Theoretical models for Mars and their seismic properties

Theoretical seismic properties of the planet Mars are investigated on the basis of the various models which have been proposed for the internal composition of the planet. The latest interpretation of gravity field data (Reasenberg, 1977), assuming a lower value of the moment of inertia, would require a less dense mantle and a larger core than previous models. If Mars is chondritic in composition, the most reasonable models are an incompletely differentiated H-chondrite or a mixture of H-chondrites and carbonaceous chondrites. Seismic profiles, travel times, and free oscillation periods are computed for various models, with the aim of establishing which seismic data is crucial for deciding among the alternatives. A detailed discussion is given of the seismic properties which could—in principle—help answer the following two questions: Is Mars' core liquid or solid? Does Mars have a partially molten asthenosphere in its upper mantle?     

Slug Tests in the Presence of Background Head Trends

We extend Bouwer and Rice (1976) slug test theory to incorporate background head trends that may be important in incompressible material of low permeability k. The extension, which features a convolution integral of the background head, is closed form for linear trends. A sensitivity study suggests that a rising background head can diminish the head changes associated with a slug-out test and underestimate k if it is ignored, as does falling background trend with a slug-in test. A falling background head can reinforce slug-in test head change and, if ignored, can overestimate k, as does a rising background head with a slug-out test. The simple extension is verified by field tests in glacial till and stratified drift deposits in eastern Massachusetts.     

New theory of the Earth

From time to time the phrase ＇Theory of the Earth＇ occurs among titles in Earth science history. It usually happens after times of changing major scientific paradigms. A first peak occurred in the Renaissance at the time of the origin of modern science with the introduction of the word geology by Ulisse Aldrovandi in 1603; and the phrase moved around in the controversy about the origin of marine fossils found in mountains, with works by Alessandro degli Alessandri （about 1500）, Girolamo Cardano （1550）, Gabriele Falloppio （1564）, Bernard Palissy （1580）, Andrea Cesalpino （1596）, and Simeone Maioli （1597）.     

Long-lived transpression in the Archean Bird River greenstone belt, western Superior Province, Southeastern Manitoba

The Archean Bird River greenstone belt (BRGB) is located on the southwestern edge of the Superior Province between the 3.2 Ga old Winnipeg River subprovince to the south and the metasedimentary belt of the English River subprovince (ERSP) to the north. This position between two major subprovinces makes the BRGB a primary target for investigating the geodynamic and kinematic evolution of a major structural boundary. New structural and geochronological data have allowed us to present an evolutionary framework for the southern boundary of the North Caribou superterrane. The BRGB underwent 3 main deformation phases. The D1 event took place ca. 2698 Ma and displays a north-side-up shearing. The D2 event, occurring at ca. 2684 Ma in a transpressive context, presents a complex structural pattern mixing vertical tectonics in the BRGB and strike-slip tectonics along the boundaries of the greenstone belt with other subprovinces. Between the BRGB and the ERSP, the 2832–2858 Ma old Maskwa batholith acted as a rigid passive block during the collision and marks the boundary between pure dextral strike-slip tectonics along his northern boundary with the ERSP and vertical south-side-up motion in the BRGB. The BRGB can be considered as a pop-up structure with anastomosed shear zones displaying different horizontal offset according to the orientation of the shear zones. The southern boundary with the Winnipeg River subprovince is represented by a sinistral south-side-up shear zone. The same pattern is found at the regional scale where major shear zones acted as a conjugate set in the horizontal plane. At ca. 2640 Ma, the D3 event occurred in a general dextral transpressive tectonic regime coeval with the emplacement of rare-elements pegmatitic plutons in a still hot (400–500 °C) country rock. The geodynamical and mechanical significance of the partitioning between pure strike-slip tectonics in the English River subprovince and vertical motion in the BRGB can be explained by the rheological behaviour of a hot and weak lithosphere undergoing transpressive strain. The structural framework of the BRGB is the result of strong interactions between hot and weak domains, coeval with widespread plutonism, and a rigid older domain (Maskwa batholith) during the D2 transpressive event.     

基于自动安置排列的多道面波分析方法

横波速度由于更能直接反映岩石的物理性质,从而在许多工程、环境和地下水勘查中有重要作用.多道面波分析方法(MASW)是一种新技术,通过求得的一维近地表横波速度剖面构建一个二维横波速度场,从而准确探测近地表介质情况.针对该方法数据的采集,提出了一种检波器排列自动安置的技术(自动安置排列),即使用牵引车辆的液压驱动装置在几秒内自动安置几十个检波器,并将其与传统安置排列的方法做了比较,结果表明,自动安置排列技术可用于多道面波分析方法,而且可以大大减少多道面波分析方法的采集时间和费用.     

Radial velocities of pulsating subdwarf B stars: KPD 2109+4401 and PB 8783

High-speed spectroscopy of two pulsating subdwarf B stars, KPD 2109+4401 and PB 8783, is presented. Radial motions are detected with the same frequencies as reported from photometric observations and with amplitudes of ∼2 km s⁻¹ in two or more independent modes. These represent the first direct observations of surface motion arising from multimode non-radial oscillations in subdwarf B stars. In the case of the sdB+F binary PB 8783, the velocities of both components are resolved; high-frequency oscillations are found only in the sdB star and not the F star. There also appears to be evidence for mutual motion of the binary components. If confirmed, it implies that the F-type companion is ≳1.2 times more massive than the sdB star, while the amplitude of the F-star acceleration over 4 h would constrain the orbital period to lie between 0.5 and 3.2 d.     

Prediction of Indoor Air Quality from Soil-Gas Data at Industrial Buildings

Subslab or shallow soil-gas data are often compared with indoor air concentration data in vapor intrusion (VI) evaluations. If no indoor air data are available or confounding sources are present, or if future scenarios are considered, the soil-gas data may be used to estimate the indoor air concentrations due to VI. The typical approach in risk assessments is to use the 95th percentile values from a set of concentration data. For VI studies, however, this rarely is an option because the data sets tend to be quite small. Therefore, various guidance documents urge the use of maximum soil-gas values. This may be reasonable for small residential buildings, but can lead to very conservatively biased estimates if applied to large industrial buildings with localized areas of contamination, especially given that the sampling locations may not be randomly selected and instead are biased toward worst-case locations. By this approach, VI guidance implicitly tolerates a large percentage of false positive decision errors to minimize the number of false negative decision errors. In this paper, implications of using maximum values are discussed and illustrated with data sets from a number of large industrial buildings at various sites. An alternative approach to using maximum soil-gas values is proposed that serves to reduce the number of false positive results while controlling the number of false negatives to an acceptable level.     

Time‐lapse seismic modelling of CO2 fluid substitution in the Devonian Redwater Reef,Alberta, Canada

Common shot ray tracing and finite difference seismic modelling experiments were undertaken to evaluate variations in the seismic response of the Devonian Redwater reef in the Alberta Basin, Canada after replacement of native pore waters in the upper rim of the reef with CO₂. This part of the reef is being evaluated for a CO₂ storage project. The input geological model was based on well data and the interpretation of depth‐converted, reprocessed 2D seismic data in the area. Pre‐stack depth migration of the ray traced and finite difference synthetic data demonstrate similar seismic attributes for the Mannville, Nisku, Ireton, Cooking Lake, and Beaverhill Lake formations and clear terminations of the Upper Leduc and Middle Leduc events at the reef margin. Higher amplitudes at the base of Upper‐Leduc member are evident near the reef margin due to the higher porosity of the foreslope facies in the reef rim compared to the tidal flat lagoonal facies within the central region of the reef. Time‐lapse seismic analysis exhibits an amplitude difference of about 14% for Leduc reflections before and after CO₂ saturation and a travel‐time delay through the reservoir of 1.6 ms. Both the ray tracing and finite difference approaches yielded similar results but, for this particular model, the latter provided more precise imaging of the reef margin. From the numerical study we conclude that time‐lapse surface seismic surveys should be effective in monitoring the location of the CO₂ plume in the Upper Leduc Formation of the Redwater reef, although the differences in the results between the two modelling approaches are of similar order to the effects of the CO₂ fluid replacement itself.     

Modelling the Planetary Nebula

Deep narrow-band imaging and spectroscopy of the Planetary Nebula (PN)surrounding V4334 Sagittarii have been obtained since the onset of thethermal pulse in the star. Although of low surface brightness,narrow-band imaging suggests a ring structure maybepresent. Abundances, expansion rates and physical parameters for thenebula, derived from spectroscopy, show the plasma to be essentiallytypical of old evolved PN (within the errors of observation). The mostrecent data show little evidence of recombination indicating a verylow plasma electron density.Assuming no recombination has occurred, models of the PN spectrum wereconstructed using both simplistic ideas as well as sophisticatedphoto-ionisation codes. These show good agreement, and suggest that thepre-outburst UV radiation field would need to be powered by aprecursor with a surface temperature of T > 10⁵K. The luminosity ofthis star is less well constrained by the models, and cannot be usedsolely to accurately determine its distance. However, by excludingunrealistic models we expect 250 > L/L_odot > 1000 or so. When plotted ona HR diagram for evolved stars this shows good agreement with thatexpected for a pre-last thermal pulse object.