Login
Register
Reset Password
Publish & Distribute
Publishing Solutions
Distribution Solutions
Subjects
Architecture and Design
Arts
Business and Economics
Chemistry
Classical and Ancient Near Eastern Studies
Computer Sciences
Cultural Studies
Engineering
General Interest
Geosciences
History
Industrial Chemistry
Jewish Studies
Law
Library and Information Science, Book Studies
Life Sciences
Linguistics and Semiotics
Literary Studies
Materials Sciences
Mathematics
Medicine
Music
Pharmacy
Philosophy
Physics
Social Sciences
Sports and Recreation
Theology and Religion
Publications
Journals
Books
Proceedings
Publishers
Blog
Contact
Search
EUR
USD
GBP
English
English
Deutsch
Polski
Español
Français
Italiano
Cart
Home
Journals
Quaestiones Geographicae
Volume 39 (2020): Issue 3 (September 2020)
Open Access
Planetary Temperatures in the Presence of an Inert, Nonradiative Atmosphere
John Leslie Nicol
John Leslie Nicol
| Sep 06, 2020
Quaestiones Geographicae
Volume 39 (2020): Issue 3 (September 2020)
About this article
Previous Article
Next Article
Abstract
Article
Figures & Tables
References
Authors
Articles in this Issue
Preview
PDF
Cite
Share
Published Online:
Sep 06, 2020
Page range:
69 - 85
Received:
Feb 07, 2020
DOI:
https://doi.org/10.2478/quageo-2020-0024
Keywords
planet
,
inert atmosphere
,
temperatures
,
capacity/conductivity
,
soil
,
air
© 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.
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.
Fig. 3
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.
Fig. 5
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.
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).
Fig. 8
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).
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.
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).
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.
Preview