While geostrophic motion occurs when the horizontal components of the Coriolis and the pressure gradient forces are in approximate balance,^{[1]} quasigeostrophic motion refers to nearly geostrophic flows where the advective derivative terms in the momentum equation are an order of magnitude smaller than the Coriolis and the pressure gradient forces.^{[2]}
Derivation
In Cartesian coordinates, the components of the geostrophic wind are

{f_o} {v_g} = {\partial \Phi \over \partial x} (1a)

{f_o} {u_g} =  {\partial \Phi \over \partial y} (1b)
where {\Phi} is the geopotential height.
The geostrophic vorticity

{\zeta_g} = {\hat{k} \cdot \nabla \times \overrightarrow{V_g}}
can therefore be expressed in terms of the geopotential as

{\zeta_g} = ) = {1 \over f_o}{\nabla^2 \Phi}} (2)
Equation (2) can be used to find {\zeta_g (x,y)} from a known field {\Phi (x,y)}. Alternatively, it can also be used to determine {\Phi} from a known distribution of {\zeta_g} by inverting the Laplacian operator.
The quasigeostrophic vorticity equation can be obtained from the {x} and {y} components of the quasigeostrophic momentum equation which can then be derived from the horizontal momentum equation

{D\overrightarrow{V} \over Dt} + f \hat{k} \times \overrightarrow{V} =  \nabla \Phi (3)
The material derivative in (3) is defined by

} (4)

where {\omega = {Dp \over Dt}} is the pressure change following the motion.
The horizontal velocity {\overrightarrow{V}} can be separated into a geostrophic {\overrightarrow{V_g}} and an ageostrophic {\overrightarrow{V_a}} part

{\overrightarrow{V} = \overrightarrow{V_g} + \overrightarrow{V_a}} (5)
Two important assumptions of the quasigeostrophic approximation are


1. {\overrightarrow{V_g} >> \overrightarrow{V_a} } More precisely ~O(Rossby number).

2. {f = f_o + \beta y} “betaplane approximation” with {f_o >> \beta y}
The second assumption justifies letting the Coriolis parameter have a constant value {f_o} in the geostrophic approximation and approximating its variation in the Coriolis force term by {f_o + \beta y}.^{[3]} However, because the acceleration following the motion, which is given in (1) as the difference between the Coriolis force and the pressure gradient force, depends on the departure of the actual wind from the geostrophic wind, it is not permissible to simply replace the velocity by its geostrophic velocity in the Coriolis term.^{[3]} The acceleration in (3) can then be rewritten as

{f \hat{k} \times \overrightarrow{V} + \nabla \Phi} = {(f_o + \beta y)\hat{k} \times (\overrightarrow{V_g} + \overrightarrow{V_a})  f_o \hat{k} \times \overrightarrow{V_g}} = {f_o \hat{k} \times \overrightarrow{V_a} + \beta y \hat{k} \times \overrightarrow{V_g} } (6)
The approximate horizontal momentum equation thus has the form

{D_g \overrightarrow{V_g} \over Dt} = {f_o \hat{k} \times \overrightarrow{V_a}  \beta y \hat{k} \times \overrightarrow{V_g}} (7)
Expressing equation (7) in terms of its components,

, and noting that geostrophic wind is nondivergent (ie, {\nabla \cdot \overrightarrow{V} = 0}), the vorticity equation is

)  \beta v_g } (9)
Because {f} depends only on {y} (ie, } (10)
Defining the geopotential tendency {\chi = {\partial \Phi \over \partial t}} and noting that partial differentiation may be reversed, equation (10) can be rewritten in terms of {\chi} as

} (11)
The righthand side of equation (11) depends on variables {\chi} and {\omega}. An analogous equation dependent on these two variables can be derived from the thermodynamic energy equation

)({\partial \Phi \over \partial p})}\sigma \omega}={kJ \over p}} (12)
where {\sigma = {R T_o \over p}{d ln \Theta_o \over dp}} and {\Theta_o} is the potential temperature corresponding to the basic state temperature. In the midtroposphere, {\Theta_o} ≈ {2.5 \times 10^{6} m{^2}Pa^{2}s^{2}}.
Multiplying (12) by {f_o \over \sigma} and differentiating with respect to {p} and using the definition of {\chi}yields

)}=)} (13)
If for simplicity {J} were set to 0, eliminating {\omega} in equations (11) and (13) yields ^{[4]}

)}}){\chi}}=+f})} (14)
Equation (14) is often referred to as the geopotential tendency equation. It relates the local geopotential tendency (term A) to the vorticity advection distribution (term B) and thickness advection (term C).
Using the chain rule of differentiation, term C can be written as

{)}} (15)
But based on the thermal wind relation,

={\hat{k} \times \nabla ({\partial \Phi \over \partial p})}}.
In other words,{\partial \overrightarrow{V_g} \over \partial p} is perpendicular to {\nabla ({\partial \Phi \over \partial p})} and the second term in equation (15) disappears. The first term can be combined with term B in equation (14) which, upon division by {f_o} can be expressed in the form of a conservation equation ^{[5]}

)q}={D_g q \over Dt}=0} (16)
where {q} is the quasigeostrophic potential vorticity defined by

{q = (+{f}+)}})} (17)
The three terms of equation (17) are, from left to right, the geostrophic relative vorticity, the planetary vorticity and the stretching vorticity.
Implications
As an air parcel moves about in the atmosphere, its relative, planetary and stretching vorticities may change but equation (17) shows that the sum of the three must be conserved following the geostrophic motion.
Equation (17) can be used to find {q} from a known field {\Phi}. Alternatively, it can also be used to predict the evolution of the geopotential field given an initial distribution of {\Phi} and suitable boundary conditions by using an inversion process.
More importantly, the quasigeostrophic system reduces the fivevariable primitive equations to a oneequation system where all variables such as {u_g}, {v_g} and {T} can be obtained from {q} or height {\Phi}.
Also, because {\zeta_g} and {\overrightarrow{V_g}} are both defined in terms of {\Phi(x,y,p,t)}, the vorticity equation can be used to diagnose vertical motion provided that the fields of both {\Phi} and {\partial \Phi \over \partial t} are known.
References

^ Phillips, N.A. (1963). “Geostrophic Motion.” Reviews of Geophysics Volume 1, No. 2., p. 123.

^ Kundu, P.K. and Cohen, I.M. (2008). Fluid Mechanics, 4th edition. Elsevier., p. 658.

^ ^{a} ^{b} Holton, J.R. (2004). Introduction to Dynamic Meteorology, 4th Edition. Elsevier., p. 149.

^ Holton, J.R. (2004). Introduction to Dynamic Meteorology, 4th Edition. Elsevier., p. 157.

^ Holton, J.R. (2004). Introduction to Dynamic Meteorology, 4th Edition. Elsevier., p. 160.
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