The World of Private Banking Cassis, Youssef; Cottrell, Philip; Fraser, Iain L.
2009, 20161205, 2013, 2009-11-01, 2016-12-05, 2016-11-08
eBook
This is a full and authoritative account of the history of private banking, beginning with its development in conjunction with the world markets served by and centred on a few European cities, ...notably Amsterdam and London. The study details the way in which private banking adapted to the age of the corporate economy from the 1870s to the 1930s, the decline during and after the Great Depression and the post-war renaissance. It concludes with an appraisal of the causes and consequences of the modern expansion of private banking. No longer the exclusive preserve of partnerships, the management of investment portfolios of wealthy individuals and institutions is now a major concern of international joint-stock banks.
The development of native-like HIV-1 envelope (Env) trimer antigens has enabled the induction of neutralizing antibody (NAb) responses against neutralization-resistant HIV-1 strains in animal models. ...However, NAb responses are relatively weak and narrow in specificity. Displaying antigens in a multivalent fashion on nanoparticles (NPs) is an established strategy to increase their immunogenicity. Here we present the design and characterization of two-component protein NPs displaying 20 stabilized SOSIP trimers from various HIV-1 strains. The two-component nature permits the incorporation of exclusively well-folded, native-like Env trimers into NPs that self-assemble in vitro with high efficiency. Immunization studies show that the NPs are particularly efficacious as priming immunogens, improve the quality of the Ab response over a conventional one-component nanoparticle system, and are most effective when SOSIP trimers with an apex-proximate neutralizing epitope are displayed. Their ability to enhance and shape the immunogenicity of SOSIP trimers make these NPs a promising immunogen platform.
With the introduction of the euro much recent attention has been focused on the role of currencies and their national and international significance. Whilst much has been made of the euro's ...achievements in harmonising Europe's financial dealings, it is often forgotten that it is by no means the first pan-national currency to enter circulation. Indeed, as the various contributions to this volume make plain, the euro can in many ways be regarded as a step 'back to the future', that is, a further international currency in a long historical tradition that includes the Athenian tetradrachm, the Spanish peso and the French franc. Covering a timespan of some two and a half millennia, the contributions within this volume fall within four broad chronological sections, the first comprising three contributions that consider aspects of the European experience from classical antiquity until the high middle ages. The discussion then leaps forward chronologically to the modern age, given a focus by three contributions devoted to nineteenth-century European developments. These, in turn, are set within a wider spatial perspective by two essays that review, first, the classical gold standard, primarily in terms of peripheral economies' experience, and, second, the Bretton Woods system. Fourth, and lastly, the euro's origins and birth are explored in three further contributions. By taking such a long term view of supra-national currencies, this volume provides a unique perspective, not only to the introduction and development of the euro, and its predecessors, but also on the broader question of the relationship between trade and common currencies.
We investigate the relationship between sulfur and oxygen fugacity at Erta Ale and Masaya volcanoes. Oxygen fugacity was assessed utilizing Fe3+/∑Fe and major element compositions measured in ...olivine‐hosted melt inclusions and matrix glasses. Erta Ale melts have Fe3+/∑Fe of 0.15–0.16, reflecting fO2 of ΔQFM 0.0 ± 0.3, which is indistinguishable from fO2 calculated from CO2/CO ratios in high‐temperature gases. Masaya is more oxidized at ΔQFM +1.7 ± 0.4, typical of arc settings. Sulfur isotope compositions of gases and scoria at Erta Ale (δ34Sgas − 0.5‰; δ34Sscoria + 0.9‰) and Masaya (δ34Sgas + 4.8‰; δ34Sscoria + 7.4‰) reflect distinct sulfur sources, as well as isotopic fractionation during degassing (equilibrium and kinetic fractionation effects). Sulfur speciation in melts plays an important role in isotope fractionation during degassing and S6+/∑S is <0.07 in Erta Ale melt inclusions compared to >0.67 in Masaya melt inclusions. No change is observed in Fe3+/∑Fe or S6+/∑S with extent of S degassing at Erta Ale, indicating negligible effect on fO2, and further suggesting that H2S is the dominant gas species exsolved from the S2−‐rich melt (i.e., no redistribution of electrons). High SO2/H2S observed in Erta Ale gas emissions is due to gas re‐equilibration at low pressure and fixed fO2. Sulfur budget considerations indicate that the majority of S injected into the systems is emitted as gas, which is therefore representative of the magmatic S isotope composition. The composition of the Masaya gas plume (+4.8‰) cannot be explained by fractionation effects but rather reflects recycling of high δ34S oxidized sulfur through the subduction zone.
Key Points
Oxygen fugacity is buffered during degassing of basalts
Sulfur isotope fractionation is an equilibrium and kinetic process
Sulfur isotopes of arc gases indicate contribution from subducted sulfate
Abstract
The prototype star for the γ Doradus class of pulsating variables was studied employing photometric and spectroscopic observations to determine the frequencies and modes of pulsation. The ...four frequencies found are self-consistent between the observation types and almost identical to those found in previous studies (1.3641 d−1, 1.8783 d−1, 1.4742 d−1, and 1.3209 d−1). Three of the frequencies are classified as l, m = (1, 1) pulsations and the other is ambiguous between l, m = (2, 0) and (2, −2) modes. Two frequencies are shown to be stable over 20 yr since their first identification. The agreement in ground-based work makes this star an excellent calibrator between high-precision photometry and spectroscopy with the upcoming TESS observations and a potential standard for continued asteroseismic modelling.
Giant branch stars in the globular clusters NGC 362 and NGC 6388 were analysed for key s- and r-process element abundances. The NGC 362 stars showed comparable enhancements in the light and heavy ...s-process elements for the sample of 13 giant stars with values of 〈l s/Fe〉= 0.32 ± 0.10 dex and 〈h s/Fe〉= 0.46 ± 0.09 dex. The small spread in these values, as well as in the derived metallicity values (〈Fe/H〉=−1.21 ± 0.09 dex), confirms the homogeneity of these elements in NGC 362. The two stars analysed in NGC 6388 showed enhancements in the light and heavy s-process elements with values of 〈l s/Fe〉= 0.58 ± 0.13 dex and 〈h s/Fe〉= 0.39 ± 0.07 dex. The light s-process elements are more enhanced in this metal-rich cluster compared to the heavy s-process elements. The derived metallicity was in good agreement between the two stars with the mean value for the cluster of 〈Fe/H〉=−0.60 ± 0.02 dex. Due to the similar metallicity of NGC 6388 with 47 Tuc, these two stars were compared with the results from Worley et al. where giant branch stars in 47 Tuc were analysed. The heavy element enhancements between the two clusters were found to be very similar indicating that the relative enhancements of ls and hs elemental abundances is metallicity dependent. When comparing the three clusters, there is a distinct trend of decreasing ls abundance with decreasing metallicity. The hs abundances are essentially the same within their respective uncertainties. This is reflected in the hs/ls ratio for the three clusters. The ratio is very similar for NGC 6388 and 47 Tuc (〈h s/l s〉=−0.18 ± 0.06 dex and 〈h s/l s〉=−0.13 ± 0.05 dex, respectively), but for NGC 362 the ratio is much higher (〈h s/l s〉=+0.14 ± 0.03 dex). The small spread of derived neutron-capture elemental abundance values for all three clusters confirms that these asymptotic giant branch stars are not undergoing third dredge-up and so are not producing the observed s-process enhancements internally.
We have determined stellar parameters and abundances for 221 giant branch stars in the globular cluster ω Centauri. A combination of photometry and lower resolution spectroscopy was used to determine ...temperature, gravity, metallicity, C/Fe, N/Fe and Ba/Fe. These abundances agree well with those found by previous researchers and expand the analysed sample of the cluster. k-means clustering analysis was used to group the stars into four homogeneous groups based upon these abundances.
These stars show the expected anticorrelation between C/Fe and N/Fe. We investigated the distribution of CN-weak/CN-strong stars on the colour-magnitude diagram. Asymptotic giant branch stars, which were selected from their position on the colour-magnitude diagram, were almost all CN weak. This is in contrast to the red giant branch where a large minority were CN strong. The results were also compared with cluster formation and evolution models. Overall, this study shows that statistically significant elemental and evolutionary conclusions can be obtained from lower resolution spectroscopy.
We present the effective temperatures, surface gravities and abundances of iron, carbon and barium of 848 giant branch stars, of which 557 also have well-defined nitrogen abundances, of the globular ...cluster ω Centauri. This work used photometric sources and lower resolution spectra for this abundance analysis. Spectral indices were used to estimate the oxygen abundance of the stars, leading to a determination of whether a particular star was oxygen rich or oxygen poor.
The 557-star subset was analysed in the context of evolutionary groups, with four broad groups identified. These groups suggest that there were at least four main periods of star formation in the cluster. The exact order of these star formation events is not yet understood.
These results compare well with those found at higher resolution and show the value of more extensive lower resolution spectral surveys. They also highlight the need for large samples of stars when working with a complex object like ω Cen.
We carried out an extensive observational study of the Slowly Pulsating B (SPB) star, HD 25558. The 2000 spectra obtained at different observatories, the ground-based and MOST satellite light curves ...revealed that this object is a double-lined spectroscopic binary with an orbital period of about nine years. The observations do not allow the inference of an orbital solution. We determined the physical parameters of the components, and found that both lie within the SPB instability strip. Accordingly, both show line-profile variations due to stellar pulsations. 11 independent frequencies were identified in the data. All the frequencies were attributed to one of the two components based on pixel-by-pixel variability analysis of the line profiles. Spectroscopic and photometric mode identification was also performed for the frequencies of both stars. These results suggest that the inclination and rotation of the two components are rather different. The primary is a slow rotator with 6 d period, seen at 60° inclination, while the secondary rotates fast with 1.2 d period, and is seen at 20° inclination. Spectropolarimetric measurements revealed that the secondary component has a magnetic field with at least a few hundred Gauss strength, while no magnetic field can be detected in the primary.
Abstract
It has been well established that Galactic Globular clusters (GCs) harbour more than one stellar population, distinguishable by the anticorrelations of light-element abundances (C–N, Na–O, ...and Mg–Al). These studies have been extended recently to the asymptotic giant branch (AGB). Here, we investigate the AGB of NGC 6397 for the first time. We have performed an abundance analysis of high-resolution spectra of 47 red giant branch (RGB) and eight AGB stars, deriving Fe, Na, O, Mg, and Al abundances. We find that NGC 6397 shows no evidence of a deficit in Na-rich AGB stars, as reported for some other GCs – the subpopulation ratios of the AGB and RGB in NGC 6397 are identical, within uncertainties. This agrees with expectations from stellar theory. This GC acts as a control for our earlier work on the AGB of M4 (with contrasting results), since the same tools and methods were used.
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