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François Ascani, Eric Firing, Julian P. McCreary, Peter Brandt, and Richard J. Greatbatch

velocity in both simulations appears to be comparable to the observations above about 1500-m depth but is larger than in the observations by a factor of 3–4 below that depth ( Fig. 9 ). Error bars are large, however, so it is not clear which solution reproduces a more realistic DEIV. Note also that both simulations lack energy at lower frequencies, especially at the two easternmost locations. Fig . 8. Variance-preserving power density spectra of equatorial υ at 23°W in (a) observations, (b) solution

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A. C. Barbosa Aguiar, C. Ménesguen, S. Le Gentil, R. Schopp, and X. Carton

above and below the core at the same location as already demonstrated for anticyclones ( Ménesguen et al. 2009 ; Hua et al. 2013 ; Meunier et al. 2015 ). Along the edges of secondary vortices and filaments there is a strong signature of layering as well. The work of Meunier et al. (2015) strongly suggests that the stacked reflectors are primarily due to tracer stirring along the streamlines of a vortex field, not excluding the possibility of other concomitant processes, such as baroclinic

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