Greenhouse effect: Difference between revisions

From Citizendium
Jump to navigation Jump to search
imported>Subpagination Bot
m (Add {{subpages}} and remove any categories (details))
imported>Paul Wormer
Line 9: Line 9:
== The physics of the greenhouse ==
== The physics of the greenhouse ==


The essential condition for a greenhouse effect is the presence in a planetary atmosphere of gases that absorb (and emit) in the [[thermal radiation]] band of the planetary surface, or lower atmospheric levels. Frequently, the greenhouse gases will be transparent, or nearly so, to incoming solar radiation (ozone is an exception). The surface thermal radiation band will be in the long-wave [[infrared radiation| infrared]] region (3.5 µm - 100 µm). The greenhouse gases are triatomic (or more, but note the exception for [[Titan]]) molecules which absorb energy into a variety of [[molecular sprectra|rotational, bending, and stretching modes]]. Common solar-system gases that meet the requirements are [[water]] vapor (H<sub>2</sub>O), [[carbon dioxide]] (CO<sub>2</sub>), [[ozone]] (O<sub>3</sub>), and [[methane]] (CH<sub>4</sub>). For Earth, H<sub>2</sub>O, CO<sub>2</sub>, and O<sub>3</sub> provide most of the greenhouse. Common diatomic gases, such as [[nitrogen]] (N<sub>2</sub>) and [[oxygen]] (O<sub>2</sub>), do not have a strong enough dipole to interact well with infrared.
The essential condition for a greenhouse effect is the presence in a planetary atmosphere of gases that absorb (and emit) in the [[thermal radiation]] band of the planetary surface, or lower atmospheric levels. Frequently, the greenhouse gases will be transparent, or nearly so, to incoming solar radiation (ozone is an exception). The surface thermal radiation band will be in the long-wave [[infrared radiation| infrared]] region (3.5 µm - 100 µm). The greenhouse gases are triatomic (or more, but note the exception for [[Titan]]) molecules which absorb energy into a variety of [[molecular sprectra|rotational, bending, and stretching modes]]. Common solar-system gases that meet the requirements are [[water]] vapor (H<sub>2</sub>O), [[carbon dioxide]] (CO<sub>2</sub>), [[ozone]] (O<sub>3</sub>), and [[methane]] (CH<sub>4</sub>). For Earth, H<sub>2</sub>O, CO<sub>2</sub>, and O<sub>3</sub> provide most of the greenhouse. Common homonuclear diatomic gases, such as [[nitrogen]] (N<sub>2</sub>) and [[oxygen]] (O<sub>2</sub>), do not afford dipole transitions in the infrared and hence hardly absorb energy.


The greenhouse effect occurs at a state near local thermodynamic equilibrium. When a gas molecule is excited by an infrared quantum, the energy is promptly redistributed, by collisions, among the available degrees of freedom (of all gases present) according to the principles of [[statistical mechanics]]. So infrared absorption adds energy directly to the local thermal reservoir. Likewise, thermal infrared emission withdraws energy.
The greenhouse effect occurs at a state near local thermodynamic equilibrium. When a gas molecule is excited by an infrared quantum, the energy is promptly redistributed, by collisions, among the available degrees of freedom (of all gases present) according to the principles of [[statistical mechanics]]. So infrared absorption adds energy directly to the local thermal reservoir. Likewise, thermal infrared emission withdraws energy.

Revision as of 06:10, 11 November 2007

This article is developing and not approved.
Main Article
Discussion
Related Articles  [?]
Bibliography  [?]
External Links  [?]
Citable Version  [?]
 
This editable Main Article is under development and subject to a disclaimer.

This article is a stub and is being actively worked on.

EPA illustration of greenhouse effect

The greenhouse effect (or "atmospheric effect") is a general attribute of planets and moons with atmospheres. It is an imbalance between surface radiation and top-of-atmosphere radiation due to the presence of greenhouse gases. For example, in the case of the Earth, the surface emits 390 W/m2[1] (averaged over a year and the whole surface), but the emission at the top of the atmosphere is 235 W/m2, giving a global-average greenhouse effect of 155 W/m2[2]. The top-of-atmosphere outgoing radiation balances the incoming 235 W/m2 of solar radiation (342 W/m2 incident minus 107 W/m2 reflected). The term "greenhouse effect" is a misnomer, since actual greenhouses operate by a different mechanism.

The greenhouse and the planets

The physics of the greenhouse

The essential condition for a greenhouse effect is the presence in a planetary atmosphere of gases that absorb (and emit) in the thermal radiation band of the planetary surface, or lower atmospheric levels. Frequently, the greenhouse gases will be transparent, or nearly so, to incoming solar radiation (ozone is an exception). The surface thermal radiation band will be in the long-wave infrared region (3.5 µm - 100 µm). The greenhouse gases are triatomic (or more, but note the exception for Titan) molecules which absorb energy into a variety of rotational, bending, and stretching modes. Common solar-system gases that meet the requirements are water vapor (H2O), carbon dioxide (CO2), ozone (O3), and methane (CH4). For Earth, H2O, CO2, and O3 provide most of the greenhouse. Common homonuclear diatomic gases, such as nitrogen (N2) and oxygen (O2), do not afford dipole transitions in the infrared and hence hardly absorb energy.

The greenhouse effect occurs at a state near local thermodynamic equilibrium. When a gas molecule is excited by an infrared quantum, the energy is promptly redistributed, by collisions, among the available degrees of freedom (of all gases present) according to the principles of statistical mechanics. So infrared absorption adds energy directly to the local thermal reservoir. Likewise, thermal infrared emission withdraws energy. In simple terms, this means that an atmosphere with greenhouse gases present absorbs heat by absorbing radiation of the proper frequency as it passes through, and loses heat by emitting the same frequencies. Whether the temperature rises or falls depends on the balance between the two effects and on any other heating or cooling processes. It should be noted that the greenhouse gas molecules maintain their identity, and are not destroyed or chemically altered. This differs from the case of ionizing radiation absorption (such as the absorption of solar ultraviolet radiation by oxygen and ozone).

References and notes

  1. Watts per square metre
  2. Trenberth, K, et al., 1996. in Climate Change 1995: The Science of Climate Change, Cambridge Univ. Press.

External links

  • [1]Astrobiology article on Titan's very unusual greenhouse.

Additional bibliography

  • Houghton, JT, 1977. The Physics of Atmospheres, 3rd Ed, Cambridge Univ. Press.
  • Peixoto, JP, and AH Oort, 1992. The Physics of Climate, American Institute of Physics.
  • Thomas, GE, and K Stamnes, 1999. Radiative Transfer in the Atmosphere and Ocean, Cambridge Univ. Press.