scholarly journals An Inverse Method for Obtaining the Attenuation Profile and Small Variations in the Sound Speed and Density Profiles of the Ocean Bottom

1987 ◽  
pp. 279-286
Author(s):  
Subramaniam D. Rajan ◽  
George V. Frisk
Keyword(s):  
Sound Speed ◽  
Inverse Method ◽  
Ocean Bottom ◽  
Density Profiles ◽  
Attenuation Profile

Effects of tidally varying sound speed on acoustic propagation over a sloping ocean bottom

1979 ◽  
Vol 66 (4) ◽  
pp. 1108-1119 ◽  
Author(s):  
K. G. Hamilton ◽  
W. L. Siegmann ◽  
M. J. Jacobson
Keyword(s):  
Sound Speed ◽  
Acoustic Propagation ◽  
Ocean Bottom

An inverse method for estimating sediment sound speed in the ocean

2012 ◽  
Vol 132 (3) ◽  
pp. 2094-2094
Author(s):  
Tao Lin ◽  
Zoi-Heleni Michalopoulou
Keyword(s):  
Sound Speed ◽  
Inverse Method

An inverse method for estimating sediment sound speed

2013 ◽  
Vol 134 (5) ◽  
pp. 4241-4241
Author(s):  
Tao Lin ◽  
Zoi-Heleni Michalopoulou
Keyword(s):  
Sound Speed ◽  
Inverse Method

scholarly journals Helioseismology and the Solar Neutrino Problem

1998 ◽  
Vol 185 ◽  
pp. 41-42
Author(s):  
H. M. Antia ◽  
S. M. Chitre
Keyword(s):  
Solar Neutrino ◽  
Sound Speed ◽  
Nuclear Energy ◽  
Solar Interior ◽  
Density Profiles ◽  
Solar Neutrino Problem ◽  
Composition Profiles ◽  
Neutrino Fluxes ◽  
Solar Material ◽  
Seismic Models

The precisely measured frequencies of solar oscillations provide us with a unique tool to probe the solar interior with sufficient accuracy. These frequencies are principally determined by the dynamical quantities like sound speed, density or the adiabatic index of the solar material and a primary inversion of the observed frequencies yields the sound speed and density profiles inside the Sun (Gough et al. 1996). The equations of thermal equilibrium enable us to determine the temperature and chemical composition profiles, but for this additional prescriptions regarding the input physics (i.e., opacities, equation of state and nuclear energy generation rate) are required (Shibahashi 1993; Antia & Chitre 1995; Shibahashi & Takata 1996; Kosovichev 1996). This information in turn can be used to calculate the neutrino fluxes, and the seismic models can thus be used to explore the possibility of an astrophysical solution to the solar neutrino problem (Roxburgh 1996; Antia & Chitre 1997).

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