METEO 300
Fundamentals of Atmospheric Science

10.4 Equations of Motion in Spherical Coordinates

The three variables used in spherical coordinates are:

  • longitude (denoted by λ)
  • latitude (denoted by φ)
  • vertical distance (denoted by r from Earth’s center, by z from Earth’s surface, since z = r-a, where a is Earth’s radius)
circle showing Conversion between spherical and Cartesian coordinates as described in the text
Conversion between spherical and Cartesian coordinates.
Credit: W. Brune

Note that the unit vectors in spherical coordinates change with position. For example, for an air parcel at the equator, the meridional unit vector, j , is parallel to the Earth’s rotation axis, whereas for an air parcel near one of the poles, j is nearly perpendicular to the Earth’s rotation axis. In spherical coordinates, the velocity vector and its components are given by:

U =u i +v j +w k u=rcosϕ Dλ Dt ,v=r Dϕ Dt ,w= Dz Dt

[10.17]

where u, v, and w are the eastward, northward, and upward components of the velocity, respectively. Changes in eastward, northward, and upward distances are given by:

dx=rcosϕdλ=change in eastward distanceacosϕdλ dy=rdϕ=change in northward distanceadϕ dz=dr=change in upward distance

Let’s now write the momentum conservation equation [10.17] in component form in spherical coordinates. We will just show you how this conversion is done without actually taking you through all the steps. Note that we need to take the total derivatives of the unit vectors as well as the velocities:

D U Dt = D Dt ( i u+ j v+ k w )= i Du Dt +u D i Dt + j Dv Dt +v D j Dt + k Dw Dt +w D k Dt

[10.18]

The terms containing derivatives of the unit vectors are called “metric terms.” They depend on the Earth being a sphere. In Cartesian coordinates, they equal zero.

Consider just one of these metric terms:

D j Dt = j t +u j x +v j y +w j z =0+u j x +v j y +0

Since for any location, j is constant with time and j does not change as a function of altitude, that leaves j MathType@MTEF@5@5@+=faaagCart1ev2aqaKnaaaaWenf2ys9wBH5garuavP1wzZbItLDhis9wBH5garmWu51MyVXgaruWqVvNCPvMCG4uz3bqee0evGueE0jxyaibaieYlf9irVeeu0dXdh9vqqj=hHeeu0xXdbba9frFj0=OqFfea0dXdd9vqaq=JfrVkFHe9pgea0dXdar=Jb9hs0dXdbPYxe9vr0=vr0=vqpi0dc9GqpWqaaeaabiGaciaacaqabeaadaqaaqaaaOqaamaaFiaabaGaamOAaaGaay51Gaaaaa@356E@ dependent only on latitude and longitude.

Look at j y first. Set y = 0 at the equator, and y = a (Earth’s radius) near the pole. As noted above, at the equator, j is parallel to Earth’s rotation axis, but near the pole, it is almost perpendicular to it. Thus the change in j going from south to north (increasing y) must be pointing down to Earth’s center and so j changes by k times a small angular change while y changes by a times the same small angular change. The net result is that:

j y = k a

Using the same approach, we can show that:

j x = tanϕ a i

The total derivatives of all three unit vectors are:

D i Dt = u acosϕ ( j sinϕ k cosϕ ) D j Dt = utanϕ a i v a k D k Dt = u a i + v a j

[10.19]

Putting this all together:

D U Dt =( Du Dt uvtanϕ a + uw a ) i + ( Dv Dt + u 2 tanϕ a + uw a ) j + ( Dw Dt u 2 + v 2 a ) k

[10.20]

Similar analysis can be done for the other terms in the Equations of Motion.

Coriolis force:

2Ω×V=2Ω( vsinϕwcosϕ ) i 2Ωusinϕ j +2Ωucosϕ k

[10.21]

Gravity:

g =g k

[10.22]

Pressure Gradient Force (PGF):

1 ρ p= 1 ρ p x i 1 ρ p y j 1 ρ p z k

[10.23]

Friction:

C d h | V | V = C d h | V |u i C d h | V |v j

[10.24]
Adding together all of the forces, the momentum equation in spherical coordinates are:

Du Dt uvtanϕ a + uw a = 1 ρ p x +2Ωvsinϕ2Ωwcosϕ C d h | V |u Dv Dt u 2 tanϕ a + vw a = 1 ρ p y 2Ωusinϕ C d h | V |v Dw Dt u 2 + v 2 a = 1 ρ p z g+2Ωucosϕ