Sodium abundances in nearby disk stars

We present sodium abundances for a sample of nearby stars. All results have been derived from NLTE statistical equilibrium calculations. The influence of collisional interactions with electrons and hydrogen atoms is evaluated by comparison of the solar spectrum with very precise fits to the Na I line cores. The NLTE effects are more pronounced in metal-poor stars since the statistical equilibrium is dominated by collisions of which at least the electronic component is substantially reduced. The resulting influence on the determination of sodium abundances is in a direction opposite to that found previously for Mg and Al. The NLTE corrections are about -0.1 in thick-disk stars with [Fe/H] about -0.6. Our [Na/Fe] abundance ratios are about solar for thick- and thin-disk stars. The increase in [Na/Fe] as a function of [Fe/H] for metal-rich stars found by Edvardsson et al. (1993) is confirmed. Our results suggest that sodium yields increase with the metallicity, and quite large amounts of sodium may be produced by AGB stars. We find that [Na/Fe]ratios, together with either [Mg/Fe] ratio, kinematic data or stellar evolutionary ages, make possible the individual discrimination between thin- and thick-disk membership.Comment: 11pages, 11 figures. A&A accepte

Non-LTE line formation for heavy elements in four very metal-poor stars

Stellar parameters and abundances of Na, Mg, Al, K, Ca, Sr, Ba, and Eu are determined for four very metal-poor stars (-2.66 < [Fe/H] < -2.15) based on non-LTE line formation and analysis of high-resolution (R ~60000 and 90000) high signal-to-noise (S/N > 200) observed spectra. A model atom for H I is presented. An effective temperature was obtained from the Balmer Halpha and Hbeta line wing fits, the surface gravity from the Hipparcos parallax if available and the non-LTE ionization balance between Ca I and Ca II. Based on the hyperfine structure affecting the Ba II resonance line, the fractional abundance of the odd isotopes of Ba was derived for HD 84937 and HD 122563 from a requirement that Ba abundances from the resonance line and subordinate lines of Ba II must be equal. For each star, non-LTE leads to a consistency of Teff from two Balmer lines and to a higher temperature compared to the LTE case, by up to 60 K. Non-LTE effects are important in spectroscopic determination of surface gravity from Ca I/Ca II. For each star with a known trigonometric gravity, non-LTE abundances from the lines of two ionization stages agree within the error bars, while a difference in the LTE abundances consists of 0.23 dex to 0.40 dex for different stars. Departures from LTE are found to be significant for the investigated atoms, and they strongly depend on stellar parameters. For HD 84937, the Eu/Ba ratio is consistent with the relative solar system r-process abundances, and the fraction of the odd isotopes of Ba, f_odd, equals 0.43+-0.14. The latter can serve as a constraint on r-process models. The lower Eu/Ba ratio and f_odd = 0.22+-0.15 found for HD 122563 suggest that the s-process or the unknown process has contributed significantly to the Ba abundance in this star.Comment: accepted for publication in A&A, November 16, 200

First Stars II. Elemental abundances in the extremely metal-poor star CS 22949--037: A diagnostic of early massive supernovae

CS 22949--037 is one of the most metal-poor giants known ([Fe/H]$\approx-4.0$), and it exhibits large overabundances of carbon and nitrogen (Norris et al.). Using VLT-UVES spectra of unprecedented quality, regarding resolution and S/N ratio, covering a wide wavelength range (from $\lambda = 350$ to 900 nm), we have determined abundances for 21 elements in this star over a wide range of atomic mass. The major new discovery is an exceptionally large oxygen enhancement, [O/Fe] $= 1.97\pm0.1$, as measured from the [OI] line at 630.0 nm. We find an enhancement of [N/Fe] of $2.56\pm 0.2$, and a milder one of [C/Fe] $= 1.17\pm$0.1, similar to those already reported in the literature. This implies $Z_{\star}=0.01 Z_{\odot}$. We also find carbon isotopic ratios $^{12}$C/$^{13}$C$=4\pm2.0$ and $^{13}$C/$^{14}$N$=0.03 ^{+0.035}_{-0.015}$, close to the equilibrium value of the CN cycle. Lithium is not detected. Na is strongly enhanced ([Na/Fe] $= +2.1 \pm 0.2$), while S and K are not detected. The silicon-burning elements Cr and Mn are underabundant, while Co and Zn are overabundant ([Zn/Fe]$= +0.7$). Zn is measured for the first time in such an extremely metal-poor star. The abundances of the neutron-capture elements Sr, Y, and Ba are strongly decreasing with the atomic number of the element: [Sr/Fe] $\approx +0.3$, [Y/Fe] $\approx -0.1$, and [Ba/Fe] $\approx -0.6$. Among possible progenitors of CS 22949--037, we discuss the pair-instability supernovae. Such very massive objects indeed produce large amounts of oxygen, and have been found to be possible sources of primary nitrogen. Other scenarios are also discussed. A 30-40$M_{\odot}$ supernova, with fallback, seems the most likely progenitor for CS 22949--037.Comment: 12 Pages, 10 figures, accepted for publication in Astronomy and Astrophysic

Chemical gradients in the Milky Way from the RAVE data

Aims. We aim at measuring the chemical gradients of the elements Mg, Al, Si, and Fe along the Galactic radius to provide new constraints on the chemical evolution models of the Galaxy and Galaxy models such as the Besancon model. Thanks to the large number of stars of our RAVE sample we can study how the gradients vary as function of the distance from the Galactic plane. Methods. We analysed three different samples selected from three independent datasets: a sample of 19 962 dwarf stars selected from the RAVE database, a sample of 10 616 dwarf stars selected from the Geneva-Copenhagen Survey (GCS) dataset, and a mock sample (equivalent to the RAVE sample) created by using the GALAXIA code, which is based on the Besancon model. The three samples were analysed by using the very same method for comparison purposes. We integrated the Galactic orbits and obtained the guiding radii (R-g) and the maximum distances from the Galactic plane reached by the stars along their orbits (Z(max)). We measured the chemical gradients as functions of R-g at different Z(max). Results. We found that the chemical gradients of the RAVE and GCS samples are negative and show consistent trends, although they are not equal: at Z(max) < 0.4 kpc and 4.5 < R-g(kpc) < 9.5, the iron gradient for the RAVE sample is d[Fe/H]/dR(g) = -0.065 dex kpc(-1), whereas for the GCS sample it is d[Fe/H]/dR(g) = -0.043 dex kpc(-1) with internal errors of +/-0.002 and +/-0.004 dex kpc(-1), respectively. The gradients of the RAVE and GCS samples become flatter at larger Z(max). Conversely, the mock sample has a positive iron gradient of d[Fe/H]/dR(g) = +0.053 +/- 0.003 dex kpc(-1) at Z(max) < 0.4 kpc and remains positive at any Z(max). These positive and unrealistic values originate from the lack of correlation between metallicity and tangential velocity in the Besancon model. In addition, the low metallicity and asymmetric drift of the thick disc causes a shift of the stars towards lower R-g and metallicity which, together with the thin-disc stars with a higher metallicity and R-g, generates a fictitious positive gradient of the full sample. The flatter gradient at larger Z(max) found in the RAVE and the GCS samples may therefore be due to the superposition of thin-and thick-disc stars, which mimicks a flatter or positive gradient. This does not exclude the possibility that the thick disc has no chemical gradient. The discrepancies between the observational samples and the mock sample can be reduced by i) decreasing the density; ii) decreasing the vertical velocity; and iii) increasing the metallicity of the thick disc in the Besancon model

The Hamburg/ESO R-process Enhanced Star survey (HERES) III. HE 0338-3945 and the formation of the r+s stars

We have derived abundances of 33 elements and upper limits for 6 additional elements for the metal-poor ([Fe/H] = -2.42) turn-off star HE 0338-3945 from high-quality VLT-UVES spectra. The star is heavily enriched, by about a factor of 100 relative to iron and the Sun, in the heavy s-elements (Ba, La, ..). It is also heavily enriched in Eu, which is generally considered an r-element, and in other similar elements. It is less enriched, by about a factor of 10, in the lighter s-elements (Sr, Y and Zr). C is also strongly enhanced and, to a somewhat lesser degree, N and O. These abundance estimates are subject to severe uncertainties due to NLTE and thermal inhomogeneities which are not taken into detailed consideration. However, an interesting result, which is most probably robust in spite of these uncertainties, emerges: the abundances derived for this star are very similar to those of other stars with an overall enhancement of all elements beyond the iron peak. We have defined criteria for this class of stars, r+s stars, and discuss nine different scenarios to explain their origin. None of these explanations is found to be entirely convincing. The most plausible hypotheses involve a binary system in which the primary component goes through its giant branch and asymptotic giant branch phases and produces CNO and s-elements which are dumped onto the observed star. Whether the r-element Eu is produced by supernovae before the star was formed (perhaps triggering the formation of a low-mass binary), by a companion as it explodes as a supernova (possibly triggered by mass transfer), or whether it is possibly produced in a high-neutron-density version of the s-process is still unclear. Several suggestions are made on how to clarify this situation.Comment: Accepted for A&A; 22 pages, 9 figures, 2 tables. Table 2 is in electronic form and available at http://www.astro.uu.se/~karin/table2.dat with description at http://www.astro.uu.se/~karin/jonsellReadMe

Innovative Business Approaches for the Reduction of Extreme Poverty and Marginality?

Extreme poverty is an immense political and market failure, wasting the potential of hundreds of millions of people. Investing in the creation of markets that include the extreme poor and marginalized should thus not only be considered as a charitable activity, but promises high returns on investments - in financial and humanitarian terms. However, while the potential of innovative business approaches to target the poor that live close to the poverty line is increasingly being recognised, the question remains how far these approaches can push the margin to also include those that are extremely poor. And how can those that are marginalized from development opportunities be brought into and benefit from market-based systems to improve the quality of their lives? The impressive rise of business approaches to combating poverty stems from a long history of debates on the role of businesses in society. From an initial focus on social objectives as an external add-on, leading business thinkers have increasingly been stressing the benefits for companies of integrating social considerations into their core business strategies, for instance by targeting lowincome consumers (or 'bottom of the pyramid' markets) or strengthening supply and distribution chains through the involvement of local communities as part of inclusive business strategies. Others - most notably Muhammed Yunus along with other social entrepreneurs - are taking this argument one step further, advocating the use of business strategies primarily to address social goals rather than for financial gains. Thus, in discussions on the role of business in society, profit maximisation as the primary objective of business operations is increasingly making way for business initiatives that are guided by social objectives. This trend is also being supported by growing interest among investors in financing enterprises that promote social or environmental objectives, either as their primary aim or in parallel with seeking to generate financial returns. How suitable these different approaches are to engage the poorest and marginalized depends in part on the extent to which they are able to involve the extreme poor themselves, their flexibility to direct business objectives towards the reduction of extreme poverty and marginality, and their ability to successfully operate with non-business public and civil society partners and in sectors of particular interest to the extreme poor. Further research and action is needed to identify outcome-focused indicators and measurement tools for social value creation, examine possible government measures to support business activities for the poorest, and consider complementarities between the different business approaches. While we recognise that it is unrealistic to expect businesses to be able to reach all of the extreme poor, we believe that the boundaries of innovative business operations can be pushed much further to include a far larger number of the poorest and marginalized

Marginality: Addressing the Root Causes of Extreme Poverty

The need to address extreme poverty from the perspective of marginality arises from the frustration that the number of the poorest and hungry remains unacceptably high. This triggered the call for an innovative approach from the side of science and action. The conceptual and analytical framework developed here views marginality as a root cause of extreme poverty. We define marginality as an involuntary position and condition of an individual or group at the edge of social, economic, and ecological systems, preventing the access to resources, assets, services, restraining freedom of choice, preventing the development of capabilities, and causing extreme poverty. Causal complexes tie the marginalized poor in systems from which they want to escape or in which they want to improve their lives. The rural and agricultural context is of particular relevance here, as we assume that large segments of the extreme poor live in rural areas. The poorest themselves have described their situation, for instance, as being trapped in a 'complex knot which can lead to further knots if the wrong threads are pulled.' While poverty is objectively a matter of absolute deficiencies, we explain why the way in which poverty is perceived by the poor themselves requires looking at poverty as a relative, subjective, dynamic and systemic phenomenon. We conceptualize marginality as patterns of causal complexes in societal and spatial dimensions. These causal complexes can, for instance, comprise different types of livelihood systems or different types of poverty traps. They include proximate as well as underlying causes of extreme poverty and specifically address social exclusion, restrained access to assets, opportunities and transport, communication and public services infrastructure. An analytical framework is developed, outlining the various steps required for the analysis of marginality in a systematic, re&#x0081;]iterative and participatory manner, involving those affected by extreme poverty themselves. From each causal complex of marginality, leverage points can be identified which match with specific intervention packages, relevant for livelihood management, policy formulation and implementation. The approach to the investigation of extreme poverty is applied and relevant for managing change towards inclusive development. Points of entry for public and private investments are being identified

Baugruppen und Werkstoffe für eine Heißwandanlage zur Züchtung von Galliumarsenid-Einkristallen

Basic investigations to seal a hot-wall crystal pulling vessel against Arsen vapour leakage have been carried out. The wall material under investigation was either quartz or metal. The corrosion behaviour of metals, alloys, protective coatings and ceramics at 700°C against As-vapour has been examined. Based an these experiments, technically feasible solutions for disconnectable (langes out of different materials have been developed. Also, a valve is presented, that can be operatedat 700°C and which is leaktied in an As-vapour environment

FOCES - a fibre optics Cassegrain échelle spectrograph

We have designed and built the éch elle spec tro graph FOCES fed by $100~\mu$m optical fibres to be mounted at the Cassegrain focus of either the 2.2 m or the 3.5 m telescope at the Calar Alto Observatory. The spec tro graph itself follows a white-pupil design collimated with two off-axis parabolic mirrors. The 15 cm beam leaving the 31.6 lines/mm R2 éch elleis refocussed in the vicinity of a small folding mirror which allows efficient removal of scattered light. The cross-dispersion is achieved with a tandem prism mounting, and the beam imaged with an $f/3$ transmission camera onto a field centered on a 10242 thinned Tektronix CCD with $24~\mu$m pixel diameter. The éch elleimage covers the visible spectral region from 380 to 750 nm displayed in 70 spectral orders with full spectral coverage. Spectral orders are separated by 20 pixels in the blue and by 10 pixels in the red. The maximum spectral resolution is $R = \lambda / \Delta\lambda\ = 40600$ with a 2 pixel resolution element; unvignetted resolution as defined by the fibre alone would be obtained at $R = 18000$. Replacing the CCD by a 20482 chip with $15~\mu$m pixel diameter and taking into account light losses from a reduced entrance slit width a full 2 pixel resolution of $R = 65000$ is obtained. The above concept has made FOCES an extremely well-defined instrument. A number of successful test installations at the Cassegrain foci of the Wendelstein 80 cm telescope, the Calar Alto 2.2 m and 3.5 m telescopes has produced spectra of high quality for up to 60 min exposures. The limiting magnitude for a 1 hr exposure with an $S/N$ ratio of 100 scales to $V = 12$ for a 3.5 m telescope which is only slightly less than expected from laboratory tests. In an alternative mode FOCES offers a second fibre carrying the sky background signal to correct extremely faint object spectra. This mode obtains the required higher cross-dispersion from an additional grism resulting in a correspondingly reduced spectral coverage