The density distribution of the Galactic stellar halo as traced by blue horizontal branch stars

Data of blue horizontal branch (BHB) stars and RR Lyrae variable stars from the literature are combined with unpublished observations of BHB stars in five fields. A flattened power law is used to model the spatial distribution of the horizontal branch stars. Completeness of the data sample and contamination by blue stragglers and metal-rich main-sequence A stars are considered, and taken into account. Using a maximum-likelihood method, the following best-fitting parameters are obtained: a power-law index α=−3.2±0.3 and an axial ratio of q =0.52±0.11 for the isodensity surfaces. From the fit a value for the local density of BHB stars of ρ₀=26⁺²⁰₋₁₁ kpc⁻³ is found. The values of the three parameters are in complete agreement with recent determinations by other authors.     

Numerical simulations of rotating cooling flows in galaxy cluster environments

We have used 2D numerical simulations to study the evolution of galaxy cluster cooling flows undergoing a rotational perturbation. We show that such rotations in the intracluster medium may arise from cluster/subcluster mergers. Our galaxy cluster initial conditions involve spherically symmetric, steady-state cooling flows with varying mass-dropout strengths. The rotational perturbation serves to break the symmetry for each of the initial cooling flows, resulting in the formation of thin, gaseous disc-like structure extending radially out to ∼10 kpc. Disc-like structure formed for low mass-dropout strength simulations appears to contain cooling condensations whereas disc-like structure in higher mass-dropout strength simulations appears smooth. This is due to the influence of mass-dropout on the degree of cooling, which serves to reduce the strength of thermal instabilities by the removal of 'cold' gas from the flow. Morphological comparisons of the disc-like structure formed in our simulations are made to structure observed in the X-ray emitting gas of A4059. Comparisons of the gas dynamics within the disc-like structure are also made to the solid-body rotation profile observed from emission-line gas within the central galaxy of Hydra A. The influence of grid effects on the simulations is also discussed.     

Fourteen years of multifrequency-coordinated observations of the X-ray/Be system A 0535+26/HDE 245770

Within the framework of a very long multifrequency campaign of coordinated, and very often simultaneous, observations of the transient X-ray/Be system A 0535+26/HDE 245770, we present a summary of this large collection of data taken with IUE and ASTRON satellites as well as with many ground-based telescopes in optical and IR regions.In this paper we emphasize the study of the physics and dynamics of the mass transfer at periastron and subsequent X-ray flaring, which is a typical problem of the X-ray/Be binary system class.Paper presented at the 11th European Regional Astronomical Meetings of the IAU on New Windows to the Universe, held 3–8 July, 1989, Tenerife, Canary Islands, Spain.     

Coherent propagation of non-relativistic solar electrons

An experimental study of the propagation of solar electrons with energyE _e > 30 keV was carried out. Measurements were made during the period 1972-1974 using the Prognoz satellite-borne instruments.A two-component structure of electron fluxes was found. The fast component, rather well-observed after solar flares of minor importance, consists of a compact beam of electrons propagating without scattering inside a narrow cone with an opening 10° along interplanetary magnetic field lines. Characteristics of this component are given.Peculiarities of the slow or diffusive component of electron fluxes are compared with the diffusive component of solar protons. It is shown that the diffusion coefficient for non-relativistic electrons is the function of the number of particles injected in the event. A model of coherent propagation of non-relativistic electrons is offered, which takes into account the presence of the fast and slow components and their interaction with solar wind plasma oscillations.     

Diatom paleoecology of Laguna Zoncho,Costa Rica

We analyzed diatoms in a sediment profile from Laguna Zoncho in southern Pacific Costa Rica (lake elevation 1190 m asl, depth 2.6 m, area 0.75 ha) spanning some 3240 cal yr. Diatoms are common in the profile, which we subdivide into three zones. Zone C (3240–1020 cal yr B.P.) is dominated by Staurosira construens var. venter and Aulacoseira spp.; during this time, the lake was dilute and circumneutral. Benthic and acidophilous taxa increase gradually in the upper section of this zone. Zone B (1020–460 cal yr B.P.) almost totally lacks Aulacoseira, and instead is dominated by combinations of Eunotia minor, Encyonema lunatum, Gomphonema gracile, and Pinnularia braunii. Previous pollen and charcoal analysis indicates that this zone falls within the peak of prehistoric agricultural activity at the lake, but diatoms may also reflect climate change. During this period, the lake was likely shallower and more acidic, but not eutrophic. Finally, Zone A (460 cal yr B.P. to AD 1997) begins near a 1.5-cm tephra layer from nearby Volcán Barú; diatom assemblages are dominated by Aulacoseira spp., and suggest deepening of the lake and return to conditions similar to Zone C. This was a time of indigenous population decline and forest recovery in the Zoncho region, probably reflecting the impact of European diseases on the native population, although climate change and impacts of the tephra deposition cannot be wholly discounted.     

Comments on thermal isostasy

The deformation of the lithosphere due to temperature anomalies caused by a heat source located below or within the layer is usually modelled as one of Pratt local isostasy. A more appropriate model is one of rheologically layered lithosphere comprising of a stiff viscoelastic or elastic layer overlying a weaker viscoelastic layer. The surface deformations are a result of not only the perturbations in body forces due to density changes, but thermal bending moments. In geophysically realistic situations the former contribution dominates. Pratt isostasy is attained if the stresses in the entire lithosphere are allowed to relax and this end state is not contingent upon the lithosphere being confined against horizontal deformation. In a rheologically layered lithosphere, even though the non-isostatic thermal stresses persist in the upper layer, the surface deformations are indistinguishable from that of local isostasy if the horizontal dimension of the heat source exceeds about three times the effective elastic thickness of the lithosphere.     

A Monte Carlo model for the gardening of the lunar regolith

The processes of movement and turnover of the lunar regolith are described by a Monte Carlo model, which includes the effects of collisions by particles from 10^?7 g to 10¹⁰ g. The movement of material by the direct cratering process is the dominant mode, but slumping is also included for angles exceeding the static angle of repose. Using a group of interrelated computer programs a large number of properties are calculated, including topography, formation of layers, depth of the disturbed layer, nuclear track distributions, cosmogenic nuclides and others. In the most complex program, the history of a 36 point square array is followed for times up to 4 × 10⁸ yr. As expected the histories generated are complex and exhibit great variety. Because a crater covers much less area than its ejecta blanket, there is a tendency for the height change at a test point to exhibit the ‘gambler's ruin’ phenomenon: periods of slow accumulation followed by sudden excavation. In general the agreement with experiment and observation seems good. Two areas of disagreement stand out. First, the calculated surface is rougher than that observed. This problem is understood, and will not occur in a newer version of the model. Second, the observed bombardment ages, of the order of 4 × 10⁸ yr, are shorter than expected (by perhaps a factor of 5). We cannot accept Fireman's (1974) explanation; this remains an important puzzle.     

Treatment of pulsating white dwarfs including general relativistic effects

In this paper, pulsating white dwarfs are treated via general relativity. Numerical integration of Einstein's equations was used to find equilibrium white dwarfs models and the fundamental periods of small oscillations about these equilibrium models. In these calculations account was taken of coulomb, Thomas-Fermi, and exchange interactions as well as ion zero point energies. It is shown that general relativity makes not just a quantitative difference in the results but a qualitative differences; pure C¹² models which are stable in Newtonian mechanics can be unstable against collapse (at a central density of 3×10¹⁰ g/cm³) when general relativity is taken into account. The collapsing model may become a neutron star or may continue towards the Schwarzschild radius.More realistic white dwarf models with carbon burning products at the center, also were studied. For these models, the density at which the star becomes unstable against collapse due to electron capture (3×10⁹ g/cm³) was found to be lower than the density at which general relativistic instability occurs.     

Reliable groundwater management: the continuous improvement method

Over the world, a majority of water resources are managed by small- and medium-sized companies. Despite having limited personnel and financial resources, these companies have to ensure their groundwater management contains adequate quality control. This is an objective that any company can achieve with the means at its disposal, by using the continuous improvement method. In contrast to the technical approaches mainly used, which focus on the aquifer and the groundwater, the method presented in this article is specifically geared towards the individual conditions of the company extracting the water. A method of sustainable groundwater management is steadily built up by starting with the resources a company has available. The advantage of this approach is that any company, with its financial and personal resources, can achieve suitable groundwater by doing as much as it can within the bounds of its possibilities. Instead of calling in expensive external experts for a short period, the continuous improvement method calls at first for the participation of the companys employees and others involved. The aim is, ultimately, for learning organizations to be able to actively develop their own quality assurance strategies. The method introduced also enables a number of different water suppliers to collaborate within a network. Moreover, usage of the same guidelines allows international comparison. The continuous improvement of groundwater quality covers three scopes: groundwater extraction, groundwater protection, and the groundwater management system. In the following, the management system is based on sections from the International Standardization Organization (ISO 9001:2000) international quality management standard. The method is described using the example of mineral water and spa companies, which are often subject to difficult hydrogeological conditions.     

Gravimetria e prospezione della crosta terrestre

Riassunto Richiamandosi al principio secondo il quale fra due superficie equipotenziali la gravità assume un valore determinato, l'A. sviluppa alcune precisazioni sulle ipotesi inerenti alla distribuzione della densità nella crosta terrestre al disotto delle singole stazioni gravimetriche.

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Zusammenfassung Durch Anwendung des Satzes, dass zwischen zwei bestimmten Aequipotentialflächen die Schwere einen bestimmten Wert haben muss, lassen sich die Annahmen über die Dichteverteilung unter dem Beobachtungsort verfeinern.