[Without Title]     

Anne Marie de Grosbosis 《Environmental Geology》2005,48(7):973-977

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Flood hazard assessment in the Kujukuri Plain of Chiba Prefecture,Japan, based on GIS and multicriteria decision analysis   总被引：1，自引：0，他引：1  

Huali Chen  Yuka Ito  Marie Sawamukai  Tomochika Tokunaga 《Natural Hazards》2015,78(1):105-120

A simple flood hazard assessment based on GIS and multicriteria decision analysis was presented, and the sensitivity analysis was applied to evaluate the uncertainty of input factors. The location chosen for the study is the Kujukuri Plain, Chiba Prefecture, Japan. The model incorporates six factors: river system, elevation, depression area, ratio of impermeable area, detention ponds, and precipitation. A hazard map for the year 2004, as an example, was obtained. The method of analytic hierarchy process was applied to calculate the weighting values of each factor. The hazard map was compared with the actual flood area, and good coincidence was found between them. The relative importance and uncertainty of the six input factors and weights were evaluated by using the global sensitivity analysis, i.e., extended FAST method, and the results showed a robust behavior of the model. The flood hazard assessment method presented here is meaningful for the flood management and environment protection in the area under the similar condition as this study.  相似文献   

[Without Title]     

Anne Marie de Grosbois 《Environmental Geology》2006,50(6):935-939

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Reviews     

Daniel F. Merriam  R. A. Reyment  John W. Harbaugh  Eric C. Dahlberg  Marie Morisawa 《Mathematical Geology》1975,7(5-6):485-492

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Clairaut's theory - integral form in terms of Hansen-Tisserand polynomials     

M. Marie  M. B. El-Shaarawy 《Earth, Moon, and Planets》1993,61(1):47-56

The fourth-order integral form of Clairaut theory have been derived in terms of Hansen-Tisserand (H-T) polynomials.  相似文献   

Chemical abundances in a UV-selected sample of galaxies     

ThierryContini  Marie A.Treyer  MarkSullivan  Richard S.Ellis 《Monthly notices of the Royal Astronomical Society》2002,330(1):75-91

We discuss the chemical properties of a sample of UV-selected intermediate-redshift  (0≲z≲0.4)  galaxies in the context of their physical nature and star-formation history. This work represents an extension of our previous studies of the rest-frame UV-luminosity function (Treyer et al.) and the star-formation properties of the same sample (Sullivan et al.) . We revisit the optical spectra of these galaxies and perform further emission-line measurements restricting the analysis to those spectra with the full set of emission lines required to derive chemical abundances. Our final sample consists of 68 galaxies with heavy-element abundance ratios and both UV and CCD B -band photometry. Diagnostics based on emission-line ratios show that all but one of the galaxies in our sample are powered by hot, young stars rather than by an AGN. Oxygen-to-hydrogen (O/H) and nitrogen-to-oxygen (N/O) abundance ratios are compared with those of various local and intermediate-redshift samples. Our UV-selected galaxies span a wide range of oxygen abundances, from ∼0.1 to 1 Z_⊙, intermediate between low-mass H  ii galaxies and massive starburst nuclei. For a given oxygen abundance, most have strikingly low N/O values. Moreover, UV-selected and H  ii galaxies systematically deviate from the usual metallicity–luminosity relation in the sense of being more luminous by  2–3 mag  . Adopting the 'delayed-release' chemical evolution model, we propose our UV-selected sources are observed at a special stage in their evolution, following a powerful starburst that enriched their ISM in oxygen and temporarily lowered their mass-to-light ratios. We discuss briefly the implications of our conclusions on the nature of similarly selected high-redshift galaxies.  相似文献   

Chemical enrichment in the early galaxy     

Birgitta NordstrÖm 《Astrophysics and Space Science》2003,284(2):779-782

New, precise abundance data for a large number of elements in a growing sample of extremely metal-poor stars are accumulating from the new 8-m telescopes. Combined with theoretical models, these results advance our understanding of the first generations of stars, whose nucleosynthesis products are fossilised in the oldest stars we see today and thus give clues to the earliest phases of evolution in the Galaxy. In particular, the heaviest elements give us insight into the different neutron capture mechanisms and the stellar sites where such elements could be produced. They also afford an independent way to determine the age of the Galaxy, by radioactive chronology. This revised version was published online in August 2006 with corrections to the Cover Date.  相似文献   

[Without Title]     

Anne Marie de Grosbosis 《Environmental Geology》2005,49(2):339-343

Events

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Hα coronagraph observations of a flare spray,March 1, 1969     

Marie K. McCabe  R. R. Fisher 《Solar physics》1970,14(1):212-220

An H solar prominence with the characteristics of a spray was ejected in association with a bright limb flare. Knots of material were observed to a distance of more than one solar radius above the west limb of the Sun. The optical event was followed by 80 MHz emission from a type IV source which was observed moving out through several solar radii.Coronagraph observations have been used to determine the trajectories and velocities of the knots in directions perpendicular to the line of sight. After some early deceleration velocities increase to 300–500 km/sec and slowly decline with variations depending on the initial direction of outflow. We suggest that the magnetic field over the spot group is deformed by the energy of the mass motions of material fragments, some of which then continue to move outward from the Sun.  相似文献   

Evolution of density in solar system ICES     

R. Smoluchowski  M. Marie  A. McWilliam 《Earth, Moon, and Planets》1984,30(3):281-288

Pores present in ices in the solar system do not remain unchanged. In isothermal conditions they shrink while in a thermal gradient they migrate towards the higher temperature and escape so that the ice densifies. This motion has been investigated for pure H₂O- and CO₂-ices in a very simple one-dimensional model assuming uniform thermal conductivity and temperature gradient. The results indicate that the densification of H₂O-ice is so slow that it could be significant only for icy satellites having an internal heat source. On the other hand, CO₂-ice densifies orders of magnitude faster and the effect should be important for the CO₂ component of cometary nuclei. No effect is expected for icy planetary rings.  相似文献