Sound speed and attenuation in marine sediments measured at high frequencies with a bottom probe system

1982 ◽  
Vol 72 (S1) ◽  
pp. S98-S98 ◽  
Author(s):  
Y. Igarashi ◽  
R. L. Allman
2006 ◽  
Vol 120 (5) ◽  
pp. 3099-3099
Author(s):  
William M. Carey ◽  
Ji‐Xun Zhou ◽  
Allan D. Pierce

2016 ◽  
Vol 140 (1) ◽  
pp. 274-282 ◽  
Author(s):  
A. Mantouka ◽  
H. Dogan ◽  
P. R. White ◽  
T. G. Leighton

Geophysics ◽  
1960 ◽  
Vol 25 (3) ◽  
pp. 659-682 ◽  
Author(s):  
George Shumway

The relationships between sound speed and the more important physical properties of unconsolidated sediments have become known in recent years largely as a result of the studies of Hamilton, 1956; Hamilton et al., 1956; Shumway, 1956, 1958; Nafe and Drake, 1957; Sutton, Berckhemer and Nafe, 1957; and Laughton, 1954, 1957. The suite of samples used in this study is larger and more varied than the suites used in any of the earlier studies, and the measurements probably were more carefully taken. A large number of shelf and harbor sediments were used in addition to sediments from deeper water in the Pacific and Arctic Oceans.


Geophysics ◽  
1984 ◽  
Vol 49 (3) ◽  
pp. 297-299 ◽  
Author(s):  
Thomas S. Edrington ◽  
Terry M. Calloway

The speed and attenuation of sound in gassy marine sediments in the Mississippi delta area have been measured by means of small (1 to 500 mg) explosive charges buried 30 m below the mud line. The respective values obtained were 800 m/sec and 1.4 dB/kHz-m. Effective gas content was estimated to be approximately 0.06 percent.


1979 ◽  
Vol 46 ◽  
pp. 77-88
Author(s):  
Edward L. Robinson

Three distinct kinds of rapid variations have been detected in the light curves of dwarf novae: rapid flickering, short period coherent oscillations, and quasi-periodic oscillations. The rapid flickering is seen in the light curves of most, if not all, dwarf novae, and is especially apparent during minimum light between eruptions. The flickering has a typical time scale of a few minutes or less and a typical amplitude of about .1 mag. The flickering is completely random and unpredictable; the power spectrum of flickering shows only a slow decrease from low to high frequencies. The observations of U Gem by Warner and Nather (1971) showed conclusively that most of the flickering is produced by variations in the luminosity of the bright spot near the outer edge of the accretion disk around the white dwarf in these close binary systems.


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