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Prediction of the performance of systems designed to discharge municipal and industrial wastes into the marine environment, and of the effects of these discharges on the environment, requires an understanding of the dynamic behavior of the system. Such an understanding can be achieved only by extensive measurement of a variety of parameters of both the marine system and of the waste materials to be discharged. Techniques for the measurement of waste characteristics are well developed. In this area, the primary problem is quantification of the variability of the waste characteristics. This problem is not so much one of instrumentation as of achieving statistical reliability, applicability, and interpretability. This is due, in part, to the variety of instruments and measurement techniques available in nearshore oceanographic work, and in part, due to the complexities of the dynamic processes in the marine environment. This paper examines and discusses a number of these and related problems. The subjects discussed will include: the types of data needed for marine outfall design, types and extent of data required for determination of environmental effects, suitability of various types of instrumentation, techniques for maximizing the reliability of data acquisition, needs for new types of instrumentation, and the interpretation of data. The paper also discusses the tradeoffs which must be made between the needs and desire for information and the costs of acquiring it. 相似文献
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A small, protected karstic feature exposed in a limestone quarry in Bermuda preserved abundant sedimentary and biogenic materials documenting a transgressive phase, still-stand, and regressive phase of a sea-level in excess of 21.3 m above present during Marine Isotope Stage (MIS) 11 (400 ka) as determined by U/Th dating and amino acid racemization. Cobbles and marine sediments deposited during the high-energy transgressive phase exhibit rim cements indicating a subsequent phreatic environment. This was succeeded stratigraphically by a still-stand deposition of fine calcareous lagoonal sediments containing bioclasts of red algae and benthic and planktonic foraminifera that was intensely burrowed by marine invertebrates, probably upogebiid shrimp, that could not be produced under any condition other than sustained marine submergence. Overlying this were pure carbonate beach sands of a low-energy regressive phase containing abundant remains of terrestrial and marine vertebrates and invertebrates. The considerable diversity of this fauna along with taphonomic evidence from seabird remains indicates deposition by high run-up waves over a minimum duration of months, if not years. The maximum duration has yet to be determined but probably did not exceed one or two thousand years. The most abundant snails in this fauna are two species indicative of brackish water and high-tide line showing that a Ghyben-Herzberg lens must have existed at > + 20 m. The nature of these sediments and fossil accumulation is incompatible with tsunami deposition and, given the absence of evidence for tectonic uplift of the Bermuda pedestal or platform, provide proof that sea-level during MIS 11 exceeded +20 m, a fact that has widespread ramifications for geologists, biogeographers, and human demographics along the world's coastlines. 相似文献
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Alex D. Storrs 《Earth, Moon, and Planets》1995,71(3):99-102
The observational determination of coma outflow velocity for gaseous species is fairly straightforward using high-resolution spectroscopy. The determination of the outflow speed of the dust is much more difficult. Most sources cite Bobrovnikoff (1954). This brief report is not a strictly refereed publication, however, and mixes data from different comets.We present here a simple analysis of some data from the International Halley Watch (IHW) archive. Differences between continuum images from successive nights show dust jets and shells clearly. Their motion is apparent to first order from the edges of the features. The component of the dust outflow velocity perpendicular to the observer's line of sight may thus be determined. This is of course a lower limit on the dust outflow velocity. Many measurements, at different heliocentric distances (R), allow determination of the heliocentric dependence of the dust outflow velocity.We find that the dust outflow velocity in comet P/Halley varied as R
–0.41
. If data from an outburst at 14 AU (Sekanina et al. 1992) is included in the fit, this dependence becomes R
–0.55. This confirms the canonical (e.g. Delsemme 1982) inverse-square-root law, and supports the conclusion of Storrs et al. (1992) on the variability of cometary gas-to-dust ratios.Space Telescope Science Institute 相似文献
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We present new reconstructions of images of main belt Asteroids 9 Metis, 18 Melpomene, 19 Fortuna, 216 Kleopatra, and 624 Hektor, made with the uncorrected Wide-Field/Planetary Camera (WF/PC) on the Hubble Space Telescope (HST). Deconvolution with the MISTRAL algorithm demonstrates that these asteroids are clearly resolved. We determine diameters, albedos, and lower limits to axial ratios for these bodies. We also review the process used to restore the aberrated images. No surface features or companions are found, but the rotation of 216 Kleopatra is clearly seen. The asteroidal albedos are similar to those determined by other procedures. 相似文献
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Alex D. Storrs 《Earth, Moon, and Planets》1996,72(1-3):99-102
The observational determination of coma outflow velocity for gaseous species is fairly straightforward using high-resolution spectroscopy. The determination of the outflow speed of the dust is much more difficult. Most sources cite Bobrovnikoff (1954). This brief report is not a strictly refereed publication, however, and mixes data from different comets. We present here a simple analysis of some data from the International Halley Watch (IHW) archive. Differences between continuum images from successive nights show dust jets and shells clearly. Their motion is apparent to first order from the edges of the features. The component of the dust outflow velocity perpendicular to the observer's line of sight may thus be determined. This is of course a lower limit on the dust outflow velocity. Many measurements, at different heliocentric distances (R), allow determination of the heliocentric dependence of the dust outflow velocity. We find that the dust outflow velocity in comet P/Halley varied as R ?0.41 . If data from an outburst at 14 AU (Sekanina et al. 1992) is included in the fit, this dependence becomes R ?0.55. This confirms the canonical (e.g. Delsemme 1982) inverse-square-root law, and supports the conclusion of Storrs et al. (1992) on the variability of cometary gas-to-dust ratios. 相似文献
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Dan Pascu Alex D. Storrs John L. Hershey James R. Rohde Douglas G. Currie 《Icarus》2006,185(2):487-491
BVI photometry of Triton and Proteus was derived from HST images taken in 1997. The VEGAMAG photometric technique was used. Triton was found to be brighter by a few percent than observations of the 1970's and 1980's, as expected due to the increasingly greater exposure of the bright south polar region. The leading side was also found to be brighter than the trailing side by 0.09 mag in all filters—50% larger than reported by Franz [Franz, O.G., 1981. Icarus 45, 602-606]. Contrary to our previous results [Pascu, D., et al., 1998. Bull. Am. Astron. Soc. 30, 1101], we found no episodic reddening. Our previous conclusions were based on an inaccurate early version of the Charge Transfer Efficiency (CTE) correction. The present result limits the start of the reddening event reported by Hicks and Buratti [Hicks, M.D., Buratti, B.J., 2004. Icarus 171, 210-218]. Our (B-V) result of 0.70±0.01 supports the global blueing described by Buratti et al. [Buratti, B.J., Goguen, J.D., Gibson, J., Mosher, J., 1994. Icarus 110, 303-314]. Our observations of July 1997 agree with the Voyager results and are among the bluest colors seen. We found Proteus somewhat brighter than earlier studies, but in good agreement with the recent value given by Karkoschka [Karkoschka, E., 2003. Icarus 162, 400-407]. A leading/trailing brightness asymmetry was detected for Proteus, with the leading side 0.1 mag brighter. The unique differences in action of the endogenic and exogenic processes on Triton and Proteus provides an opportunity to separate the endogenic and exogenic effects on Triton. 相似文献
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