Distance over which a quantity decreases by a factor of e
The earth atmosphere's scale height is about 8.5km, as can be confirmed from this diagram of air pressure p by altitude h: At an altitude of 0, 8.5, and 17km, the pressure is about 1000, 370, and 140hPa, respectively.
Scale height used in a simple atmospheric pressure model
For planetary atmospheres, scale height is the increase in altitude for which the atmospheric pressure decreases by a factor of e. The scale height remains constant for a particular temperature. It can be calculated by[1][2] or equivalently, where
The pressure (force per unit area) at a given altitude is a result of the weight of the overlying atmosphere. If at a height of z the atmosphere has densityρ and pressure P, then moving upwards an infinitesimally small height dz will decrease the pressure by amount dP, equal to the weight of a layer of atmosphere of thicknessdz.
Thus: where g is the acceleration due to gravity. For small dz it is possible to assume g to be constant; the minus sign indicates that as the height increases the pressure decreases. Therefore, using the equation of state for an ideal gas of mean molecular mass M at temperature T, the density can be expressed as
Combining these equations gives which can then be incorporated with the equation for H given above to give which will not change unless the temperature does. Integrating the above and assuming P0 is the pressure at height z = 0 (pressure at sea level), the pressure at height z can be written as This translates as the pressure decreasing exponentially with height.[5]
In Earth's atmosphere, the pressure at sea level P0 averages about 1.01×105Pa, the mean molecular mass of dry air is 28.964Da, and hence m = 28.964Da × 1.660×10−27kg/Da = 4.808×10−26kg. As a function of temperature, the scale height of Earth's atmosphere is therefore H/T = kB/mg = 1.381×10−23J⋅K−1 / (4.808×10−26kg × 9.81m⋅s−2) = 29.28m/K. This yields the following scale heights for representative air temperatures:
T = 290K, H = 8500m,
T = 273K, H = 8000m,
T = 260K, H = 7610m,
T = 210K, H = 6000m.
These figures should be compared with the temperature and density of Earth's atmosphere plotted at NRLMSISE-00, which shows the air density dropping from 1200g/m3 at sea level to 0.125g/m3 at 70km, a factor of 9600, indicating an average scale height of 70/ln(9600) = 7.64km, consistent with the indicated average air temperature over that range of close to 260K.
Note:
Density is related to pressure by the ideal gas laws. Therefore, density will also decrease exponentially with height from a sea-level value of ρ0 roughly equal to 1.2kg⋅m−3.
At an altitude over 100km, the atmosphere is no longer well-mixed, and each chemical species has its own scale height.
Here temperature and gravitational acceleration were assumed to be constant, but both may vary over large distances.
Planetary examples
Approximate atmospheric scale heights for selected Solar System bodies:
A schematic depiction of the force balance in a gas disk around a central object, e.g., a star
For a disk of gas around a condensed central object, such as, for example, a protostar, one can derive a disk scale height which is somewhat analogous to the planetary scale height. We start with a disc of gas that has a mass small relative to the central object. We assume that the disc is in hydrostatic equilibrium with the z component of gravity from the star, where the gravity component is pointing to the midplane of the disk: where
r = the radial cylindrical coordinate for the distance from the center of the star or centrally condensed object
z = the height/altitude cylindrical coordinate for the distance from the disk midplane (or center of the star)
M* = the mass of the star/centrally condensed object
P = the pressure of the gas in the disk
= the gas mass density in the disk
In the thin disk approximation, , and the hydrostatic equilibrium, the equation is
To determine the gas pressure, one can use the ideal gas law: with
T = the gas temperature in the disk, where the temperature is a function of r, but independent of z
= the mean molecular mass of the gas
Using the ideal gas law and the hydrostatic equilibrium equation, gives which has the solution where is the gas mass density at the midplane of the disk at a distance r from the center of the star, and is the disk scale height with with the solar mass, the astronomical unit, and the dalton.
As an illustrative approximation, if we ignore the radial variation in the temperature , we see that and that the disk increases in altitude as one moves radially away from the central object.
Due to the assumption that the gas temperature T in the disk is independent of z, is sometimes known[17] as the isothermal disk scale height.
A magnetic field in a thin gas disk around a central object can change the scale height of the disk.[18][19][20] For example, if a non-perfectly conducting disk is rotating through a poloidal magnetic field (i.e., the initial magnetic field is perpendicular to the plane of the disk), then a toroidal (i.e., parallel to the disk plane) magnetic field will be produced within the disk, which will pinch and compress the disk. In this case, the gas density of the disk is[20] where the cut-off density has the form where
is the magnetic flux density of the poloidal field in the direction
is the rotational angular velocity of the central object (if the poloidal magnetic field is independent of the central object, then can be set to zero)
↑ Justus, C. G.; Aleta Duvall; Vernon W. Keller (1 August 2003). "Engineering-Level Model Atmospheres For Titan and Mars". International Workshop on Planetary Probe Atmospheric Entry and Descent Trajectory Analysis and Science, Lisbon, Portugal, October 6–9, 2003, Proceedings: ESA SP-544. ESA. Retrieved 28 September 2013.
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