equilibrium temperature

The planetary equilibrium temperature is a theoretical temperature that a planet would be if it were in radiative equilibrium, typically under the assumption that it radiates as a black body being heated only by its parent star. In this model, the presence or absence of an atmosphere (and therefore any greenhouse effect) is irrelevant, as the equilibrium temperature is calculated purely from a balance with incident stellar energy.

Other authors use different names for this concept, such as equivalent blackbody temperature of a planet. The effective radiation emission temperature is a related concept, but focuses on the actual power radiated rather than on the power being received, and so may have a different value if the planet has an internal energy source or when the planet is not in radiative equilibrium.

Planetary equilibrium temperature differs from the global mean temperature and surface air temperature, which are measured observationally by satellites or surface-based instruments, and may be warmer than the equilibrium temperature due to the greenhouse effect.

Calculation of equilibrium temperature

Consider a planet orbiting its host star. The star emits radiation isotropically, and some fraction of this radiation reaches the planet. The amount of radiation arriving at the planet is referred to as the incident solar radiation, $I_o$. The planet has an albedo that depends on the characteristics of its surface and atmosphere, and therefore only absorbs a fraction of radiation. The planet absorbs the radiation that isn't reflected by the albedo, and heats up. One may assume that the planet radiates energy like a blackbody at some temperature according to the Stefan–Boltzmann law. Radiative equilibrium exists when the power supplied by the star is equal to the power emitted by the planet. The temperature at which this balance occurs is the planetary equilibrium temperature.

Derivation

The solar flux absorbed by the planet from the star is equal to the flux emitted by the planet:

$_=_$

Assuming a fraction of the incident sunlight is reflected according to the planet's Bond albedo, $A_B$:

$(1-A_B)_=_$

where $_$ represents the area- and time-averaged incident solar flux, and may be expressed as:

$F_=I_o/4$

The factor of 1/4 in the above formula comes from the fact that only a single hemisphere is lit at any moment in time (creates a factor of 1/2), and from integrating over angles of incident sunlight on the lit hemisphere (creating another factor of 1/2).

Assuming the planet radiates as a blackbody according to the Stefan–Boltzmann law at some equilibrium temperature $_$, a balance of the absorbed and outgoing fluxes produces:

$(1-A_B)\left ( \frac \right )=\sigma\ T_^4$ where $\sigma$ is the Stefan-Boltzmann constant.

Rearranging the above equation to find the equilibrium temperature leads to:

$_=^$

$T_\mathrm=^$ where ''$L_0$'' is the luminosity of the Sun ($3,828\cdot 10^$ W), and ''$d$'' the distance between the planet and the Sun, then :

$T_\mathrm= 1.07652\cdot 10^8 ^$ (with ''$d$'' in metres), or :

$T_\mathrm= 3,404.255\cdot ^$ (with ''$d$'' in million kilometres).

Calculation for extrasolar planets

For a planet around another star, $I_o$(the incident stellar flux on the planet) is not a readily measurable quantity. To find the equilibrium temperature of such a planet, it may be useful to approximate the host star's radiation as a blackbody as well, such that:

$F_=\sigma T_^4$

The luminosity ($L$) of the star, which can be measured from observations of the star's apparent brightness, can then be written as:

$L=4\pi R_^2\sigma T_^4$ where the flux has been multiplied by the surface area of the star.

To find the incident stellar flux on the planet, $I_x$, at some orbital distance from the star, $a$, one can divide by the surface area of a sphere with radius $a$:

$I_x=\left ( \frac\right )$

Plugging this into the general equation for planetary equilibrium temperature gives:

$_=^$

If the luminosity of the star is known from photometric observations, the other remaining variables that must be determined are the Bond albedo and orbital distance of the planet. Bond albedos of exoplanets can be constrained by flux measurements of transiting exoplanets, and may in future be obtainable from direct imaging of exoplanets and a conversion from geometric albedo. Orbital properties of the planet such as the orbital distance can be measured through radial velocity and transit period measurements.

Alternatively, the planetary equilibrium may be written in terms of the temperature and radius of the star:

$_=T_\sqrt \left( 1-A_B \right)^$

Caveats

The equilibrium temperature is neither an upper nor lower bound on actual temperatures on a planet. There are several reasons why measured temperatures deviate from predicted equilibrium temperatures.

Greenhouse effect

In the greenhouse effect, long wave radiation emitted by a planet is absorbed by certain gases in the atmosphere, reducing longwave emissions to space. Planets with substantial greenhouse atmospheres emit more longwave radiation at the surface than what reaches space. Consequently, such planets have surface temperatures higher than their effective radiation emission temperature. For example, Venus has an effective temperature of approximately , but a surface temperature of . Similarly, Earth has an effective temperature of , but a surface temperature of about due to the greenhouse effect in our lower atmosphere. The surface temperatures of such planets are more accurately estimated by modeling thermal radiation transport through the atmosphere.

Airless bodies

On airless bodies, the lack of any significant greenhouse effect allows equilibrium temperatures to approach mean surface temperatures, as on Mars, where the equilibrium temperature is and the mean surface temperature of emission is . There are large variations in surface temperature over space and time on airless or near-airless bodies like Mars, which has daily surface temperature variations of 50–60 K. Because of a relative lack of air to transport or retain heat, significant variations in temperature develop. Assuming the planet radiates as a blackbody (i.e. according to the Stefan-Boltzmann law), temperature variations propagate into emission variations, this time to the power of 4. This is significant because our understanding of planetary temperatures comes not from direct measurement of the temperatures, but from measurements of the fluxes. Consequently, in order to derive a meaningful mean surface temperature on an airless body (to compare with an equilibrium temperature), a global average surface emission flux is considered, and then an 'effective temperature of emission' that would produce such a flux is calculated. The same process would be necessary when considering the surface temperature of the Moon, which has an equilibrium temperature of , but can have temperatures of in the daytime and at night. Again, these temperature variations result from poor heat transport and retention in the absence of an atmosphere.

Internal energy fluxes

Orbiting bodies can also be heated by tidal heating, geothermal energy which is driven by radioactive decay in the core of the planet, or accretional heating. These internal processes will cause the effective temperature (a blackbody temperature that produces the observed radiation from a planet) to be warmer than the equilibrium temperature (the blackbody temperature that one would expect from solar heating alone).

For example, on Saturn, the effective temperature is approximately 95 K, compared to an equilibrium temperature of about 63 K. This corresponds to a ratio between power emitted and solar power received of ~2.4, indicating a significant internal energy source. Jupiter and Neptune have ratios of power emitted to solar power received of 2.5 and 2.7, respectively.

Close correlation between the effective temperature and equilibrium temperature of Uranus can be taken as evidence that processes producing an internal flux are negligible on Uranus compared to the other giant planets.

Earth has insufficient geothermal heating to significantly affect its global temperature, with geothermal heating supplying only 0.03% of Earth's total energy budget.

See also

*Earth's energy budget
*Effective temperature
*Thermal equilibrium

References

Sources

*
* {{cite book , last1=Wallace , first1=J.M. , last2=Hobbs , first2=P.V. , year=2006 , title=Atmospheric Science. An Introductory Survey , edition=2nd , publisher=Elsevier , location=Amsterdam , isbn=978-0-12-732951-2

Thermodynamics
Planetary science
Equations of astronomy