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Notes on Mixing Length Theory

These notes are mostly inspired from reading Cox & Giuli (“Principles of stellar structure”); some insights are from A.Maeder (“Physics, formation and evolution of rotating stars”) and Kippenhahn & Weigert (“Stellar Structure and Evolution”)

In hydrostatic equilibrium we can define the total pressure scale height, \({H_{\mathrm{P}}}\), as \[-\frac{{{\mathrm d}}\ln {\mathrm{P}}}{{{\mathrm d}}r} \equiv \frac{1}{{H_{\mathrm{P}}}} = \frac{\rho g}{{\mathrm{P}}}\] where \({\mathrm{P}}\) is the total pressure (\({\mathrm{P}}_{gas} + {\mathrm{P}}_{rad}\)). The pressure scale height is a measure of the distance over which the pressure changes by an appreciable fraction of itself.

We can define the gradients \(\nabla \equiv \frac{{{\mathrm d}}\ln {T}}{{{\mathrm d}}\ln {\mathrm{P}}}\) and \(\nabla' \equiv \frac{{{\mathrm d}}\ln {T}'}{{{\mathrm d}}\ln {\mathrm{P}}}\). Here \(\nabla\) represents the average temperature gradient with respect to pressure of all matter at a given level, while \(\nabla'\) is the temperature gradient with respect to pressure of a rising/falling fluid element. At first order the temperature excess of such fluid elements can therefore be written as \[\Delta {T}(\Delta r) = {T}'(r + \Delta r) - {T}(r + \delta r) \simeq \Delta r \bigg[ \frac{{{\mathrm d}}{T}'}{{{\mathrm d}}r}-\frac{{{\mathrm d}}{T}}{{{\mathrm d}}r}\bigg].\] Assuming \({T}' \simeq {T}\), i.e. the temperature is not changing drastically within the distance \(\Delta r\), one can write \[\Delta {T}(\Delta r) = \Delta r \, {T}\bigg[ -\frac{{{\mathrm d}}\ln {T}}{{{\mathrm d}}r}- \bigg(-\frac{{{\mathrm d}}\ln {T}'}{{{\mathrm d}}r}\bigg)\bigg],\] and using the assumption of pressure equilibrium, the definitions of pressure scale height \({H_{\mathrm{P}}}\) and the gradients \(\nabla\) and \(\nabla'\) we obtain \[\label{eq:deltat} \Delta {T}(\Delta r) = - \frac{{{\mathrm d}}\ln {\mathrm{P}}}{{{\mathrm d}}r} \Delta r \, {T}\bigg[ \frac{{{\mathrm d}}\ln {T}}{{{\mathrm d}}\ln {\mathrm{P}}}- \bigg(\frac{{{\mathrm d}}\ln {T}'}{{{\mathrm d}}\ln {\mathrm{P}}}\bigg)\bigg] = \Delta r \frac{{T}}{{H_{\mathrm{P}}}}\, (\nabla - \nabla').\] Note that in general the value of \(\nabla'\) depends on the rate at which the moving fluid element is exchanging heat with its surroundings. However in the deep interiors of a star a good approximation is \(\nabla' = {\nabla_{\mathrm{\!ad}}}\equiv \big(\frac{{{\mathrm d}}\ln {T}}{{{\mathrm d}}\ln {\mathrm{P}}}\big)_{\textrm{ad}}\), where \({\nabla_{\mathrm{\!ad}}}\) is the temperature gradient of a fluid element moving adiabatically.

Since a non-zero temperature gradient always implies a radiative flux, in a convective region part of the energy is still going to be transported by radiation. This flux can be written as \[\label{eq:radtransfer} F_{r} = -\frac{4ac}{3}\frac{T^3}{\kappa \rho}\frac{{{\mathrm d}}\ln T}{{{\mathrm d}}\ln {\mathrm{P}}} = \frac{4ac}{3}\frac{T^4}{\kappa \rho}\frac{\nabla}{{H_{\mathrm{P}}}}.\] Finally the fictitious (but computable) radiative gradient can be defined as the gradient of temperature required by radiation to carry the total stellar flux: \[\label{eq:totalflux} F = F_{c} + F_{r} \equiv \frac{4ac}{3}\frac{T^4}{\kappa \rho}\frac{\nabla_r}{{H_{\mathrm{P}}}}.\]

In a stellar convection zone where no energy is produced by nuclear reactions, the following inequalities are satisfied: \(\nabla_r > \nabla > \nabla' > {\nabla_{\mathrm{\!ad}}}\)

In the “Mixing Length Theory” of convection it is assumed that an element of fluid rises in pressure equilibrium and retains its identity while it moves through a radial distance \(\Delta r\), after which it mixes with its surroundings, releasing its excess heat energy. The distance \(\Delta r\) is called mixing length and is usually denoted as \(\lambda\). The heat transferred by upward moving elements can then be quantified as: \[F_{c} = \frac{1}{2} \rho \bar{v}\, {c_{\mathrm{P}}}\, \lambda \bigg[ \frac{{{\mathrm d}}{T}'}{{{\mathrm d}}r}-\frac{{{\mathrm d}}{T}}{{{\mathrm d}}r}\bigg] ,\] where the factor 1/2 comes from the fact that at each level approximately one-half of the matter is rising and one-half is descending. Here \(\rho\), \(\bar{v}\) and \({c_{\mathrm{P}}}\) are averages along the distance \(\lambda\) of density, velocity and specific heat at constant pressure of upward and downward moving fluid elements. Using equation \ref{eq:deltat} we can write \[\label{eq:convectiveflux} F_{c} = \frac{1}{2} \rho \bar{v}\, {c_{\mathrm{P}}}\, T \frac{\lambda}{{H_{\mathrm{P}}}} ( \nabla - \nabla') ,\]

We can calculate the accelaration of a convective fluid element \[\ddot{r} = - g - \frac{1}{\rho} \frac{\partial {\mathrm{P}}}{\partial r},\] which expanded at first order around the equilibrium state leads to an estimate of the total net force (buoyant minus gravitation) \(f=-g \Delta \rho\). Along the distance \(\Delta r\) a convective fluid element experience the force \(f(\Delta r) = - g \Delta \rho (\Delta r)\). Here the variation of \(g\) with height is considered negligible. The work done per unit volume over the distance \(\Delta r\) is therefore \[W (\Delta r) = \int_{0}^{\Delta r} f(x) {{\mathrm d}}x = - g \int_{0}^{\Delta r} \Delta \rho (x) {{\mathrm d}}x = - \frac{1}{2} g \Delta \rho (\Delta r) \Delta r.\] An average of \(W(\Delta r)\) over all possible values of \(\Delta r\) and a choice of a numerical factor (1/4) in exchanging \(\Delta r\) with \(\lambda\) leads to the following expression (\(W\) depends quadratically on \(\Delta r\)): \[\overline{W} (\lambda) = \frac{1}{4} W(\lambda) = - \frac{1}{8} g \Delta \rho (\lambda) \lambda.\] Under the assumption of no dissipative forces, no transfer of kinetic energy to surrounding matter and no heat loss, then one would conclude \(\bar{W}(\lambda) = \bar{1/2\rho v^2}\). However in the MLT one assumes that only half of this work is transformed into kinetic energy. This leads to \[\overline{\frac{1}{2}\rho v^2} \simeq \frac{1}{2}\rho \bar{v}^2 = \frac{1}{2}\overline{W} (\lambda) = - \frac{1}{16} g \Delta \rho (\lambda) \lambda,\] so that the velocity of convective elements at the level where the mixing length is \(\lambda\) can be expressed as \[\label{eq:velocity2} \bar{v}^2 = - \frac{1}{8} g (\Delta \rho (\lambda)/\rho) \lambda.\] Relating \(\Delta \rho\) and \(\Delta T\) requires the equation of state for the gas \(\rho = \rho (\mu, T, {\mathrm{P}})\), which in differential form can be written as \[{{\mathrm d}}\rho = \bigg(\frac{\partial \rho}{\partial \mu} \bigg)_{{\mathrm{P}},T} {{\mathrm d}}\mu + \bigg(\frac{\partial \rho}{\partial T} \bigg)_{{\mathrm{P}},\mu} {{\mathrm d}}T + \bigg(\frac{\partial \rho}{\partial {\mathrm{P}}} \bigg)_{\mu,T} {{\mathrm d}}{\mathrm{P}},\] , \[{{\mathrm d}}\rho = \frac{\rho}{\mu}\bigg(\frac{\partial \ln \rho}{\partial \ln \mu} \bigg)_{{\mathrm{P}},T} {{\mathrm d}}\mu + \frac{\rho}{T} \bigg(\frac{\partial \ln \rho}{\partial \ln T} \bigg)_{{\mathrm{P}},\mu} {{\mathrm d}}T + \frac{\rho}{{\mathrm{P}}} \bigg(\frac{\partial \ln \rho}{\partial \ln {\mathrm

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