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Planetary Temperatures in the Presence of an Inert, Nonradiative Atmosphere

John Leslie Nicol

John Leslie Nicol

Department of Physics, James Cook University of North QueenslandAustralia
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Nicol, John Leslie
  
06. Sept. 2020
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Online veröffentlicht: 06. Sept. 2020
Seitenbereich: 69 - 85
Eingereicht: 07. Feb. 2020
DOI: https://doi.org/10.2478/quageo-2020-0024
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© 2020 John Leslie Nicol, published by Sciendo
This work is licensed under the Creative Commons Attribution 3.0 Public License.

Fig. 1

Energy from the visible sunlight absorbed by the planet's surface raising the temperature of the soil below as the heat is transmitted to lower levels. The air above is also warmed through the contact with the hot surface skin, which also emits energy to space as infrared radiation.
Energy from the visible sunlight absorbed by the planet's surface raising the temperature of the soil below as the heat is transmitted to lower levels. The air above is also warmed through the contact with the hot surface skin, which also emits energy to space as infrared radiation.

Fig. 2

Diurnal temperature changes at various depths of 5, 15, 30, 45 and 60 cm. Earth conductivity = 1. Phases of the so-called temperature-waves similar to those shown in the diagram of experimental measurements – Figure 3.
Diurnal temperature changes at various depths of 5, 15, 30, 45 and 60 cm. Earth conductivity = 1. Phases of the so-called temperature-waves similar to those shown in the diagram of experimental measurements – Figure 3.

Fig. 3

Continuous measurements of soil temperatures over 7 days by CSIRO, Australia, in January (Summer) 1939 (acc. to West 1952).
Continuous measurements of soil temperatures over 7 days by CSIRO, Australia, in January (Summer) 1939 (acc. to West 1952).

Fig. 4

Temperature of the radiating surface skin of the planet where the temperature of the internal layer at a depth of 30 cm varies from 200 to 350 K and for various assumed thermal conductivities of the soil ranging from 1 to 4 Wm−1K−1.
Temperature of the radiating surface skin of the planet where the temperature of the internal layer at a depth of 30 cm varies from 200 to 350 K and for various assumed thermal conductivities of the soil ranging from 1 to 4 Wm−1K−1.

Fig. 5

The planetary soil and inert atmosphere (air) with a higher temperature Ta than solid layers at greater depths.
The planetary soil and inert atmosphere (air) with a higher temperature Ta than solid layers at greater depths.

Fig. 6

Model of inert atmosphere above a planetary surface under conditions of slow warming of the solid material from the previously heated atmospheric gases above. Note the thin, stable layer of cooled air shown in white in the right-hand model.
Model of inert atmosphere above a planetary surface under conditions of slow warming of the solid material from the previously heated atmospheric gases above. Note the thin, stable layer of cooled air shown in white in the right-hand model.

Fig. 7

Time series of temperatures: during a clear sky period near Summit, Greenland. IR skin 2 m in air (acc. Adolph et al. 2018).
Time series of temperatures: during a clear sky period near Summit, Greenland. IR skin 2 m in air (acc. Adolph et al. 2018).

Fig. 8

A comparison of the surface and air temperatures at Marblemount, Washington.
A comparison of the surface and air temperatures at Marblemount, Washington.

Fig. 9

Relations between surface temperature and air temperature on a local scale during winter nights (acc. to Kawashima et al. 2000).
Relations between surface temperature and air temperature on a local scale during winter nights (acc. to Kawashima et al. 2000).

Fig. 10

Characteristic temperatures of a solid planet with an inert atmosphere.1 – mean air temperature approximately 1.2 m above the surface skin, 2 – effective emission temperature of the surface skin and 3 – mean temperature of the surface skin.
Characteristic temperatures of a solid planet with an inert atmosphere.1 – mean air temperature approximately 1.2 m above the surface skin, 2 – effective emission temperature of the surface skin and 3 – mean temperature of the surface skin.

Fig. 11

The Vostok surface (solid line) and 500 hPa (dashed line ~5500 m) temperature records for July 1983 (acc. to Turner et al. 2009).
The Vostok surface (solid line) and 500 hPa (dashed line ~5500 m) temperature records for July 1983 (acc. to Turner et al. 2009).

Figure A

The temperature of the surface skin of the earth (blue) and of the air at 1.2 m above the ground (red) over 24 h. The air is assumed to have a thermal conductivity of 0.03 W m−1 K−1 and a thermal capacitance of 1.006 kJ Kg−1 K−1.For a maximum solar intensity of: a – 200 Wm−2, b – 400 Wm−2, c – 600 Wm−2, d – 800 Wm−2, e – 1000 Wm−2, f – 1200 Wm−2, g – 1500 Wm−2 and h – 2000 Wm−2.
The temperature of the surface skin of the earth (blue) and of the air at 1.2 m above the ground (red) over 24 h. The air is assumed to have a thermal conductivity of 0.03 W m−1 K−1 and a thermal capacitance of 1.006 kJ Kg−1 K−1.For a maximum solar intensity of: a – 200 Wm−2, b – 400 Wm−2, c – 600 Wm−2, d – 800 Wm−2, e – 1000 Wm−2, f – 1200 Wm−2, g – 1500 Wm−2 and h – 2000 Wm−2.
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