown in figure 2 d). Very similar structures are also seen at large amplitudes in fully kinetic simulations (Kunz et al. Reference Kunz, Stone and Bai2014b ).

In contrast, the effect of the nonlinearity at intermediate amplitudes $\unicode[STIX]{x1D6FF}B\lesssim B_{0}$ differs between plasma regimes (collisionless and Braginskii) and background field configurations. For modes growing in a purely vertical background field, the nonlinear modification of the mode is modest, so long as the mirror fluctuations limit $\unicode[STIX]{x1D6E5}$ to be close to $1/\unicode[STIX]{x1D6FD}$ . However, even moderate overshoot past the mirror limit – for example, as might occur in numerical simulations due to insufficient scale separation between $\unicode[STIX]{x1D6FA}_{i}$ and $\unicode[STIX]{x1D6FA}$ , see § 6 – can cause quite strong modifications and/or cause the mode to move to longer wavelengths. Modes evolving in a mixed-vertical–azimuthal background field behave very differently, because the pressure perturbation participates directly in the linear instability (Reference Quataert, Dorland and HammettQ02). Upon reaching the mirror and firehose microinstability limits, the pressure perturbation can no longer contribute to the linear growth and the mode moves towards the smaller scales characteristic of the standard MRI once $\unicode[STIX]{x1D6FF}B_{y}\gtrsim \unicode[STIX]{x1D6FD}^{-2/3}B_{0}$ (or $\unicode[STIX]{x1D6FF}B_{x}\gtrsim \unicode[STIX]{x1D6FD}^{-1/3}B_{0}$ ). This transition is illustrated graphically in figure 3.

4.1 Linear parasitic-mode growth rates

In this section we directly calculate parasitic-mode growth rates for MRI and KMRI channel modes in a vertical background magnetic field. We do not consider a mixed-azimuthal–vertical background field configuration here primarily because the 1-D results of § 3.3 suggested that such modes are always relatively disordered when they reach large amplitudes anyway, due to their strong nonlinear disruption (from long wavelengths to short wavelengths) when $\unicode[STIX]{x1D6FF}B_{y}\sim B_{y}$ (see, e.g. figure 3 b). Thus the very idealized linear problem, based on purely sinusoidal background profiles, is presumably much less relevant for this case (we rectify this omission in the 3-D simulations below; see figure 6 b).

Motivated by previous MHD studies (Goodman & Xu Reference Goodman and Xu1994; Latter et al. Reference Latter, Lesaffre and Balbus2009, Reference Latter, Fromang and Gressel2010; Pessah & Goodman Reference Pessah and Goodman2009), we consider 3-D linear perturbations, $f(\boldsymbol{x})=f_{k_{x}k_{y}}(z)\exp (\text{i}k_{x}x+\text{i}k_{y}y)$ for $f=\{\boldsymbol{u}^{\prime },\,\boldsymbol{B}^{\prime },\,\unicode[STIX]{x1D70C}^{\prime },\,p_{\bot ,\Vert }^{\prime }\}$ , evolving on top of a channel-mode background ( $\unicode[STIX]{x1D6FF}\boldsymbol{u}$ and $\unicode[STIX]{x1D6FF}\boldsymbol{B}$ from (3.1), with $\unicode[STIX]{x1D6FF}B_{0}$ a free parameter). That is, we decompose the fields as

(4.1) $$\begin{eqnarray}\left.\begin{array}{@{}c@{}}\boldsymbol{u}=-Sx\hat{\boldsymbol{y}}-\sqrt{{\displaystyle \frac{3}{5}}}{\displaystyle \frac{\unicode[STIX]{x1D6FF}B_{0}}{\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}}}}\sin (kz)(\hat{\boldsymbol{x}}+\hat{\boldsymbol{y}})+\boldsymbol{u}^{\prime },\\ \boldsymbol{B}=B_{0}\hat{\boldsymbol{z}}-\unicode[STIX]{x1D6FF}B_{0}\cos (kz)(\hat{\boldsymbol{x}}-\hat{\boldsymbol{y}})+\boldsymbol{B}^{\prime },\\ \unicode[STIX]{x1D70C}=\unicode[STIX]{x1D70C}_{0}+0+\unicode[STIX]{x1D70C}^{\prime },\\ p_{\bot }=p_{0}+\unicode[STIX]{x1D6FF}p_{\bot 0}+p_{\bot }^{\prime },\\ p_{\Vert }=p_{0}+\unicode[STIX]{x1D6FF}p_{\Vert 0}+p_{\Vert }^{\prime },\end{array}\right\}\end{eqnarray}$$

with $k=2\unicode[STIX]{x03C0}/L_{z}$ , and linearize (2.1)–(2.7) in $\boldsymbol{u}^{\prime }$ , $\boldsymbol{B}^{\prime }$ , $\unicode[STIX]{x1D70C}^{\prime }$ and $p_{\bot ,\Vert }^{\prime }$ . (For simplicity, we ignore spatial variation in $\unicode[STIX]{x1D6FF}p_{\bot ,\Vert 0}$ ; see discussion below.) The resulting equations are solved numerically in a box with dimensionsFootnote ⁸ $(L_{x},L_{y},L_{z})=(4,4,1)$ , on a $16\times 16$ grid of Fourier modes in the homogeneous $x$ and $y$ directions, and with a pseudospectral method and $64$ modes in the inhomogeneous $z$ direction. Hyperviscous damping is used to remove energy just above the grid scale. We initialize with random noise in all variables, and evolve in time until $t=10\unicode[STIX]{x03A9}^{-1}$ (by which time the most-unstable parasitic eigenmode mostly dominates). Fitting an exponential to the energy evolution at later times yields the growth rate $\unicode[STIX]{x1D6FE}$ of the least-stable parasitic mode. Intuitively, a large parasitic-mode growth rate should be associated with rapid collapse of the channel mode into MRI turbulence, because the parasitic modes will quickly ‘overtake’ the mode itself, with their 3-D structure acting as a seed for the turbulence. Further, as the MRI mode grows (i.e. as $\unicode[STIX]{x1D6FF}B_{0}$ increases) the parasitic growth rates should increase, since there are stronger gradients of $\unicode[STIX]{x1D6FF}\boldsymbol{u}$ and $\unicode[STIX]{x1D6FF}\boldsymbol{B}$ to feed the instabilities.

To assess the impact of the pressure anisotropy, we apply a spatially constant background pressure anisotropy $\unicode[STIX]{x0394}p_{0}=\unicode[STIX]{x1D6FF}p_{\bot 0}-\unicode[STIX]{x1D6FF}p_{\Vert 0}$ in the KMHD models and calculate the resulting change in the maximum parasitic growth rate with $\unicode[STIX]{x0394}p_{0}$ . A strong variation in growth rate with $\unicode[STIX]{x0394}p_{0}$ would indicate that the saturation into turbulence is likely to depend sensitively on the self-generated pressure anisotropy, and thus differ strongly between collisional and collisionless plasmas. Of course, as discussed in § 3, there will be spatial variation in $\unicode[STIX]{x0394}p$ at large $\unicode[STIX]{x1D6FF}B_{0}$ , so the study here should be considered an approximation to the full problem, considering only the simplest effects. Similarly, we neglect the influence of the background shear on the parasitic modes (this is common in previous MHD analyses), because without this simplification the resulting time dependence of $k_{y}$ implies that an analysis in terms of eigenmodes is incorrect (one should consider transient, or non-modal, growth; Schmid Reference Schmid2007, Squire & Bhattacharjee Reference Squire and Bhattacharjee2014a ,Reference Squire and Bhattacharjee b ). This assumption is not truly valid except at very large mode amplitudes when $\unicode[STIX]{x1D6FF}\boldsymbol{u}$ dominates strongly over the mean shear, although we expect to capture the correct qualitative trends when the parasitic growth rate is larger than the shearing rate. As mentioned above, given that the pressure anisotropy appears to cause little change to growth rates, we deliberately keep this section brief, postponing to possible future work the detailed study of the mode structure and morphology (e.g. Kelvin–Helmholtz versus tearing-mode instability) or the variation of growth rates with $k_{x}$ and $k_{y}$ (Goodman & Xu Reference Goodman and Xu1994; Latter et al. Reference Latter, Lesaffre and Balbus2009; Prajapati & Chhajlani Reference Prajapati and Chhajlani2010).

Figure 4.

Maximum parasitic growth rates $\unicode[STIX]{x1D6FE}/\unicode[STIX]{x1D6FA}$ as a function of $\unicode[STIX]{x1D6E5}=(\unicode[STIX]{x1D6FF}p_{\bot 0}-\unicode[STIX]{x1D6FF}p_{\Vert 0})/p_{0}$ for $\unicode[STIX]{x1D6FD}_{0}\approx 90$ ( $B_{0z}/\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}_{0}}=0.15c_{s}$ ) for (a) $\unicode[STIX]{x1D6FF}B_{0}/\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}_{0}}=0.5c_{s}\approx 3.3B_{0z}$ , (b) $\unicode[STIX]{x1D6FF}B_{0}/\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}_{0}}=c_{s}\approx 6.7B_{0z}$ , (c) $\unicode[STIX]{x1D6FF}B_{0}/\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}_{0}}=2c_{s}\approx 13.3B_{0z}$ . Note that $\unicode[STIX]{x1D6E5}=0.1$ would correspond to a plasma fixed at the mirror limit in a constant background field $B_{0}\approx \sqrt{8\unicode[STIX]{x03C0}\unicode[STIX]{x0394}p_{0}}\approx 0.45c_{s}\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}_{0}}$ (but note that the channel-mode field varies sinusoidally). In each figure the yellow stars illustrate the growth rate in KMHD without heat fluxes (i.e. CGL, $q_{\bot }=q_{\Vert }=0$ ), while purple crosses illustrate KMHD growth rates including the simple model (2.12) for the heat fluxes. For comparison, the dashed blue line shows the incompressible MHD result and the dash-dotted red line shows the isothermal compressible MHD result (each at $\unicode[STIX]{x1D6E5}=0$ ). The dotted black line is the MRI channel-mode growth rate $\unicode[STIX]{x1D6FE}/\unicode[STIX]{x1D6FA}=3/4$ . Evidently, the variation of $\unicode[STIX]{x1D6FE}$ with $\unicode[STIX]{x1D6E5}$ is modest, and is probably too small to be of much consequence to MRI saturation.

Figure 5.

As in figure 4 but with a background field $\unicode[STIX]{x1D6FD}_{0}\approx 800$ ( $B_{0z}/\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}_{0}}=0.05c_{s}$ ). Although a growing MRI mode would have a shorter wavelength at this $B_{0z}$ , which will make the parasitic modes more unstable at a given amplitude due to the larger gradients, we choose to keep the same $k=2\unicode[STIX]{x03C0}/L_{z}$ as figure 4 to provide a direct comparison (recall also from § 3 that the mode wavelength can increase during evolution).

Figures 4 and 5 illustrate representative examples of $\unicode[STIX]{x1D6FE}$ as a function of $\unicode[STIX]{x1D6E5}=(\unicode[STIX]{x1D6FF}p_{\bot 0}-\unicode[STIX]{x1D6FF}p_{\Vert 0})/p_{0}$ and $\unicode[STIX]{x1D6FF}B_{0}$ . In each case the chosen mode energy is of order the thermal energy $\unicode[STIX]{x1D6FF}B_{0}/\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}_{0}}\sim c_{s}$ and is larger than the background $B_{0z}$ field. Because of this large $\unicode[STIX]{x1D6FF}B_{0}$ , the parasitic growth rates are mostly larger than the MRI-mode growth rate (dotted line), as required for a parasite to cause the channel mode to break up into turbulence. The maximum of $\unicode[STIX]{x1D6E5}$ plotted ( $\unicode[STIX]{x1D6E5}=0.1$ ) corresponds to a plasma that is everywhere at the mirror limit in a constant field of $B_{0}\approx \sqrt{8\unicode[STIX]{x03C0}\unicode[STIX]{x0394}p_{0}}\approx 0.45c_{s}\sqrt{4\unicode[STIX]{x03C0}\unicode[STIX]{x1D70C}_{0}}$ , which is larger than the background $B_{0z}$ in each case (but smaller than the maximum $\unicode[STIX]{x1D6FF}B_{0}$ studied). The first feature that is evident in figures 4 and 5 is the suppression in parasitic-mode growth rates in the kinetic models (solid lines) and compressible fluids (red dash-dotted line), in comparison to incompressible fluids (blue dashed line). This property was also noted for compressible MHD in Latter et al. (Reference Latter, Lesaffre and Balbus2009).Footnote ⁹ Aside from this, we see that the differences between the kinetic models (both with and without heat fluxes) and MHD are relatively modest.Footnote ¹⁰ While there is there is a slight tendency for $\unicode[STIX]{x1D6FE}$ to decrease with $\unicode[STIX]{x0394}p$ at large mode amplitudes, changes in $\unicode[STIX]{x1D6FE}$ of this magnitude are unlikely to make any notable differences in a nonlinear simulation. Furthermore, there does not appear to be any significant change in behaviour at even higher $\unicode[STIX]{x1D6FF}B_{0}$ (not shown), which leads us to conclude that parasitic modes are broadly unaffected by the kinetic effects contained within the CGL and LF models.

Obviously, the results shown in figures 4 and 5 cover only a small portion of parameter space in a rather idealized setting. In addition to the results shown, we have calculated growth rates across a much wider parameter space in $B_{0z}$ , $p_{0}$ , $\unicode[STIX]{x1D6FF}B_{0}$ , $\unicode[STIX]{x1D6E5}$ , $k$ (the channel mode wavelength), small-scale dissipation coefficients (hyper-viscosity, hyper-resistivity and their ratio) and box dimensions. In addition, we have varied the ratio of $\unicode[STIX]{x1D6FF}\boldsymbol{u}$ and $\unicode[STIX]{x1D6FF}\boldsymbol{B}$ away from that of the fastest-growing channel mode (i.e. differently from (3.1)), as might be caused, for example, by the effects of the self-generated pressure anisotropy on the mode. Finally, we have also considered parasitic-mode evolution on more angular compressible profiles, similar to those shown in figure 2(d) (Latter et al. Reference Latter, Lesaffre and Balbus2009). In all cases, we have failed to find any significant difference between standard compressible MHD and the CGL or LF models, and so we refrain from presenting these results in any detail here. Of course, these studies have all assumed a spatially constant $\unicode[STIX]{x1D6E5}$ and $\unicode[STIX]{x1D70C}_{0}$ profile, which will certainly change results quantitatively in some regimes. It is also possible that there are modes in other regimes (e.g. much longer or shorter wavelength than the KMRI mode), that have not been captured by these studies. Nevertheless, we feel that the general conclusion that the parasitic modes are mostly insensitive to background pressure anisotropy should be robust, given the wide range of parameter space for which this conclusion appears to hold.

4.2 Nonlinear simulation

Our second method for probing parasitic-mode behaviour is to simply observe the evolution of a nonlinear KMRI channel mode in three dimensions. The maximum amplitude that such a mode reaches before breaking up into turbulence should give a simple indication of the effectiveness of the parasitic modes. We use the modified version of the Zeus code described in Reference Sharma, Hammett, Quataert and StoneS06, which solves (2.1)–(2.5) with the LF closure (2.6)–(2.7) and pressure-anisotropy limiters.

This method is complementary to that described in the previous section: although it cannot provide detailed information on individual modes or variation with parameters, it is free from some of the caveats of the linear parasitic-mode study (for example, the assumption of spatially homogeneous background density profiles). It also allows us to consider the mixed-azimuthal–vertical field KMRI in a moderately realistic settling (as mentioned above, the stronger effects of 1-D nonlinearities in this case suggest that an idealized parasitic-mode study is not very worthwhile for the azimuthal-field KMRI). Most importantly, 3-D simulations directly address the issue we most care about: is the nonlinear saturation significantly different between the kinetic and MHD models? In Reference Sharma, Hammett, Quataert and StoneS06 the authors noted that there was a significant difference, with MRI modes in kinetic models growing to significantly larger amplitudes before being disrupted, even though the turbulence itself maintained a similar level of angular-momentum transport. While this may appear to be at odds with our findings from the previous section, here we argue that this difference is primarily a consequence of the 1-D effects described in § 3. Specifically, the positive pressure anisotropy can increase the wavelength of the mode well before it reaches saturation amplitudes. This effect was caused by the choice of $\unicode[STIX]{x1D6E5}\approx 7/\unicode[STIX]{x1D6FD}$ for the mirror instability limit in Reference Sharma, Hammett, Quataert and StoneS06, which allows the anisotropies to have a strong dynamical effect before the mirror limit is enforced. For a given mode amplitude, these longer-wavelength modes are attacked more slowly by the parasites, due to the smaller gradients of $\unicode[STIX]{x1D6FF}\boldsymbol{u}$ and $\unicode[STIX]{x1D6FF}\boldsymbol{B}$ (Goodman & Xu Reference Goodman and Xu1994), thus leading to a larger transient amplitude before the transition into turbulence.

Our studies have deliberately used a set-up that is similar to Reference Sharma, Hammett, Quataert and StoneS06. We initialize with random noise in all variables and a background magnetic field with $\unicode[STIX]{x1D6FD}_{0}=400$ in a box of dimension $(L_{x},L_{y},L_{z})=(1,2\unicode[STIX]{x03C0},1)$ . We take $k_{L}\approx 14$ , which corresponds to capturing Landau damping correctly ( $k_{\Vert }\approx k_{L}$ ) for low-amplitude modes with a wavelength of approximately half of the size of the box, and limit the positive pressure anisotropy at $p_{\bot }/p_{\Vert }-1<\unicode[STIX]{x1D709}_{\text{Mir}}/\unicode[STIX]{x1D6FD}_{\bot }$ (this is $\unicode[STIX]{x1D6E5}<\unicode[STIX]{x1D709}_{\text{Mir}}/\unicode[STIX]{x1D6FD}$ for $\unicode[STIX]{x0394}p\ll p_{0}$ ). With either a purely vertical background field, or a mixed-azimuthal–vertical background field ( $B_{0y}=B_{0z}$ ), we compare the mode saturation between MHD, the LF model with $\unicode[STIX]{x1D709}_{\text{Mir}}=7$ , and the LF model with $\unicode[STIX]{x1D709}_{\text{Mir}}=1$ . The vertical-field LF model runs are identical to runs Zl4 and Zl5 of Reference Sharma, Hammett, Quataert and StoneS06.

Figure 6.

Energy of the MRI perturbation, $E_{\text{MRI}}=\int \text{d}z\,(\unicode[STIX]{x1D70C}\,\unicode[STIX]{x1D6FF}u^{2}/2+\unicode[STIX]{x1D6FF}B^{2}/8\unicode[STIX]{x03C0})$ , as a function of time for a set of 3-D Zeus simulations at $\unicode[STIX]{x1D6FD}_{0}=400$ . We compare the evolution of the LF model (2.1)–(2.7) with mirror limiter $\unicode[STIX]{x1D6E5}=7/\unicode[STIX]{x1D6FD}$ as used in Reference Sharma, Hammett, Quataert and StoneS06 (blue solid lines), the LF model with mirror limiter $\unicode[STIX]{x1D6E5}=1/\unicode[STIX]{x1D6FD}$ (red dashed lines) and standard MHD (black dotted lines). The insets show the vertical mode structure ( $\unicode[STIX]{x1D6FF}B_{x}$ , blue; $\unicode[STIX]{x1D6FF}B_{y}$ , red) at the times indicated by the circles. Panel (a) shows the case with a purely vertical background magnetic field ( $B_{0y}=0$ ). This illustrates how an artificially high mirror limit ( $\unicode[STIX]{x1D6E5}=7/\unicode[STIX]{x1D6FD}$ ; blue solid line) causes the mode to move to longer wavelengths after it reaches the mirror limit at $t\approx 17$ , which subsequently causes the mode to reach a very large amplitude before saturation. Panel (b) shows simulations with an azimuthal background magnetic field ( $B_{0y}=B_{0z}$ ; the dotted line shows the energy of $B_{0y}$ ); in this case, all three modes saturate into turbulence at similar amplitudes. Given the relatively disordered mode structure in the kinetic runs (the insets compare the late-time structures of all three cases, as labelled), this behaviour is consistent with the idea that there are not major differences between the parasitic modes’ properties in the kinetic (LF) model and MHD (see text for further discussion). Note that the time scale of the MHD case in panel (b) has been shifted to the left, so that all three modes reach saturation amplitudes at a similar time (the linear growth of the KMRI mode is faster, see figure 1).

Our findings are illustrated in figure 6, which plots the modes’ energy evolution in both LF cases and standard MHD, with a purely vertical field (left-hand panel a) and with a mixed-azimuthal–vertical field (right-hand panel b). The key result of this figure is the larger ( ${\sim}$ factor $10$ ) overshoot of the vertical-field KMRI mode (panel a) with $\unicode[STIX]{x1D709}_{\text{Mir}}=7$ (compared to MHD), which disappears at $\unicode[STIX]{x1D709}_{\text{Mir}}=1$ (i.e. there is effectively no difference between MHD and the LF model with the $\unicode[STIX]{x1D709}_{\text{Mir}}=1$ mirror limiter). As mentioned above, this leads us to attribute the differences between MHD and the LF model saturation to the difference in the large-amplitude wavelength of the MRI modes. Specifically, the strength of the vertical magnetic field for $\unicode[STIX]{x1D6FD}_{0}=400$ is such that modes with $k_{z}=4\unicode[STIX]{x03C0}/L_{z}$ dominate during the linear phase, but, with the artificially high mirror boundary $\unicode[STIX]{x1D709}_{\text{Mir}}=7$ , $\unicode[STIX]{x1D6E5}$ becomes large enough to cause the KMRI mode to increase in scale to the largest in the box by later times (see insets). This does not occur with the standard mirror limit $\unicode[STIX]{x1D709}_{\text{Mir}}=1$ . While not unexpected, these results do show that there are not inherent differences in the parasitic modes’ properties between the kinetic (LF) model and MHD for the vertical-field MRI. Examination of mode evolution at a variety of other values for $\unicode[STIX]{x1D6FD}_{0}$ and $\unicode[STIX]{x1D709}_{\text{Mir}}$ (not shown) has produced results that are generally consistent with this idea.

In figure 6(b), showing a mixed-azimuthal–vertical background field configuration, we see that the saturation amplitudes of all three cases (the MHD model, and the $\unicode[STIX]{x1D709}_{\text{Mir}}=1$ and $\unicode[STIX]{x1D709}_{\text{Mir}}=7$ LF models) are similar. This seems to be because even at large amplitudes, the KMRI modes are relatively disordered and each have both $k=2\unicode[STIX]{x03C0}/L_{z}$ and $k=4\unicode[STIX]{x03C0}/L_{z}$ components, while the MHD mode is nearly a pure $k=4\unicode[STIX]{x03C0}/L_{z}$ mode. This more disordered KMRI state is expected based on the 1-D analysis of § 3.3: the mode is strongly disrupted as $\unicode[STIX]{x1D6FF}B_{y}$ surpasses $B_{0y}$ , and has not had time to ‘pick out’ the fastest-growing mode (see also figure 3 b). Thus although the MHD mode might be more easily attacked by the parasitic modes (given its smaller scale), the more disordered KMRI modes are further from being nonlinear solutions, and thus more easily evolve into turbulence. The net result is that they all saturate at approximately the same amplitude. As further evidence for this scenario, we see that the $k=2\unicode[STIX]{x03C0}/L_{z}$ component of the $\unicode[STIX]{x1D709}_{\text{Mir}}=7$ mode is larger than that of the $\unicode[STIX]{x1D709}_{\text{Mir}}=1$ mode (as expected because $\unicode[STIX]{x0394}p$ is larger, increasing the effective magnetic tension), explaining its slightly higher saturation amplitude. Thus, these mixed-azimuthal–vertical field KMRI results also suggest that there is little difference between the parasitic-mode properties in the kinetic (LF) model and MHD. Again, we have examined mode evolution at various other values for $\unicode[STIX]{x1D6FD}_{0}$ and $\unicode[STIX]{x1D709}_{\text{Mir}}$ (not shown) and seen similar results; however, to truly study this case in detail would require much higher resolution simulations (so as to allow higher $\unicode[STIX]{x1D6FD}_{0}$ ; see figure 3), which are beyond the scope of this work.

Overall, we see that all of our calculations – both of linear parasitic-mode growth rates in idealized settings and 3-D studies using the full nonlinear LF model – are consistent with the idea that parasitic modes are not strongly affected by the kinetic effects contained within the fluid models considered in this work. This seems to be the case for both the vertical-field KMRI and the mixed-azimuthal–vertical field KMRI (although we did not study the parasitic modes directly for the mixed-field case). An obvious caveat of this conclusion is that we have considered only the LF model in this work, and future studies with fully kinetic methods (in particular, those that can correctly capture plasma microinstability saturation) are needed to shed light on whether our conclusions also hold for truly collisionless plasmas.

6.1 Pressure-anisotropy overshoot due to finite scale separation

First, in order for the mirror instability to effectively regulate the positive pressure anisotropy during the growth of KMRI, the growth of the mirrors must deplete the anisotropy faster than it is being adiabatically replenished by the KMRI. This requires $\unicode[STIX]{x1D6FE}_{m}/\unicode[STIX]{x1D6FE}_{\text{kmri}}>1$ , where $\unicode[STIX]{x1D6FE}_{m}$ and $\unicode[STIX]{x1D6FE}_{\text{kmri}}$ are the growth rates of the mirror instability and KMRI, respectively. The maximum growth rate of the mirror instability is given by $\unicode[STIX]{x1D6FE}_{m}\sim \unicode[STIX]{x1D6FA}_{i}\unicode[STIX]{x1D6EC}_{m}^{2}$ , where $\unicode[STIX]{x1D6EC}_{m}\doteq \unicode[STIX]{x1D6E5}-1/\unicode[STIX]{x1D6FD}_{\bot }$ is positive when the plasma is mirror unstable (Hellinger Reference Hellinger2007). Thus, we require $\unicode[STIX]{x1D6EC}_{m}>(\unicode[STIX]{x1D6FE}_{\text{kmri}}/\unicode[STIX]{x1D6FA}_{i})^{1/2}$ for the mirror instability to outpace the KMRI-driven production of positive pressure anisotropy. For the vertical-field case, $\unicode[STIX]{x1D6FE}_{\text{kmri}}=S/2$ at maximum growth, and so we require $\unicode[STIX]{x1D6EC}_{m}>(S/2\unicode[STIX]{x1D6FA}_{i})^{1/2}$ .Footnote ¹¹ When there is an azimuthal magnetic field present, $\unicode[STIX]{x1D6FE}_{\text{kmri}}\approx (2S\unicode[STIX]{x1D6FA})^{1/2}$ at maximum growth, and so we require $\unicode[STIX]{x1D6EC}_{m}>(S/\unicode[STIX]{x1D6FA}_{i})^{1/2}\,(2\unicode[STIX]{x1D6FA}/S)^{1/4}\approx (S/\unicode[STIX]{x1D6FA}_{i})^{1/2}$ . Of course, in this case we must also contend with the firehose instability in regions where $\unicode[STIX]{x1D6E5}\propto \unicode[STIX]{x1D6FF}B_{y}<0$ (see (3.6)), for which the instability criterion is $\unicode[STIX]{x1D6EC}_{f}\doteq \unicode[STIX]{x1D6E5}+2/\unicode[STIX]{x1D6FD}_{\Vert }<0$ . With $\unicode[STIX]{x1D6FE}_{f}\sim \unicode[STIX]{x1D6FA}_{i}|\unicode[STIX]{x1D6EC}_{f}|^{1/2}$ as the growth rate for the fastest-growing oblique firehose (Yoon et al. Reference Yoon, Wu and de Assis1993; Hellinger & Matsumoto Reference Hellinger and Matsumoto2000), we require $|\unicode[STIX]{x1D6EC}_{f}|>(S/\unicode[STIX]{x1D6FA}_{i})^{2}\,(2\unicode[STIX]{x1D6FA}/S)\simeq (S/\unicode[STIX]{x1D6FA}_{i})^{2}$ for the firehose instability to outpace the KMRI-driven production of negative pressure anisotropy. The parallel-propagating firehose has $\unicode[STIX]{x1D6FE}_{f}=\unicode[STIX]{x1D6FA}_{i}|\unicode[STIX]{x1D6EC}_{f}|$ as its maximum growth rate (e.g. Davidson & Völk Reference Davidson and Völk1968; Rosin et al. Reference Rosin, Schekochihin, Rincon and Cowley2011), and thus grows slower than its oblique counterpart for $|\unicode[STIX]{x1D6EC}_{f}|\lesssim 1$ .

We now determine whether these criteria place prohibitive constraints on kinetic simulations. For the vertical-field KMRI, $\unicode[STIX]{x1D6E5}\sim (\unicode[STIX]{x1D6FF}B/B_{0})^{2}$ (see (3.2)), and so the mirror instability will grow fast enough to deplete the pressure anisotropy $\unicode[STIX]{x1D6EC}_{m}\rightarrow 0^{+}$ when

(6.1) $$\begin{eqnarray}\left(\frac{\unicode[STIX]{x1D6FF}B}{B_{0}}\right)^{2}\gtrsim \frac{1}{\unicode[STIX]{x1D6FD}_{0}}+\left(\frac{S}{\unicode[STIX]{x1D6FA}_{i}}\right)^{\!1/2},\end{eqnarray}$$

beyond which the plasma is kept marginally mirror stable (and the results of this paper then follow). The asymptotic limit $(S/\unicode[STIX]{x1D6FA}_{i})\unicode[STIX]{x1D6FD}_{0}^{2}\rightarrow 0$ was taken throughout this paper to obtain $(\unicode[STIX]{x1D6FF}B/B_{0})^{2}\sim 1/\unicode[STIX]{x1D6FD}_{0}$ at the mirror instability threshold. The additional factor of $(S/\unicode[STIX]{x1D6FA}_{i})^{1/2}$ due to overshoot beyond this threshold may be quite appreciable in a contemporary kinetic simulation of the MRI, perhaps ${\sim}0.1$ (e.g. Kunz et al. Reference Kunz, Stone and Quataert2016) or even more (e.g. Riquelme et al. Reference Riquelme, Quataert, Sharma and Spitkovsky2012; Hoshino Reference Hoshino2015), and thus might be comparable to, if not larger than, $1/\unicode[STIX]{x1D6FD}_{0}$ . The situation will, of course, improve as the amplification of the magnetic-field strength by the KMRI increases $\unicode[STIX]{x1D6FA}_{i}$ and decreases $\unicode[STIX]{x1D6FD}$ . Thus, in the final, turbulent saturated state, the effect of finite scale separation will presumably be less severe than during the early, weakly nonlinear phases that have been the focus of this work; nonetheless, one should at least be aware of the impact of insufficient scale separation on the early phase of the KMRI.

In a mixed-azimuthal–vertical guide field, the KMRI-driven pressure anisotropy is linear in the mode amplitude (see (3.6)). Because, in this case, it is the pressure anisotropy which provides the azimuthal torque to transport angular momentum and drive the instability (rather than the magnetic tension), it matters all the more how efficiently the pressure anisotropy is regulated. If the lack of scale separation allows the pressure anisotropy to grow much beyond the mirror threshold, the instability’s behaviour once $\unicode[STIX]{x1D6FF}B_{y}\gtrsim \unicode[STIX]{x1D6FD}_{0}^{-2/3}B_{0y}$ may be completely different. Let us be quantitative, assuming $B_{0y}\approx B_{0z}$ and that $\unicode[STIX]{x1D6FD}_{0}$ is sufficiently high ( $\unicode[STIX]{x1D6FD}_{0z}\gtrsim 10^{3}$ at least) that the scalings derived in appendix A hold. Then, the maximum growth rate of the azimuthal KMRI, $\unicode[STIX]{x1D6FE}\approx (2S\unicode[STIX]{x03A9})^{1/2}$ , occurs at wavenumbers satisfying $|k|v_{Az}/\unicode[STIX]{x1D6FA}\approx 2\unicode[STIX]{x1D6FD}_{0}^{-1/6}$ (see (A 2)), and the driven pressure anisotropy (3.6) is

(6.2) $$\begin{eqnarray}\unicode[STIX]{x1D6E5}\approx \sqrt{\frac{\unicode[STIX]{x03C0}S}{\unicode[STIX]{x1D6FA}}}\unicode[STIX]{x1D6FD}_{0}^{-1/3}\frac{\unicode[STIX]{x1D6FF}B_{y}(t)}{B_{0}}\left(\frac{2\unicode[STIX]{x1D6FD}_{0}^{-1/6}\unicode[STIX]{x1D6FA}}{v_{Az}|k|}\right),\end{eqnarray}$$

where the final term in parentheses is order unity. Thus, the mirror instability will grow fast enough to deplete the excess positive pressure anisotropy when

(6.3) $$\begin{eqnarray}\left(\frac{\unicode[STIX]{x1D6FF}B_{y}}{B_{0}}\right)^{2}\gtrsim \frac{\unicode[STIX]{x1D6FA}}{\unicode[STIX]{x03C0}S}\left(\frac{1}{\unicode[STIX]{x1D6FD}_{0}^{2/3}}+\frac{S^{1/2}\unicode[STIX]{x1D6FD}_{0}^{1/3}}{\unicode[STIX]{x1D6FA}_{i}^{1/2}}\right)^{2},\end{eqnarray}$$

which may be readily compared to (6.1). The asymptotic limit $(S/\unicode[STIX]{x1D6FA}_{i})\unicode[STIX]{x1D6FD}_{0}^{2}\rightarrow 0$ was taken throughout this paper to obtain $\unicode[STIX]{x1D6FF}B_{y}/B_{0}\sim \unicode[STIX]{x1D6FD}_{0}^{-2/3}$ at the mirror instability threshold. The additional factor of $(S/\unicode[STIX]{x1D6FA}_{i})^{1/2}\unicode[STIX]{x1D6FD}_{0}^{1/3}$ is due to the necessary overshoot beyond this threshold, which, again, may not be all that small in a contemporary kinetic simulation. For the firehose, the negative pressure anisotropy will be efficiently depleted when

(6.4) $$\begin{eqnarray}\left(\frac{\unicode[STIX]{x1D6FF}B_{y}}{B_{0}}\right)^{2}\gtrsim \frac{4\unicode[STIX]{x1D6FA}}{\unicode[STIX]{x03C0}S}\left(\frac{1}{\unicode[STIX]{x1D6FD}_{0}^{2/3}}+\frac{S^{2}\unicode[STIX]{x1D6FD}_{0}^{1/3}}{2\unicode[STIX]{x1D6FA}_{i}^{2}}\right)^{2},\end{eqnarray}$$

which will occur after the mirror criterion (6.3) is satisfied because of its more forgiving threshold (as long as $(S/\unicode[STIX]{x1D6FA}_{i})^{1/2}$ is small compared to $1/\unicode[STIX]{x1D6FD}_{0}$ ).

6.2 The impact of pressure-anisotropy overshoot on the KMRI

One notable impact of these pressure-anisotropy overshoots is on the fastest-growing KMRI-mode wavelength. For the vertical-field case, this wavelength will increase due to the nonlinear pressure anisotropy by an amount ${\approx}(3/2+\unicode[STIX]{x1D6FD}\unicode[STIX]{x1D6EC}_{m}/2)^{1/2}$ . With $\unicode[STIX]{x1D6EC}_{m}\gtrsim (S/\unicode[STIX]{x1D6FA}_{i})^{1/2}$ required for the mirrors to outpace the production of anisotropy, this could easily be a factor of several increase unless adequate scale separation is used. For example, having $\unicode[STIX]{x1D6FD}=400$ and $S/\unicode[STIX]{x1D6FA}_{i}=0.01$ would result in a pressure-anisotropy-driven increase in the KMRI wavelength by a factor of ${\approx}5$ . In a computational box with vertical extent $L_{z}\equiv c_{s}/\unicode[STIX]{x1D6FA}$ , this means that a maximally growing mode with $kv_{A}\simeq \unicode[STIX]{x1D6FA}$ and $\unicode[STIX]{x1D6FE}\simeq S/2$ would shift from having $\unicode[STIX]{x1D706}/L_{z}\approx 2\unicode[STIX]{x03C0}(2/\unicode[STIX]{x1D6FD})^{1/2}\approx 0.4$ to $\unicode[STIX]{x1D706}/L_{z}\approx 2$ , bigger than the box. The mode’s wavelength would, of course, stop increasing once $\unicode[STIX]{x1D706}/L_{z}=1$ . But if, at that point, $\unicode[STIX]{x1D6EC}_{m}\geqslant (S/\unicode[STIX]{x1D6FA})/2\unicode[STIX]{x03C0}^{2}-3/\unicode[STIX]{x1D6FD}$ , then all the KMRI modes in the box would be stabilized by the effectively increased magnetic tension. Since $\unicode[STIX]{x1D6EC}_{m}$ must grow to ${\sim}(S/\unicode[STIX]{x1D6FA}_{i})^{1/2}$ before the mirrors can efficiently relax the pressure anisotropy and thereby remove some of this excess tension, we find that values of $S/\unicode[STIX]{x1D6FA}_{i}\geqslant [(S/\unicode[STIX]{x1D6FA})/2\unicode[STIX]{x03C0}^{2}-3/\unicode[STIX]{x1D6FD}]^{2}$ will ultimately stabilize the KMRI.Footnote ¹² It is, however, likely that this stabilization would be transient: even if the KMRI stops growing, the mirrors will continue relaxing $\unicode[STIX]{x0394}p$ (albeit rather slowly), and at some point $\unicode[STIX]{x0394}p$ would be sufficiently low so as to render the KMRI unstable again. Finally, we note that if the box does continue to support unstable KMRI modes on the largest scales $\unicode[STIX]{x1D706}/L_{z}=1$ , one must ensure that the horizontal extent of the box is large enough to fit the parasitic modes (§ 4.1).

In the azimuthal–vertical-field case, the fastest-growing mode occurs on scales satisfying $kv_{Az}/\unicode[STIX]{x1D6FA}\sim \unicode[STIX]{x1D6FD}_{0}^{-1/6}$ , or $\unicode[STIX]{x1D706}/L_{z}\sim \unicode[STIX]{x1D6FD}_{0}^{-1/3}$ . These scales are larger than those of the standard MRI and the vertical-field KMRI. We have predicted that, as the mirror and firehose instabilities kick in and regulate the pressure anisotropy, the influence of the $\unicode[STIX]{x1D6FF}p_{\bot }$ and $\unicode[STIX]{x1D6FF}p_{\Vert }$ perturbations on the mode evolution is suppressed and the KMRI reverts back to its standard, MHD-like behaviour. This involves a suppression of long-wavelength MRI modes (i.e. $\unicode[STIX]{x1D6FE}_{\text{kmri}}$ decreases for $kv_{A}\lesssim 1$ ) and a transition phase in the nonlinear evolution (‘Region 2’ in figure 3 a), in which the mode becomes more MHD-like at smaller scales with the kinetic and magnetic energies in approximate equipartition. If the mirror regularization is especially sluggish due to inadequate scale separation, this phase might be skipped altogether and a $\unicode[STIX]{x1D706}/L_{z}=1$ mode will take the place of what is instead seen in figure 3(b). It is also worth noting that the large value of $\unicode[STIX]{x1D6FD}_{0}=5000$ used in § 3.3 to accentuate the different regions of evolution would require an especially small value of $S/\unicode[STIX]{x1D6FA}_{i}$ in a kinetic simulation.

6.3 The microphysics of the firehose and mirror instabilities

A further constraint on the choice of $S/\unicode[STIX]{x1D6FA}_{i}$ concerns the means by which mirror/firehose instabilities regulate the pressure anisotropy. In order for these instabilities to efficiently keep the anisotropy near the instability thresholds via the anomalous pitch-angle scattering of particles, the scattering rate must be ${\sim}S\unicode[STIX]{x1D6FD}$ , and this number must be smaller than $\unicode[STIX]{x1D6FA}_{i}$ .

In the case of the firehose instability, when $S/\unicode[STIX]{x1D6FA}_{i}\ll 1/\unicode[STIX]{x1D6FD}$ the firehose fluctuations saturate at a mean level $\langle |\unicode[STIX]{x1D6FF}\boldsymbol{B}/B|^{2}\rangle \sim (\unicode[STIX]{x1D6FD}S/\unicode[STIX]{x1D6FA}_{i})^{1/2}$ in a time ${\sim}[\unicode[STIX]{x1D6FD}/(S\unicode[STIX]{x1D6FA}_{i})]^{1/2}\ll S^{-1}\sim \unicode[STIX]{x1D6FE}_{\text{kmri}}^{-1}$ (Kunz et al. Reference Kunz, Schekochihin and Stone2014a ; Melville et al. Reference Melville, Schekochihin and Kunz2016). This is achieved via pitch-angle scattering of the particles off Larmor-scale firehose fluctuations, which precludes the adiabatic production of pressure anisotropy. In this limit, since local shear in a macroscopic plasma flow will change in time at the rate comparable to the shear itself, one can safely consider the anomalous collisionality associated with the firehose fluctuations to turn on instantaneously, in line with the macroscopic modelling assumption used in this paper. At sufficiently high $\unicode[STIX]{x1D6FD}$ and/or $S$ such that $\unicode[STIX]{x1D6FD}\gtrsim \unicode[STIX]{x1D6FA}_{i}/S$ , however, this is no longer true and the firehose fluctuations saturate at an order-unity level independent of either $\unicode[STIX]{x1D6FD}$ or $S$ , after growing secularly without scattering particles for one shear time (Melville et al. Reference Melville, Schekochihin and Kunz2016). Thus, for kinetic simulations of MRI turbulence to reliably demonstrate the anomalous-scattering model of pressure-anisotropy regulation used in this work and others (e.g. Sharma et al. Reference Sharma, Hammett, Quataert and Stone2006; Mogavero & Schekochihin Reference Mogavero and Schekochihin2014; Santos-Lima et al. Reference Santos-Lima, de Gouveia Dal Pino, Kowal, Falceta-Gonçalves, Lazarian and Nakwacki2014; Chandra et al. Reference Chandra, Gammie, Foucart and Quataert2015; Foucart et al. Reference Foucart, Chandra, Gammie and Quataert2015), parameters must be chosen such that $S/\unicode[STIX]{x1D6FA}_{i}<1/\unicode[STIX]{x1D6FD}$ , preferably by a decade or more. Again, satisfying this inequality becomes easier as the KMRI grows the magnetic-field strength. But, for the early phases of evolution, this cautions against setting $\unicode[STIX]{x1D6FD}_{0}$ too high, because this will impose stiff constraints on an acceptable value of $S/\unicode[STIX]{x1D6FA}_{i0}$ .

In the arguably more relevant case of the mirror instability, when $S/\unicode[STIX]{x1D6FA}_{i}\ll 1/\unicode[STIX]{x1D6FD}$ the mirror fluctuations saturate at a mean level $\langle (\unicode[STIX]{x1D6FF}B/B)^{2}\rangle \sim 1$ in a time ${\sim}S^{-1}\sim \unicode[STIX]{x1D6FE}_{\text{kmri}}^{-1}$ (Kunz et al. Reference Kunz, Schekochihin and Stone2014a ; Riquelme et al. Reference Riquelme, Quataert and Verscharen2015; Melville et al. Reference Melville, Schekochihin and Kunz2016). While marginal stability and mirror saturation is ultimately achieved via pitch-angle scattering of the particles off Larmor-scale bends at the ends of the magnetic mirrors, there is a long ( ${\sim}S^{-1}$ ) phase in which the pressure anisotropy is held marginal without appreciable particle scattering. This is achieved by corralling an ever increasing number of particles into the deepening magnetic wells, in which these particles become trapped, approximately conserve their $\unicode[STIX]{x1D707}$ as they bounce to and fro, and perceive no average change in $B$ (and thus no generation of net pressure anisotropy) along their bounce orbits. The increase in the large-scale $B$ is offset by the decrease in the intra-mirror $B$ . During this phase of evolution, the mirror fluctuations grow at the rate required to offset the production of pressure anisotropy by the KMRI-driven growth in the large-scale magnetic-field strength. A few things must be satisfied for kinetic simulations of KMRI growth to produce results similar to those predicted in this paper. First, the hard-wall limiter on the pressure anisotropy that we (and others) use must be an adequate (if not complete) representation of the otherwise more complicated mirror-driven regulation. This is particularly true during the $\unicode[STIX]{x1D707}$ -conserving phase of the mirror instability: does it matter to the large (i.e. KMRI) scales that an ever-increasing population of trapped particles are ignorant of the KMRI-driven magnetic-field growth during this phase? If not, then fine; simply limit the pressure anisotropy at the mirror instability using an enhanced collisionality, nothing more sophisticated being necessary. But, if so, then an effort must be made in the kinetic simulation to ensure that its results, if different from those predicted in this paper, are truly asymptotic. Namely, since the $\unicode[STIX]{x1D707}$ -conserving phase of the mirror instability lasts just one shear time, whereas the KMRI growth phase typically lasts several shear times, there must be enough scale separation so that the mirrors can saturate before $\unicode[STIX]{x1D6FF}B/B_{0}$ of the KMRI enters into the nonlinear phases we predicted in § 3. Secondly, do the Larmor-scale mirror distortions in the magnetic-field direction greatly affect the efficacy of the heat flow? An answer in the affirmative is suggested by Komarov et al. (Reference Komarov, Churazov, Kunz and Schekochihin2016), Riquelme et al. (Reference Riquelme, Quataert and Verscharen2016), Riquelme et al. (Reference Riquelme, Quataert and Verscharen2017). But, if the effect of these distortions is simply a reduction in the magnitude of the heat flow, then the footnote in § 2.1 applies: our results are not strongly affected. The reason is that, by the time the mirror instability is triggered, the heat flows have already spatially smoothed the pressure anisotropy on the scale of the KMRI mode, fulfilling their main role in influencing the mode evolution.

6.4 Finite-Larmor-radius effects

There is additional physics that enters when $S/\unicode[STIX]{x1D6FA}_{i}$ is not sufficiently small, which might complicate the evolution of the KMRI beyond that envisaged herein. First, gyroviscous effects become important when $\unicode[STIX]{x1D6FD}\gtrsim 4\unicode[STIX]{x1D6FA}_{i}/\unicode[STIX]{x1D6FA}$ (Ferraro Reference Ferraro2007; Heinemann & Quataert Reference Heinemann and Quataert2014). For such $\unicode[STIX]{x1D6FD}$ , the polarity of the mean magnetic field influences the stability and MRI growth rates. Without a good scale separation between $\unicode[STIX]{x1D6FA}$ and $\unicode[STIX]{x1D6FA}_{i}$ , finite-Larmor-radius effects might therefore artificially modify the KMRI, even at modest $\unicode[STIX]{x1D6FD}$ . Secondly, note that an equilibrium particle distribution function in a strongly magnetized differentially rotating disc can be quite different than an equilibrium distribution function in an unmagnetized disc. In the latter, a tidal anisotropy of the in-plane thermal motions of the particles is enforced by epicyclic motion in the rotational supported plasma (see § 3.1 of Heinemann & Quataert Reference Heinemann and Quataert2014); this effect goes away in a strongly magnetized plasma, where gyrotropy of the distribution function about the magnetic field is enforced. This is important because, if the initial magnetic field is inclined with respect to the rotation axis (i.e. $b_{y}\neq 0$ , $b_{z}\neq 1$ ) and $S/\unicode[STIX]{x1D6FA}_{i}$ is not sufficiently small, this tidal anisotropy can function as a field-biased pressure anisotropy and potentially drive mirror fluctuations in the equilibrium state. To wit, the equilibrium field-biased pressure anisotropy is $\unicode[STIX]{x1D6E5}\approx (3/2)(S/\unicode[STIX]{x1D6FA}_{i})(b_{y}^{2}-1/3)/b_{z}$ to leading order in $S/\unicode[STIX]{x1D6FA}_{i}$ when $b_{z}\neq 0$ . A disc with $b_{y}=b_{z}=1/\sqrt{2}$ would be mirror unstable from the tidal anisotropy alone if $S/\unicode[STIX]{x1D6FA}_{i}\gtrsim 2\sqrt{2}\unicode[STIX]{x1D6FD}^{-1}$ . (A plasma with, say, $\unicode[STIX]{x1D6FD}_{0}=400$ and $S/\unicode[STIX]{x1D6FA}_{i}=0.01$ would thus be mirror unstable, even without the KMRI-driven pressure anisotropy.) If the background field is exactly azimuthal, then the field-biased pressure anisotropy $\unicode[STIX]{x1D6E5}=S/(2\unicode[STIX]{x1D6FA})>0$ , and any large- $\unicode[STIX]{x1D6FD}$ plasma would be trivially mirror unstable, no matter how strongly the plasma is magnetized.

6.5 The saturated state

Finally, one must be cognizant of the physical constraints and computational demands not only during the early stages of the KMRI, but also in the saturated state. In going, say, from $\unicode[STIX]{x1D6FD}_{0}\approx 10^{3}$ to $\unicode[STIX]{x1D6FD}\approx 4$ , as often seen in a typical magnetorotationally turbulent saturated state (e.g. Pessah, Chan & Psaltis Reference Pessah, Chan and Psaltis2006), the ion Larmor radius might shrink by a factor between ${\approx}4$ (if $\unicode[STIX]{x1D707}$ is somehow conserved during this process) and ${\approx}16$ (if $\unicode[STIX]{x1D707}$ is not). Increased scale separation is, of course, a good thing, but only to a point. If $\unicode[STIX]{x1D70C}_{i}$ decreases so much that it falls under the numerical grid, then the anomalous particle scattering from ion-Larmor-scale magnetic structures that plays a regulatory role for the pressure anisotropy will be attenuated, fundamentally changing the physics of the mirror and firehose instabilities.