Observations of energetic low frequency current fluctuations in the Charlie-Gibbs fracture zone

Also published as: Journal of Marine Research 36 (1978): 725-734Relatively energetic low frequency fluctuations in horizontal currents are found to exist below the thermocline in the northern trough of the Charlie-Gibbs Fracture Zone. For example, deep eddy kinetic energy levels there are about twice as large as those observed at similar relative depths in the MODE-I region. Eddy kinetic energies are about 2-10 times larger than mean kinetic energies. The vertical distribution of eddy kinetic energy is frequency dependent, increasing toward the thermocline for the longer time scales and intensifying toward the bottom at higher frequencies. In addition to the expected mean westward motion of Norwegian Sea Overflow Water through the northern trough of the fracture, rather consistent mean southward flow is observed at a depth immediately above the overflow.Prepared f or the Office of Naval Research under Contract N00014-76-C-0197; NR 083- 400

When Yankee Doodle Learns To Parlez Vous Francais

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Observations of energetic low frequency current fluctuations in the Charlie-Gibbs Fracture Zone

Relatively energetic low frequency fluctuations in horizontal currents are found to exist below the thermocline in the northern trough of the Charlie-Gibbs Fracture Zone. For example, deep eddy kinetic energy levels there are about twice as large as those observed at similar relative depths in the MODE-I region. Eddy kinetic energies are about 2-10 times larger than mean kinetic energies...

When The Moon Begins To Shine : Through The Pines Of Carolin\u27

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She\u27ll Miss Me Most Of All

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Exploratory observations of abyssal currents in the South Atlantic near Vema Channel

Vema Channel (nominal location 30S, 40W) is a major passage for the flow of Antarctic Bottom Water on its way northward from the Argentine Basin to the Brazil Basin. New data based on approximately year-long current meter deployments at abyssal depths yield mean or time-averaged kinetic energies as strong as 240 cm2s−2, and eddy kinetic energies from 8 to 40 cm2s−2. We observe a persistent northward flow of AABW with maximum speed near 40 cm s−1, as is found at abyssal depths in the vicinity of the Gulf Stream. The highest value of mean kinetic energy in Vema Channel (240 cm2 s−2) is much larger than that (∼20 cm2 s−2) found in the flow of Antarctic Bottom Water near the Ceara Rise, and comparable to values of 220 cm2 s−2 for the southward flow of North Atlantic Deep Water on the Blake-Bahama Outer Ridge. Existing observations of mean kinetic energy at locations near the Gulf Stream System do not exceed 100 cm2 s−2 in the abyssal depth range.Eddy kinetic energies of 8 cm−2 s−2 are comparable to estimates (at similar depths) from areas at roughly equivalent latitudes, like MODE (Mid-Ocean Dynamics Experiment, nominal location 28N, 70W). However, abyssal kinetic energies as large as 40 cm2 s−2 are normally found only near strong current regimes, in contrast to values of roughly 1 cm2 s−2 in the ocean interior. Values of 18 to 64 cm2 s−2 have been observed near the southward flow of North Atlantic Deep Water on and adjacent to the Blake-Bahama Outer Ridge near 30N, and up to 20 cm2 s−2 in the flow of Antarctic Bottom Water over the Ceara Rise. The strongest abyssal eddy field yet observed, ∼100 to 150 cm2 s−2, occurs near the Gulf Stream

Evaluation of Risk Management Methods for Satsuma Mandarin

Simulation of production budgets were used to compare net discounted returns and the distribution of returns under alternative risk-mitigation scenarios. Results indicate that the combination of freeze protection and crop insurance increases expected net discounted 20-year returns while decreasing the downside risk. Break-even prices ranged from $.257 to$.289 per pound. Crop insurance returns were constant across price.Satsuma oranges, freeze protection, crop insurance, production budget, simulation, Crop Production/Industries, Farm Management, Risk and Uncertainty, C63, D81, Q12,

Mandarin Market Segments Based on Consumer Sensory Evaluations

Ninety-five consumers in seven grocery stores tasted unidentified peeled sections of three mandarins (a tangerine, a satsuma, and a clementine), and provided demographic and purchase information. Forty-four percent of the respondents preferred tangerines, 34 percent satsumas, and 22 percent clementines. The probability of preferring each of type of mandarin was estimated from internal quality analysis of paired samples, as well as from demographic and purchase responses. Model simulations were used to recommend harvest standards for satsumas based on Brix-to-acid ratios.Demand and Price Analysis, Food Consumption/Nutrition/Food Safety,

A Chemical Composition Survey of the Iron-Complex Globular Cluster NGC 6273 (M 19)

Recent observations have shown that a growing number of the most massive Galactic globular clusters contain multiple populations of stars with different [Fe/H] and neutron-capture element abundances. NGC 6273 has only recently been recognized as a member of this "iron-complex" cluster class, and we provide here a chemical and kinematic analysis of > 300 red giant branch (RGB) and asymptotic giant branch (AGB) member stars using high resolution spectra obtained with the Magellan-M2FS and VLT-FLAMES instruments. Multiple lines of evidence indicate that NGC 6273 possesses an intrinsic metallicity spread that ranges from about [Fe/H] = -2 to -1 dex, and may include at least three populations with different [Fe/H] values. The three populations identified here contain separate first (Na/Al-poor) and second (Na/Al-rich) generation stars, but a Mg-Al anti-correlation may only be present in stars with [Fe/H] > -1.65. The strong correlation between [La/Eu] and [Fe/H] suggests that the s-process must have dominated the heavy element enrichment at higher metallicities. A small group of stars with low [alpha/Fe] is identified and may have been accreted from a former surrounding field star population. The cluster's large abundance variations are coupled with a complex, extended, and multimodal blue horizontal branch (HB). The HB morphology and chemical abundances suggest that NGC 6273 may have an origin that is similar to omega Cen and M 54.Comment: Accepted for Publication in The Astrophysical Journal; 50 pages; 18 figures; 8 tables; higher resolution figures are available upon request or in the published journal articl