Planetary boundary layer

Source: Wikipedia, the free encyclopedia.
Not to be confused with planetary boundaries.

This movie is a combined visualization of the PBL and wind dynamics over the Los Angeles basin for a one-month period. Vertical motion of the PBL is represented by the gray "blanket". The height of the PBL is largely driven by convection associated with the changing surface temperature of the Earth (for example, rising during the day and sinking at night). The colored arrows represent the strength and direction of winds at different altitudes.
Depiction of where the planetary boundary layer lies on a sunny day.

In meteorology, the planetary boundary layer (PBL), also known as the atmospheric boundary layer (ABL) or peplosphere, is the lowest part of the atmosphere and its behaviour is directly influenced by its contact with a planetary surface.[1] On Earth it usually responds to changes in surface radiative forcing in an hour or less. In this layer physical quantities such as flow velocity, temperature, and moisture display rapid fluctuations (turbulence) and vertical mixing is strong. Above the PBL is the "free atmosphere",[2] where the wind is approximately geostrophic (parallel to the isobars),[3] while within the PBL the wind is affected by surface drag and turns across the isobars (see Ekman layer for more detail).

Cause of surface wind gradient

The difference in the amount of aerosols below and above the boundary layer is easy to see in this aerial photograph. Light pollution from the city of Berlin is strongly scattered below the layer, but above the layer it mostly propagates out into space.
See also: Wind shear, Wind gradient, Wind engineering, and Ekman layer

Typically, due to

drag, there is a wind gradient in the wind flow ~100 meters above the Earth's surface—the surface layer of the planetary boundary layer. Wind speed increases with increasing height above the ground, starting from zero[4] due to the no-slip condition.[5] Flow near the surface encounters obstacles that reduce the wind speed, and introduce random vertical and horizontal velocity components at right angles to the main direction of flow.[6]
This
pollutants[7] and in soil erosion.[8]

The reduction in velocity near the surface is a function of surface roughness, so wind velocity profiles are quite different for different terrain types.[5] Rough, irregular ground, and man-made obstructions on the ground can reduce the geostrophic wind speed by 40% to 50%.[9][10] Over open water or ice, the reduction may be only 20% to 30%.[11][12] These effects are taken into account when siting wind turbines.[13][14]

For

exponential coefficient based on surface type. The height above ground where surface friction has a negligible effect on wind speed is called the "gradient height" and the wind speed above this height is assumed to be a constant called the "gradient wind speed".[10][15][16] For example, typical values for the predicted gradient height are 457 m for large cities, 366 m for suburbs, 274 m for open terrain, and 213 m for open sea.[17]

Although the power law exponent approximation is convenient, it has no theoretical basis.[18] When the temperature profile is adiabatic, the wind speed should vary logarithmically with height.[19] Measurements over open terrain in 1961 showed good agreement with the logarithmic fit up to 100 m or so (within the surface layer), with near constant average wind speed up through 1000 m.[20]

The shearing of the wind is usually three-dimensional,[21] that is, there is also a change in direction between the 'free' pressure gradient-driven geostrophic wind and the wind close to the ground.[22] This is related to the Ekman spiral effect. The cross-isobar angle of the diverted ageostrophic flow near the surface ranges from 10° over open water, to 30° over rough hilly terrain, and can increase to 40°-50° over land at night when the wind speed is very low.[12]

After sundown the wind gradient near the surface increases, with the increasing stability.[23] Atmospheric stability occurring at night with radiative cooling tends to vertically constrain turbulent eddies, thus increasing the wind gradient.[8] The magnitude of the wind gradient is largely influenced by the weather, principally atmospheric stability and the height of any convective boundary layer or capping inversion. This effect is even larger over the sea, where there is much less diurnal variation of the height of the boundary layer than over land.[24] In the convective boundary layer, strong mixing diminishes vertical wind gradient.[25]

Nocturnal and diurnal conditions

The planetary boundary layer is different between day and night. During the day inversion layers formed during the night are broken up as a consequence of the turbulent rise of heated air.[26] The boundary layer stabilises "shortly before sunset" and remains so during the night.[26] All this make up a daily cycle.[26] During winter and cloudy days the breakup of the nighttime layering is incomplete and atmospheric conditions established in previous days can persist.[26][27] The breakup of the nighttime boundary layer structure is fast on sunny days.[27] The driving force is convective cells with narrow updraft areas and large areas of gentle downdraft.[27] These cells exceed 200–500 m in diameter.[27]

Constituent layers

community area to over the Regents Park twin towers and out over Lake Michigan

As Navier–Stokes equations suggest, the planetary boundary layer turbulence is produced in the layer with the largest velocity gradients that is at the very surface proximity. This layer – conventionally called a surface layer – constitutes about 10% of the total PBL depth. Above the surface layer the PBL turbulence gradually dissipates, losing its kinetic energy to friction as well as converting the kinetic to potential energy in a density stratified flow. The balance between the rate of the turbulent kinetic energy production and its dissipation determines the planetary boundary layer depth. The PBL depth varies broadly. At a given wind speed, e.g. 8 m/s, and so at a given rate of the turbulence production, a PBL in wintertime Arctic could be as shallow as 50 m, a nocturnal PBL in mid-latitudes could be typically 300 m in thickness, and a tropical PBL in the trade-wind zone could grow to its full theoretical depth of 2000 m. The PBL depth can be 4000 m or higher in late afternoon over desert.

In addition to the surface layer, the planetary boundary layer also comprises the PBL core (between 0.1 and 0.7 of the PBL depth) and the PBL top or entrainment layer or capping inversion layer (between 0.7 and 1 of the PBL depth). Four main external factors determine the PBL depth and its mean vertical structure:

  1. the free atmosphere wind speed;
  2. the surface heat (more exactly buoyancy) balance;
  3. the free atmosphere density stratification;
  4. the free atmosphere vertical wind shear or
    baroclinicity
    .
Further information: Ekman layer

Principal types

Convective planetary boundary layer (CBL)

Main article: Convective planetary boundary layer

A convective planetary boundary layer is a type of planetary boundary layer where positive buoyancy flux at the surface creates a thermal instability and thus generates additional or even major turbulence. (This is also known as having CAPE or

Intertropical convergence zone
).

Stably stratified planetary boundary layer (SBL)

Interactions between the carbon (green), water (blue) and heat (red) cycles in the coupled land–ABL system. As the atmospheric boundary layer decreases in height due to subsidence, it experiences an increase in temperature, a reduction in moisture, and a depletion of CO2. This implies a reaction of the land surface ecosystem that will evapotranspire (evaporation from the soil and transpiration from plants) more, to compensate for this loss of moisture in the lower layer, but gradually causing a drying of the soil. (Source: Combe, M., Vilà-Guerau de Arellano, J., Ouwersloot, H. G., Jacobs, C. M. J., and Peters, W.: Two perspectives on the coupled carbon, water and energy exchange in the planetary boundary layer, Biogeosciences, 12, 103–123, .https://doi.org/10.5194/bg-12-103-2015, 2015)

The SBL is a PBL when negative buoyancy flux at the surface damps the turbulence; see Convective inhibition. An SBL is solely driven by the wind shear turbulence and hence the SBL cannot exist without the free atmosphere wind. An SBL is typical in nighttime at all locations and even in daytime in places where the Earth's surface is colder than the air above. An SBL plays a particularly important role in high latitudes where it is often prolonged (days to months), resulting in very cold air temperatures.

Physical laws and equations of motion, which govern the planetary boundary layer dynamics and microphysics, are strongly non-linear and considerably influenced by properties of the Earth's surface and evolution of processes in the free atmosphere. To deal with this complexity, the whole array of

turbulence modelling has been proposed. However, they are often not accurate enough to meet practical requirements. Significant improvements are expected from application of a large eddy simulation
technique to problems related to the PBL.

Perhaps the most important processes,[

hydrological cycle
, and energy exchange.

See also

References

  1. ^ "Planetary boundary layer | atmospheric science | Britannica". www.britannica.com. Retrieved 28 June 2020.
  2. ^ "Free atmosphere". glossary.ametsoc.org. Retrieved 21 March 2021.
  3. ^ "Geostrophic wind level". glossary.ametsoc.org. Retrieved 20 September 2018.
  4. ISBN 978-1-84407-262-0
    . The relation between wind speed and height is called the wind profile or wind gradient.
  5. ^
    ISBN 0-471-34877-5
    .
  6. ^ Dalgliesh, W. A. & D. W. Boyd (1 April 1962). "CBD-28. Wind on Buildings". Canadian Building Digest. Archived from the original on 12 November 2007. Retrieved 30 June 2007. Flow near the surface encounters small obstacles that change the wind speed and introduce random vertical and horizontal velocity components at right angles to the main direction of flow.
  7. ISBN 0-88385-709-X
    .
  8. ^
    ISBN 0-8493-5053-0
    .
  9. ISBN 0-415-04319-0
    . Therefore the vertical gradient of mean wind speed (dū/dz) is greatest over smooth terrain, and least over rough surfaces.
  10. ^
    ISBN 0-471-84298-2
    .
  11. ISBN 0-85404-584-8
    .
  12. ^
    ISBN 0-415-17145-8
    .
  13. ^ Maeda, Takao, Shuichiro Homma, and Yoshiki Ito. Effect of Complex Terrain on Vertical Wind Profile Measured by SODAR Technique. Retrieved on 2008-07-04.
  14. ISBN 3-540-40340-X
    .
  15. ISBN 0-8493-8969-0
    .
  16. ISBN 1-4020-2850-4
    .
  17. ISBN 0-8493-2674-5
    .
  18. ISBN 978-1-84265-125-4
    .
  19. ISBN 90-277-2768-6
    . ...both the wind gradient and the mean wind profile itself can usually be described diagnostically by the log wind profile.
  20. ISSN 1520-0450
    .
  21. ISBN 0-412-41160-1
    .
  22. ISBN 0-471-48997-2
    .
  23. ISSN 1520-0450
    .
  24. ^ Johansson, C.; Uppsala, S.; Smedman, A.S. (2002). "Does the height of the boundary layer influence the turbulence structure near the surface over the Baltic Sea?". 15th Conference on Boundary Layer and Turbulence. 15th Conference on Boundary Layer and Turbulence. American Meteorological Society.
  25. ISBN 978-0-7923-6657-7
    . In the bulk of the convective boundary layer, strong mixing diminishes vertical wind gradient...
  26. ^ a b c d Foken 2017, p. 7.
  27. ^ a b c d Foken 2017, p. 8.
  • Foken, Thomas (2017). Micrometeorology. Translated by Nappo, Carmen J.; Klein. Berlin, Germany: Springer.
    ISBN 978-3-642-25439-0
    .

External links
Retrieved from "https://en.wikipedia.org/w/index.php?title=Planetary_boundary_layer&oldid=1211060948"