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Potential temperature

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Potential temperature

The potential temperature of a parcel of fluid at pressure P is the temperature that the parcel would acquire if adiabatically brought to a standard reference pressure P_{0}, usually 1000 millibars. The potential temperature is denoted \theta and, for air, is often given by

\theta = T \left(\frac{P_0}{P}\right)^{R/c_p},

where T is the current absolute temperature (in K) of the parcel, R is the gas constant of air, and c_p is the specific heat capacity at a constant pressure. R/c_p = 0.286 for air (meteorology).


  • Contexts 1
  • Comments 2
  • Potential temperature perturbations 3
  • Derivation 4
  • Related quantities 5
  • References 6
  • Bibliography 7
  • External links 8
  • See also 9


The concept of potential temperature applies to any stratified fluid. It is most frequently used in the atmospheric sciences and oceanography.[1] The reason that it is used in both fluids is that changes in pressure result in warmer fluid residing under colder fluid- examples being the fact that air temperature drops as one climbs a mountain and water temperature can increase with depth in very deep ocean trenches and within the ocean mixed layer. When potential temperature is used instead, these apparently unstable conditions vanish.


Potential temperature is a more dynamically important quantity than the actual temperature. This is because it is not affected by the physical lifting or sinking associated with flow over obstacles or large-scale atmospheric turbulence. A parcel of air moving over a small mountain will expand and cool as it ascends the slope, then compress and warm as it descends on the other side- but the potential temperature will not change in the absence of heating, cooling, evaporation, or condensation (processes that exclude these effects are referred to as dry adiabatic). Since parcels with the same potential temperature can be exchanged without work or heating being required, lines of constant potential temperature are natural flow pathways.

Under almost all circumstances, potential temperature increases upwards in the atmosphere, unlike actual temperature which may increase or decrease. Potential temperature is conserved for all dry adiabatic processes, and as such is an important quantity in the planetary boundary layer (which is often very close to being dry adiabatic).

Potential temperature is a useful measure of the static stability of the unsaturated atmosphere. Under normal, stably stratified conditions, the potential temperature increases with height,

\frac{\partial \theta}{\partial z} > 0

and vertical motions are suppressed. If the potential temperature decreases with height,

\frac{\partial \theta}{\partial z} < 0

the atmosphere is unstable to vertical motions, and convection is likely. Since convection acts to quickly mix the atmosphere and return to a stably stratified state, observations of decreasing potential temperature with height are uncommon, except while vigorous convection is underway or during periods of strong insolation. Situations in which the equivalent potential temperature decreases with height, indicating instability in saturated air, are much more common.

Since potential temperature is conserved under adiabatic or isentropic air motions, in steady, adiabatic flow lines or surfaces of constant potential temperature act as streamlines or flow surfaces, respectively. This fact is used in isentropic analysis, a form of synoptic analysis which allows visualization of air motions and in particular analysis of large-scale vertical motion.[2][3]

Potential temperature perturbations

The atmospheric boundary layer (ABL) potential temperature perturbation is defined as the difference between the potential temperature of the ABL and the potential temperature of the free atmosphere above the ABL. This value is called the potential temperature deficit in the case of a katabatic flow, because the surface will always be colder than the free atmosphere and the PT perturbation will be negative.


The enthalpy form of the first law of thermodynamics can be written as:

dh = T \, ds + v \, dp,

where dh denotes the enthalpy change, T the temperature, ds the change in entropy, v the specific volume, and p the pressure.

For adiabatic processes, the change in entropy is 0 and the 1st law simplifies to:

dh = v \, dp.

For approximately ideal gases, such as the dry air in the Earth's atmosphere, the equation of state, pv = RT can be substituted into the 1st law yielding, after some rearrangement:

\frac{dp}{p} = {\frac{c_p}{R}\frac{dT}{T}},

where the dh = c_{p}dT was used and both terms were divided by the product pv

Integrating yields:

\left(\frac{p_1}{p_0}\right)^{R/c_p} = \frac{T_1}{T_0},

and solving for T_{0}, the temperature a parcel would acquire if moved adiabatically to the pressure level p_{0}, you get:

T_0 = T_1 \left(\frac{p_0}{p_1}\right)^{R/c_p} \equiv \theta.

Related quantities

The Brunt–Väisälä frequency is a closely related quantity that uses potential temperature and is used extensively in investigations of atmospheric stability.


  1. ^ TAMU
  2. ^ "Isentropic Analysis". COMET. Retrieved 19 June 2012. 
  3. ^ "Isentropic Analysis". College of DuPage. Retrieved 19 June 2012. 


  • M K Yau and R.R. Rogers, Short Course in Cloud Physics, Third Edition, published by Butterworth-Heinemann, January 1, 1989, 304 pages. EAN 9780750632157 ISBN 0-7506-3215-1

External links

  • Eric Weisstein's World of Physics at Wolfram Research

See also

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