World Library  
Flag as Inappropriate
Email this Article

Tidal heating

Article Id: WHEBN0005903656
Reproduction Date:

Title: Tidal heating  
Author: World Heritage Encyclopedia
Language: English
Subject: Ganymede (moon), Enceladus, Solar System/Selected article/13, Reference desk/Archives/Science/2013 February 21, Volcanoes/Selected article/5
Collection: Planetary Science, Tides
Publisher: World Heritage Encyclopedia
Publication
Date:
 

Tidal heating

Tidal heating (also known as tidal working) occurs through the tidal friction processes: orbital and rotational energy are dissipated as heat in either the surface ocean or interior of a planet or satellite. Io, a moon of Jupiter, is the most volcanically active body in the solar system, with no impact craters surviving on its surface. This is because the tidal force of Jupiter deforms Io;[1] the eccentricity of Io's orbit (a consequence of its participation in a Laplace resonance) causes the height of Io's tidal bulge to vary significantly (by up to 100 m) over the course of an orbit; the friction from this tidal flexing then heats up its interior. A similar but weaker process is theorised to have melted the lower layers of the ice surrounding the rocky mantle of Jupiter's next large moon, Europa. Saturn's moon Enceladus is similarly thought to have a liquid water ocean beneath its icy crust. The water vapor geysers which eject material from Enceladus are thought to be powered by friction generated within this moon's shifting ice crust.[2]

The total amount of tidal heating q_{tid} is given by

q_{tid} = 63 \rho n^5 r^4 e^2 / (38 \mu Q)

where \rho is the mean density of the satellite, n is the mean orbital motion, r is the satellite’s radius, e is the eccentricity of the orbit, \mu is the shear modulus, and Q is a dimensionless dissipation factor. The role of tidal heating is sometimes expressed by dimensionless number C equal to quotient of tidal heating and total internal heating.[3]

See also

References

  1. ^ Peale, S. J.; Cassen, P.; Reynolds, R. T. (1979), "Melting of Io by Tidal Dissipation", Science 203 (4383): 892–894,  
  2. ^ Peale, S.J. Tidally induced volcanism. Celest. Mech. & Dyn. Astr. 87, 129– 155, 2003.
  3. ^ Czechowski, L., 2006, Parameterized model of convection driven by tidal and radiogenic heating, Adv. Space Res, 38, 4, 788-793


This article was sourced from Creative Commons Attribution-ShareAlike License; additional terms may apply. World Heritage Encyclopedia content is assembled from numerous content providers, Open Access Publishing, and in compliance with The Fair Access to Science and Technology Research Act (FASTR), Wikimedia Foundation, Inc., Public Library of Science, The Encyclopedia of Life, Open Book Publishers (OBP), PubMed, U.S. National Library of Medicine, National Center for Biotechnology Information, U.S. National Library of Medicine, National Institutes of Health (NIH), U.S. Department of Health & Human Services, and USA.gov, which sources content from all federal, state, local, tribal, and territorial government publication portals (.gov, .mil, .edu). Funding for USA.gov and content contributors is made possible from the U.S. Congress, E-Government Act of 2002.
 
Crowd sourced content that is contributed to World Heritage Encyclopedia is peer reviewed and edited by our editorial staff to ensure quality scholarly research articles.
 
By using this site, you agree to the Terms of Use and Privacy Policy. World Heritage Encyclopedia™ is a registered trademark of the World Public Library Association, a non-profit organization.
 



Copyright © World Library Foundation. All rights reserved. eBooks from World Library are sponsored by the World Library Foundation,
a 501c(4) Member's Support Non-Profit Organization, and is NOT affiliated with any governmental agency or department.