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Reynolds-averaged Navier-Stokes equations allow to split the description of a turbulent fluid into an averaged (typically laminar) flow on some length and/or time-scale and separate equations for the turbulent fluctuations. The resulting equations look like this $$\rho\bar{u}_j \frac{\partial \bar{u}_i }{\partial x_j} = \rho \bar{f}_i + \frac{\partial}{\partial x_j} \left[ - \bar{p}\delta_{ij} + \mu \left( \frac{\partial \bar{u}_i}{\partial x_j} + \frac{\partial \bar{u}_j}{\partial x_i} \right) - \rho \overline{u_i^\prime u_j^\prime} \right ]$$ Here the bars denotes the averaged values, and $\rho \overline{u_i^\prime u_j^\prime}$ is called the Reynolds stress tensor characterizing the influence of the turbulent fluctuations on the mean flow.

To actually evaluate the Reynolds stress one usually passes to something called the Boussinesque hypothesis and that is that you can actually model the stress as a viscous stress tensor with a "turbulent viscosity" $\mu_t$ and an isotropic stress coming from "turbulent kinetic energy" $k$. That is, in Cartesian coordinates $$\rho \overline{u_i^\prime u_j^\prime} = \mu_t \left( \frac{\partial \bar{u}_i}{\partial x_j} + \frac{\partial \bar{u}_j}{\partial x_i} \right) -\frac{2}{3} k \delta_{ij}$$ Then there is a number of models for how to compute the quantities $\mu_t$ and $k$. Just for illustration, one of them is the k-epsilon model, where two transport equations for variables $k,\epsilon$ are solved $$\frac{\partial (\rho k)}{\partial t}+ \frac {\partial (\rho k \bar{u}_i)}{\partial x_i}= f(k, \epsilon, \bar{u}_j, \partial \bar{u}_j/\partial x_k,...)$$ $$\frac{\partial (\rho \epsilon)}{\partial t}+ \frac {\partial (\rho \epsilon \bar{u}_i)}{\partial x_i}= g(k, \epsilon, \bar{u}_j, \partial \bar{u}_j/\partial x_k,...)$$ and turbulent viscosity is then determined as $\mu_t = \mu_t(k,\epsilon)$. Many other models exist.

Of course, in astrophysics we are talking about plasma dynamics, which is modeled by (radiative) compressible magneto-hydrodynamics. However, this set of equations can be Reynolds-averaged in very much the same way as the pure-fluid equations. The equations of models such as the k-epsilon model would have to be generalized by introducing the production of turbulent kinetic energy due to effects such as the magneto-rotational instability but otherwise the models should work in a similar fashion. Possibly, one would also have to include a model for the turbulent magnetic-field fluctuations in the Maxwell stress $\sim \overline{B_i B_j}$.


So now for my question: These Reynolds averaged models seem to have applications only in engineering, but I have never seen them applied in an astrophysical context. Why is this so?

I have instead seen a single, very special model, and that is the Shakura-Sunyaev prescription for turbulent viscosity in steady, thin accretion disks: $\mu_t = \alpha \rho \bar{p}$, where $\alpha$ is a constant. However, I do not see any other context than steady, thin disks where this kind of prescription can be useful. Does one perhaps use more sophisticated prescriptions in other astrophysical contexts such as the theory of stellar structure, intergalactic medium, or the solar wind?

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  • $\begingroup$ Typically, astrophysical fluids are significantly affected by magnetohydrodynamic (MHD) terms, since almost everything is a plasma. As such, I can't imagine that even an advanced pure-fluid model that doesn't include MHD terms would be particularly useful (but I'm also not an expert). $\endgroup$ – probably_someone Jan 16 '18 at 17:22
  • $\begingroup$ @probably_someone I could think of some cases (e.g., early universe simulations, GR), but I think "most guys doing astrophysical fluids use MHD" is an acceptable assumption. $\endgroup$ – Kyle Kanos Jan 16 '18 at 17:28
  • $\begingroup$ @probably_someone It is true that compressible MHD would require generalizations of these models, I have added a comment about this to the post. However, I do not see this as a reason why the Reynolds-averaging models should not be applied to astrophysics at all. The alpha prescription kind of does this, it actually includes transport both due to turbulent fluctuations and large-scale Maxwell stress. $\endgroup$ – Void Jan 16 '18 at 18:04
  • $\begingroup$ Thinking about this a little more, there aren't any astrophysical situations that I can think of where a time-averaged value would be useful--not to say there won't be any, just that I can't think of any. I've always seen that the interest is in the dynamical evolution of the physical object (SNR, galaxy, etc). $\endgroup$ – Kyle Kanos Jan 16 '18 at 18:13
  • $\begingroup$ @KyleKanos Maybe in stellar structure? But there are already pretty sophisticated custom models for that anyway. $\endgroup$ – probably_someone Jan 16 '18 at 18:59
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Closure models might not be popular in astrophysics but they certainly have been tried for a while. In the context of accretion disks, several people have tried more sophisticated closures compared to the Shakura-Sunyaev prescription, see for example:

http://adsabs.harvard.edu/abs/1995PASJ...47..629K

http://adsabs.harvard.edu/abs/2003MNRAS.340..969O

Stellar convection is another case where closure models have been used: https://arxiv.org/abs/1401.5176

Some of these models do not incorporate the "dynamo" closure - that is the (turbulent) terms responsible for generation and sustenance of magnetic fields. For one such attempt that tries to incorporate alpha-Omega dynamo closure for accretion disks, see this:

https://academic.oup.com/mnras/article/195/4/881/1746346

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