Lifetimes of some excited states in the rare earths: La ii,Ce ii,Pr ii,Nd ii,Sm ii,Yb i,Yb ii,and Lu ii

Radiative lifetimes for excited states in La ii, Ce ii, Pr ii, Nd ii, Sm ii, Yb i, Yb ii, and Lu ii have been determined by means of the beam-foil technique or the zero-field level-crossing method. The lifetimes for La, Ce, Pr, Nd, Sm, and Yb are shorter than those computed by summing the transition probabilities of Corliss and Bozman by a factor of up to ~5. The large discrepancies between the abundance of La, Ce, Pr, Nd, and Sm in the solar photosphere and in meteorites are eliminated or greatly reduced if the abundance determinations of the solar photosphere are based upon the gf values of Corliss and Bozman, corrected for by the present lifetimes.     

Urban fieldwork in geographical education in Levanger,Norway

Despite a long tradition of fieldwork and outdoor education in Norwegian schools, teachers and pupils are not familiar with conducting systematic field studies of modern urban environments. The authors of the present article are convinced that urban fieldwork ought to be included in the teaching syllabus in Norwegian schools, and for several years they have worked on developing urban fieldwork as a part of the study programme in teacher education at Nord-Trøndelag University College (Høgskolen in Nord-Trøndelag or HiNT). The fieldwork element has gradually been expanded, and in recent years pupils from neighbouring primary schools have participated in the programme. The use of ICT has increasingly become an important part of the work in the field as well as in the follow-up phase. Special emphasis has been put on the use of digital stories. The experiences of this work are presented and discussed in the article. In the final section of the article the authors discuss further development of urban fieldwork, paying particular attention to the use of new digital technology and enquiry approaches.     

Odyssey: a solar system mission

The Solar System Odyssey mission uses modern-day high-precision experimental techniques to test the laws of fundamental physics which determine dynamics in the solar system. It could lead to major discoveries by using demonstrated technologies and could be flown within the Cosmic Vision time frame. The mission proposes to perform a set of precision gravitation experiments from the vicinity of Earth to the outer Solar System. Its scientific objectives can be summarized as follows: (1) test of the gravity force law in the Solar System up to and beyond the orbit of Saturn; (2) precise investigation of navigation anomalies at the fly-bys; (3) measurement of Eddington’s parameter at occultations; (4) mapping of gravity field in the outer solar system and study of the Kuiper belt. To this aim, the Odyssey mission is built up on a main spacecraft, designed to fly up to 13 AU, with the following components: (a) a high-precision accelerometer, with bias-rejection system, measuring the deviation of the trajectory from the geodesics, that is also giving gravitational forces; (b) Ka-band transponders, as for Cassini, for a precise range and Doppler measurement up to 13 AU, with additional VLBI equipment; (c) optional laser equipment, which would allow one to improve the range and Doppler measurement, resulting in particular in an improved measurement (with respect to Cassini) of the Eddington’s parameter. In this baseline concept, the main spacecraft is designed to operate beyond the Saturn orbit, up to 13 AU. It experiences multiple planetary fly-bys at Earth, Mars or Venus, and Jupiter. The cruise and fly-by phases allow the mission to achieve its baseline scientific objectives [(1) to (3) in the above list]. In addition to this baseline concept, the Odyssey mission proposes the release of the Enigma radio-beacon at Saturn, allowing one to extend the deep space gravity test up to at least 50 AU, while achieving the scientific objective of a mapping of gravity field in the outer Solar System [(4) in the above list].      

River–aquifer interactions in a semi‐arid environment stressed by groundwater abstraction

Rivers and aquifers are, in many cases, a connected resource and as such the interactions between them need to be understood and quantified for the resource to be managed appropriately. The objective of this paper is to advance the understanding of river–aquifer interactions processes in semi‐arid environments stressed by groundwater abstraction. This is performed using data from a specific catchment where records of precipitation, evapotranspiration, river flow, groundwater levels and groundwater abstraction are analysed using basic statistics, hydrograph analysis and a simple mathematical model to determine the processes causing the spatial and temporal changes in river–aquifer interactions. This combined approach provides a novel but simple methodology to analyse river–aquifer interactions, which can be applied to catchments worldwide. The analysis revealed that the groundwater levels have declined (~ 3 m) since the onset of groundwater abstraction. The decline is predominantly due to the abstraction rather than climatic changes (r = 0.84 for the relationship between groundwater abstraction and groundwater levels; r = 0.92 for the relationship between decline in groundwater levels and magnitude of seasonal drawdown). It is then demonstrated that, since the onset of abstraction, the river has changed from being gaining to losing during low‐flow periods, defined as periods with flow less than 0.5, 1.0 or 1.5 GL/day (1 GL/day = 1 × 10⁶ m³/day). If defined as < 1.0 GL/day, low‐flow periods constitute approximately 65% of the river flows; the periods where the river is losing at low‐flow conditions are thus significant. Importantly, there was a significant delay (> 10 years) between the onset of groundwater abstraction and the changeover from gaining to losing conditions. Finally, a relationship between the groundwater gradient towards the river and the river flow at low‐flow is demonstrated. The results have important implications for water management as well as water ecology and quality. Copyright © 2012 John Wiley & Sons, Ltd.     

Local Stars as Tracers of Galactic Evolution

We describe the overall properties of a new catalogue of metallicities, ages, and galactic orbits for a large, complete sample of F and G dwarfs in the solar neighbourhood. Based on a magnitude-limited sample of ∼ 14000 stars, it is volume-complete to ∼ 40 pc. Together with the astrophysical parameters of direct relevance to models of the evolution of the disk, it will contain the basic photometric, astrometric, and radial velocity data from which they are derived. Information on duplicity is also included. The full exploitation of the data will require a lengthy analysis, in particular to assess the degree of completeness of subsamples of stars of different population types. An early result on the effects of diffusion of galactic orbits in the disk – essential for understanding the scatter in the age-metallicity diagram and estimating the birth radius of stars – is briefly illustrated. This revised version was published online in July 2006 with corrections to the Cover Date.     

Glacial Geomorphologic Maps of Llanquihue Drift in the Area of the Southern Lake District, Chile

We present four glacial geomorphic maps of Llanquihue drift in the region of the southern Lake District, Seno Reloncaví, and the eastern half of northern Isla Grande de Chiloé, Chile. These maps form the basis of an interdisciplinary research project to establish a paleoclimate reconstruction of the last glacial cycle in the middle latitudes of the Southern Hemisphere. Therefore we stressed morphologic rather than lithologic units in our mapping program in order to delineate the glacial geomorphic forms that are surface manifestations of former ice-marginal fluctuations. The resulting maps show the lobate shape and low surface slopes of the former piedmont glaciers that, at the last glacial maximum, spread westward from the Andes into the Valle Centralto fill Lago Puyehue, Lago Rupanco, Lago Llanquihue, Seno Reloncaví, Golfo de Ancud, and northern Gulfo Corcovado. These maps are the framework to tie together in this volume the stratigraphic sections and radiocarbon samples from within the Llanquihue moraine belts as well as the pollen cores from surface mires on the belts.     

The science case of the PEPSI high‐resolution echelle spectrograph and polarimeter for the LBT

We lay out the scientific rationale for and present the instrumental requirements of a high‐resolution adaptiveoptics Echelle spectrograph with two full‐Stokes polarimeters for the Large Binocular Telescope (LBT) in Arizona. Magnetic processes just like those seen on the Sun and in the space environment of the Earth are now well recognized in many astrophysical areas. The application to other stars opened up a new field of research that became widely known as the solarstellar connection. Late‐type stars with convective envelopes are all affected by magnetic processes which give rise to a rich variety of phenomena on their surface and are largely responsible for the heating of their outer atmospheres. Magnetic fields are likely to play a crucial role in the accretion process of T‐Tauri stars as well as in the acceleration and collimation of jet‐like flows in young stellar objects (YSOs). Another area is the physics of active galactic nucleii (AGNs) , where the magnetic activity of the accreting black hole is now believed to be responsible for most of the behavior of these objects, including their X‐ray spectrum, their notoriously dramatic variability, and the powerful relativistic jets they produce. Another is the physics of the central engines of cosmic gamma‐ray bursts, the most powerful explosions in the universe, for which the extreme apparent energy release are explained through the collimation of the released energy by magnetic fields. Virtually all the physics of magnetic fields exploited in astrophysics is somehow linked to our understanding of the Sun's and the star's magnetic fields. (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)