The Galapagos Spreading Centre: Lithospheric Cooling and Hydrothermal Circulation

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Abstract

The spatial pattern of cooling near a spreading ridge crest was investigated with a suite of 71 precisely‐navigated heat‐flow stations on the Galapagos spreading centre, East Pacific, near 86°W longitude. Stations are on crust less than 1 0 My old on which bathymetry and sediment distribution are well known. Values vary from near zero to greater than 30 HFU (10−6 cal cm−2 s−1). The average over the entire region is significantly less than that predicted by theoretical conduction models of a cooling lithosphere. We observe a regular variation of the heat‐flow pattern with a wavelength of 6 ± 1 km approximately normal to the ridge crest. Heat‐flow maxima are characteristically located near faults and local topographic highs. The locations of fields of small sediment mounds, apparently hydrothermal vents, are also restricted to these faulted, elevated areas of high heat flow. Near‐axis, bottom water temperature anomalies of several hundredths °C were detected. The low average, the low minima in the heat‐flow pattern, and the water temperature anomalies suggest that hydrothermal circulation accounts for approximately 80 per cent of the geothermal heat released near the ridge crest. We conclude that the hydrothermal circulation pattern is controlled by one or more of the following physical properties of the system: highly developed cellular convection, discrete zones of high permeability, variation in the strength of heat sources near the base of the crust, or bottom topography. Our results imply that heat‐flow studies near active oceanic ridges will be of most value if they are sufficiently detailed and well navigated to define the systematic small‐scale variations that appear to be caused by hydrothermal circulation. Copyright © 1974, Wiley Blackwell. All rights reserved

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Williams, D. L., Von Herzen, R. P., Sclater, J. G., & Anderson, R. N. (1974). The Galapagos Spreading Centre: Lithospheric Cooling and Hydrothermal Circulation. Geophysical Journal of the Royal Astronomical Society, 38(3), 587–608. https://doi.org/10.1111/j.1365-246X.1974.tb05431.x

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