Gaia-ESO Survey: Analysis of pre-main sequence stellar spectra

Context. The Gaia-ESO Public Spectroscopic Survey is obtaining high-quality spectroscopy of some 100 000 Milky Way stars using the FLAMES spectrograph at the VLT, down to V = 19 mag, systematically covering all the main components of the Milky Way and providing the first homogeneous overview of the distributions of kinematics and chemical element abundances in the Galaxy. Observations of young open clusters, in particular, are giving new insights into their initial structure, kinematics, and their subsequent evolution. Aims. This paper describes the analysis of UVES and GIRAFFE spectra acquired in the fields of young clusters whose population includes pre-main sequence (PMS) stars. The analysis is applied to all stars in such fields, regardless of any prior information on membership, and provides fundamental stellar atmospheric parameters, elemental abundances, and PMS-specific parameters such as veiling, accretion, and chromospheric activity. Methods. When feasible, different methods were used to derive raw parameters (e.g. line equivalent widths) fundamental atmospheric parameters and derived parameters (e.g. abundances). To derive some of these parameters, we used methods that have been extensively used in the past and new ones developed in the context of the Gaia-ESO survey enterprise. The internal precision of these quantities was estimated by inter-comparing the results obtained by these different methods, while the accuracy was estimated by comparison with independent external data, such as effective temperature and surface gravity derived from angular diameter measurements, on a sample of benchmarks stars. A validation procedure based on these comparisons was applied to discard spurious or doubtful results and produce recommended parameters. Specific strategies were implemented to resolve problems of fast rotation, accretion signatures, chromospheric activity, and veiling. Results. The analysis carried out on spectra acquired in young cluster fields during the first 18 months of observations, up to June 2013, is presented in preparation of the first release of advanced data products. These include targets in the fields of the ρ Oph, Cha I, NGC 2264, γ Vel, and NGC 2547 clusters. Stellar parameters obtained with the higher resolution and larger wavelength coverage from UVES are reproduced with comparable accuracy and precision using the smaller wavelength range and lower resolution of the GIRAFFE setup adopted for young stars, which allows us to provide stellar parameters with confidence for the much larger GIRAFFE sample. Precisions are estimated to be ≈120 K rms in Teff, ≈0.3 dex rms in log g, and ≈0.15 dex rms in [Fe/H] for the UVES and GIRAFFE setups.

The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars

Context. The ongoing Gaia-ESO Public Spectroscopic Survey is using FLAMES at the VLT to obtain high-quality medium-resolution Giraffe spectra for about 105 stars and high-resolution UVES spectra for about 5000 stars. With UVES, the Survey has already observed 1447 FGK-type stars. Aims. These UVES spectra are analyzed in parallel by several state-of-the-art methodologies. Our aim is to present how these analyses were implemented, to discuss their results, and to describe how a final recommended parameter scale is defined. We also discuss the precision (method-to-method dispersion) and accuracy (biases with respect to the reference values) of the final parameters. These results are part of the Gaia-ESO second internal release and will be part of its first public release of advanced data products. Methods. The final parameter scale is tied to the scale defined by the Gaia benchmark stars, a set of stars with fundamental atmospheric parameters. In addition, a set of open and globular clusters is used to evaluate the physical soundness of the results. Each of the implemented methodologies is judged against the benchmark stars to define weights in three different regions of the parameter space. The final recommended results are the weighted medians of those from the individual methods. Results. The recommended results successfully reproduce the atmospheric parameters of the benchmark stars and the expected Teff-log  g relation of the calibrating clusters. Atmospheric parameters and abundances have been determined for 1301 FGK-type stars observed with UVES. The median of the method-to-method dispersion of the atmospheric parameters is 55 K for Teff, 0.13 dex for log  g and 0.07 dex for [Fe/H]. Systematic biases are estimated to be between 50−100 K for Teff, 0.10−0.25 dex for log  g and 0.05−0.10 dex for [Fe/H]. Abundances for 24 elements were derived: C, N, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Mo, Ba, Nd, and Eu. The typical method-to-method dispersion of the abundances varies between 0.10 and 0.20 dex. Conclusions. The Gaia-ESO sample of high-resolution spectra of FGK-type stars will be among the largest of its kind analyzed in a homogeneous way. The extensive list of elemental abundances derived in these stars will enable significant advances in the areas of stellar evolution and Milky Way formation and evolution.

The Gaia-ESO Survey: Empirical determination of the precision of stellar radial velocities and projected rotation velocities

Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey at the European Southern Observatory Very Large Telescope. Aims. A key aim is to provide precise radial velocities (RVs) and projected equatorial velocities (vsini) for representative samples of Galactic stars, which will complement information obtained by the Gaia astrometry satellite. Methods. We present an analysis to empirically quantify the size and distribution of uncertainties in RV and vsini using spectra from repeated exposures of the same stars. Results. We show that the uncertainties vary as simple scaling functions of signal-to-noise ratio (S/N) and vsini, that the uncertainties become larger with increasing photospheric temperature, but that the dependence on stellar gravity, metallicity and age is weak. The underlying uncertainty distributions have extended tails that are better represented by Student’s t-distributions than by normal distributions. Conclusions. Parametrised results are provided, which enable estimates of the RV precision for almost all GES measurements, and estimates of the vsini precision for stars in young clusters, as a function of S/N, vsini and stellar temperature. The precision of individual high S/N GES RV measurements is 0.22–0.26 km s-1, dependent on instrumental configuration.

Obama 2: future implications for EU-US relations. Jean Monnet/Robert Schuman Paper Series Vol. 12, No. 8, November 2012

Introduction. The week following his reelection, President Obama traveled to Asia – Thailand, Myanmar, and Cambodia –, while facing at home a fiscal cliff, the need to select the next Secretaries of State, Defense, and Treasury, and the resignation of one of America’s most senior and respected generals and Director of the CIA, David Petraeus; all this at the moment wherein the Middle East is burning in flames due to another round of violence between Israel and Hamas. On the other side of the pond, the EU is currently trying to solve or at least contain several crises: the Eurozone, agreeing on the Multiannual Financial Framework 2014-2020, or MFF 2014-2020,2 and saving France.3 For both giants, the American and European priorities are domestic; they both need to do some ‘nation-building at home.’4 The threat of the fiscal cliff in the US and the one of the Eurocrisis in Europe are too important to be ignored and so visceral that they will affect the way both actors behave internationally and interact with one another. The big question since Obama’s reelection has been what will the EU-US relations look like under his second mandate? And will there be any differences from the first one?5 This paper argues that the US-EU relations will remain quite similar as it was under the first Obama presidency. Nevertheless, with the current shift to Asia, the ‘pivot,’ the EU will be required to increase its contributions to global politics and international security. This paper is structured in three parts. First, the economic and political climax of the EU and the US will be presented. In a second a part, the EU and US strategies and foreign policies will be laid out. Last but not least, several core issues facing the Euro-Atlantic community, such as the Asia pivot, Iran, climate change, and the economy will be addressed. Other issues such as Syria, Afghanistan, and the Middle East and North Africa will not be addressed in this paper.6

Forerunners or scaremongers? Germany to abandon nuclear power. OSW Commentary No. 58, 2011-07-21

The German government’s final decision to abandon nuclear power as of 2022 has been expected for months. However, instead of calming the waters, providing solutions and answering the question ‘What next?’, it has only fanned the flames. Even the adoption of legal amendments enforcing the government’s decision by the German parliament (both the Bundestag and the Bundesrat) in late June and early July has not calmed the situation. It is more than apparent that these decisions have been made under emotional pressure: there was not enough time for accurate calculations to be made and consideration to be given to the consequences of Germany abandoning nuclear power. Chancellor Angela Merkel has so far been unable to fully convince the public that the ‘energy shift is a huge opportunity’ and that this process will be carried out on condition that ‘the supplies remain secure, the climate protected and the whole process economically efficient’1. German economic associations have warned against a politically motivated, ill-judged and irreversible abandonment of nuclear energy. They are anxious about an increase in electricity prices, the instability of supplies and environmental damage. The government believes, however, that green technologies will become a new driving force for the German economy and its main export commodity. Before that happens the industry will have to increase its use of electricity produced from fossil fuels, mainly natural gas imported from Russia. This may be exploited by Gazprom which will try to strengthen its position on the German market, and thus in the entire EU.

spotlight europe #2015/02—July 2015: A Gulf CSC Could Bring Peace and Greater Security to the Middle East

Wars continue to ravage in Syria, Iraq and Yemen. Refugees are wandering around aimlessly in the Middle East with many fleeing to Europe. Saudi Arabia and Iran are adding fuel to the flames. They are vying for supremacy while remaining highly suspicious of each other. A Conference for Security and Cooperation could help to ease existing tensions. Many years ago the CSCE was a resounding success. It could thus serve as a blueprint with the nuclear agreement with Iran as a starting point of such a venture.

Conflicts and online community social capital:the influence of conflict management practices

Conflicts are part and parcel of online community dynamics (De Valck 2007; Harrison and Jenkins 1996; Kozinets 2001) – from flames about publishing inappropriate content (De Zwart and Lindsay 2009) to battles to win high status positions (Campbell, Fletcher and Greenhill 2009) and stigmatization of illegitimate insiders (Tikkanen, Hietanen, Henttonen, and Rokka 2009) up to bashing and smearing campaigns (Bocij 2002). As the concept of community presumes unity, marketers may be inclined to suppress any dissonance in their online brand communities thinking that it may hurt brand image or community attractiveness. However, Fournier and Lee (2009) advise marketers to embrace the conflicts that make communities thrive. As tensions and conflict cannot be avoided this seems logical advice. Nevertheless, are all tensions and conflicts created equally? Are some not more constructive (or destructive) than others? Thus, should all tensions and conflicts really be embraced, and what can be done to channel tensions and conflicts such that they do not become destructive? These questions form the starting point of this paper.

La cinematica nel core dell'ammasso globulare NGC 6266 da osservazioni SINFONI

Lo studio delle regioni più interne degli ammassi globulari risulta fondamentale per la ricerca di buchi neri di massa intermedia (IMBH). La scoperta di tali oggetti avrebbe un impatto sostanziale su un gran numero di problemi astrofisici aperti, dalla formazione dei buchi neri supermassicci, all'interpretazione delle Ultra Luminous X-ray Sources, fino allo studio delle onde gravitazionali. Il presente lavoro di tesi si inserisce all'interno di un progetto osservativo mirato a studiare la dinamica interna degli ammassi globulari e volto ad investigare la presenza di IMBH nel centro di tali sistemi tramite l'analisi sistematica dei profili di dispersione di velocità e di rotazione. In questo elaborato presentiamo lo studio della cinematica del core dell'ammasso globulare NGC 6266, realizzato con lo spettrografo a campo integrale IFU-SINFONI, assistito da un sistema di ottiche adattive. Grazie all'utilizzo dell'ottica adattiva, SINFONI è in grado di realizzare osservazioni ad alta risoluzione spaziale e misurare la velocità radiale di stelle individuali anche nelle regioni più interne degli ammassi globulari, dove le misure spettroscopiche tradizionali falliscono a causa dell'elevato crowding stellare. Questo ci ha permesso di determinare il profilo centrale della dispersione di velocità di NGC 6266 dalla misura delle velocità radiali individuali di circa 400 stelle, localizzate negli 11 arcsec più interni dell'ammasso. Utilizzando dati complementari, provenienti da osservazioni realizzate con lo spettrografo multi-oggetto FLAMES, siamo stati in grado di costruire il profilo di dispersione di velocità di NGC 6266 fino ad una distanza radiale di 250 arcsec. Il profilo di dispersione di velocità osservato permette di escludere la presenza di un IMBH di massa superiore a 2500 masse solari e mostra un calo nella regione centrale, simile a quello rilevato in un numero crescente di ammassi globulari, che potrebbe indicare la presenza di anisotropia tangenziale.

England's Yellow Peril: Sinophobia and the Great War

As England suffered heavy casualties at the front during World War One, the nation closed ranks against outsiders at home. England sought to reaffirm its racial dominance at the heart of the empire, and the Chinese in London became the principal scapegoat for anti-foreign sentiment. A combination of propaganda and popular culture, from the daily paper to the latest theatre sensation, fanned the flames of national resentment into a raging Sinophobia. Opium smoking, gambling and interracial romance became synonymous with London's Limehouse Chinatown, which was exoticised by Sax Rohmer's evil mastermind Fu Manchu and Thomas Burke's tales of lowlife love. England's Yellow Peril exploded in the midst of a catastrophic war and defined the representation of Chinese abroad in the decades to come.

Rotational velocities of single and binary O-type stars in the Tarantula Nebula

Rotation is a key parameter in the evolution of massive stars, affecting their evolution, chemical yields, ionizing photon budget, and final fate. We determined the projected rotational velocity, υ e sin i, of ~330 O-type objects, i.e. ~210 spectroscopic single stars and ~110 primaries in binary systems, in the Tarantula nebula or 30 Doradus (30 Dor) region. The observations were taken using VLT/FLAMES and constitute the largest homogeneous dataset of multi-epoch spectroscopy of O-type stars currently available. The most distinctive feature of the υ e sin i distributions of the presumed-single stars and primaries in 30 Dor is a low-velocity peak at around 100 km s^-1. Stellar winds are not expected to have spun-down the bulk of the stars significantly since their arrival on the main sequence and therefore the peak in the single star sample is likely to represent the outcome of the formation process. Whereas the spin distribution of presumed-single stars shows a well developed tail of stars rotating more rapidly than 300 km s^-1, the sample of primaries does not feature such a high-velocity tail. The tail of the presumed-single star distribution is attributed for the most part - and could potentially be completely due - to spun-up binary products that appear as single stars or that have merged. This would be consistent with the lack of such post-interaction products in the binary sample, that is expected to be dominated by pre-interaction systems. The peak in this distribution is broader and is shifted toward somewhat higher spin rates compared to the distribution of presumed-single stars. Systems displaying large radial velocity variations, typical for short period systems, appear mostly responsible for these differences.

The large- and small-scale Ca IIK structure of the Milky Way from observations of Galactic and Magellanic sightlines

Aims. The large and small-scale (pc) structure of the Galactic interstellar medium can be investigated by utilising spectra of early-type stellar probes of known distances in the same region of the sky. This paper determines the variation in line strength of Ca ii at 3933.661 Å as a function of probe separation for a large sample of stars, including a number of sightlines in the Magellanic Clouds. 

Methods. FLAMES-GIRAFFE data taken with the Very Large Telescope towards early-type stars in 3 Galactic and 4 Magellanic open clusters in Ca ii are used to obtain the velocity, equivalent width, column density, and line width of interstellar Galactic calcium for a total of 657 stars, of which 443 are Magellanic Cloud sightlines. In each cluster there are between 43 and 111 stars observed. Additionally, FEROS and UVES Ca ii K and Na i D spectra of 21 Galactic and 154 Magellanic early-type stars are presented and combined with data from the literature to study the calcium column density - parallax relationship. 

Results. For the four Magellanic clusters studied with FLAMES, the strength of the Galactic interstellar Ca ii K equivalent width on transverse scales from ∼0.05-9 pc is found to vary by factors of ∼1.8-3.0, corresponding to column density variations of ∼0.3-0.5 dex in the optically-thin approximation. Using FLAMES, FEROS, and UVES archive spectra, the minimum and maximum reduced equivalent widths for Milky Way gas are found to lie in the range ∼35-125 mÅ and ∼30-160 mÅ for Ca ii K and Na i D, respectively. The range is consistent with a previously published simple model of the interstellar medium consisting of spherical cloudlets of filling factor ∼0.3, although other geometries are not ruled out. Finally, the derived functional form for parallax (π) and Ca ii column density (N_CaII) is found to be π(mas) = 1 / (2.39 × 10^-13 × N_CaII (cm^-2) + 0.11). Our derived parallax is ∼25 per cent lower than predicted by Megier et al. (2009, A&A, 507, 833) at a distance of ∼100 pc and ∼15 percent lower at a distance of ∼200 pc, reflecting inhomogeneity in the Ca ii distribution in the different sightlines studied.

Combustion Noise

Combustion noise is becoming increasingly important as a major noise source in aeroengines and ground based gas turbines. This is partially because advances in design have reduced the other noise sources, and partially because next generation combustion modes burn more unsteadily, resulting in increased external noise from the combustion. This review reports recent progress made in understanding combustion noise by theoretical, numerical and experimental investigations. We first discuss the fundamentals of the sound emission from a combustion region. Then the noise of open turbulent flames is summarized. We subsequently address the effects of confinement on combustion noise. In this case not only is the sound generated by the combustion influenced by its transmission through the boundaries of the combustion chamber, there is also the possibility of a significant additional source, the so-called ‘indirect’ combustion noise. This involves hot spots (entropy fluctuations) or vorticity perturbations produced by temporal variations in combustion, which generate pressure waves (sound) as they accelerate through any restriction at the exit of the combustor. We describe the general characteristics of direct and indirect noise. To gain further insight into the physical phenomena of direct and indirect sound, we investigate a simple configuration consisting of a cylindrical or annular combustor with a low Mach number flow in which a flame zone burns unsteadily. Using a low Mach number approximation, algebraic exact solutions are developed so that the parameters controlling the generation of acoustic, entropic and vortical waves can be investigated. The validity of the low Mach number approximation is then verified by solving the linearized Euler equations numerically for a wide range of inlet Mach numbers, stagnation temperature ratios, frequency and mode number of heat release fluctuations. The effects of these parameters on the magnitude of the waves produced by the unsteady combustion are investigated. In particular the magnitude of the indirect and direct noise generated in a model combustor with a choked outlet is analyzed for a wide range of frequencies, inlet Mach numbers and stagnation temperature ratios. Finally, we summarize some of the unsolved questions that need to be the focus of future research

Asymmetric hydrogen flame in a heated micro-channel: role of Darrieus-Landau and thermal-diffusive instabilities

Present work examines numerically the asymmetric behavior of hydrogen/air flame in a micro-channel subjected to a non-uniform wall temperature distribution. A high resolution (with cell size of 25 μm × 25 μm) of two-dimensional transient Navier–Stokes simulation is conducted in the low-Mach number formulation using detailed chemistry evolving 9 chemical species and 21 elementary reactions. Firstly, effects of hydrodynamic and diffusive-thermal instabilities are studied by performing the computations for different Lewis numbers. Then, the effects of preferential diffusion of heat and mass transfer on the asymmetric behavior of the hydrogen flame are analyzed for different inlet velocities and equivalence ratios. Results show that for the flames in micro-channels, interactions between thermal diffusion and molecular diffusion play major role in evolution of a symmetric flame into an asymmetric one. Furthermore, the role of Darrieus–Landau instability found to be minor. It is also found that in symmetric flames, the Lewis number decreases behind the flame front. This is related to the curvature of flame which leads to the inclination of thermal and mass fluxes. The mass diffusion vectors point toward the walls and the thermal diffusion vectors point toward the centerline. Asymmetric flame is observed when the length of flame front is about 1.1–1.15 times of the channel width.

Prediction of Upward Flame Spread over Polymers

In this work, the existing understanding of flame spread dynamics is enhanced through an extensive study of the heat transfer from flames spreading vertically upwards across 5 cm wide, 20 cm tall samples of extruded Poly (Methyl Methacrylate) (PMMA). These experiments have provided highly spatially resolved measurements of flame to surface heat flux and material burning rate at the critical length scale of interest, with a level of accuracy and detail unmatched by previous empirical or computational studies. Using these measurements, a wall flame model was developed that describes a flame’s heat feedback profile (both in the continuous flame region and the thermal plume above) solely as a function of material burning rate. Additional experiments were conducted to measure flame heat flux and sample mass loss rate as flames spread vertically upwards over the surface of seven other commonly used polymers, two of which are glass reinforced composite materials. Using these measurements, our wall flame model has been generalized such that it can predict heat feedback from flames supported by a wide range of materials. For the seven materials tested here – which present a varied range of burning behaviors including dripping, polymer melt flow, sample burnout, and heavy soot formation – model-predicted flame heat flux has been shown to match experimental measurements (taken across the full length of the flame) with an average accuracy of 3.9 kW m-2 (approximately 10 – 15 % of peak measured flame heat flux). This flame model has since been coupled with a powerful solid phase pyrolysis solver, ThermaKin2D, which computes the transient rate of gaseous fuel production of constituents of a pyrolyzing solid in response to an external heat flux, based on fundamental physical and chemical properties. Together, this unified model captures the two fundamental controlling mechanisms of upward flame spread – gas phase flame heat transfer and solid phase material degradation. This has enabled simulations of flame spread dynamics with a reasonable computational cost and accuracy beyond that of current models. This unified model of material degradation provides the framework to quantitatively study material burning behavior in response to a wide range of common fire scenarios.

Measurement and Simulation of Suppression Effects in a Buoyant Turbulent Line Fire

An experimental and numerical study of turbulent fire suppression is presented. For this work, a novel and canonical facility has been developed, featuring a buoyant, turbulent, methane or propane-fueled diffusion flame suppressed via either nitrogen dilution of the oxidizer or application of a fine water mist. Flames are stabilized on a slot burner surrounded by a co-flowing oxidizer, which allows controlled delivery of either suppressant to achieve a range of conditions from complete combustion through partial and total flame quenching. A minimal supply of pure oxygen is optionally applied along the burner to provide a strengthened flame base that resists liftoff extinction and permits the study of substantially weakened turbulent flames. The carefully designed facility features well-characterized inlet and boundary conditions that are especially amenable to numerical simulation. Non-intrusive diagnostics provide detailed measurements of suppression behavior, yielding insight into the governing suppression processes, and aiding the development and validation of advanced suppression models. Diagnostics include oxidizer composition analysis to determine suppression potential, flame imaging to quantify visible flame structure, luminous and radiative emissions measurements to assess sooting propensity and heat losses, and species-based calorimetry to evaluate global heat release and combustion efficiency. The studied flames experience notable suppression effects, including transition in color from bright yellow to dim blue, expansion in flame height and structural intermittency, and reduction in radiative heat emissions. Still, measurements indicate that the combustion efficiency remains close to unity, and only near the extinction limit do the flames experience an abrupt transition from nearly complete combustion to total extinguishment. Measurements are compared with large eddy simulation results obtained using the Fire Dynamics Simulator, an open-source computational fluid dynamics software package. Comparisons of experimental and simulated results are used to evaluate the performance of available models in predicting fire suppression. Simulations in the present configuration highlight the issue of spurious reignition that is permitted by the classical eddy-dissipation concept for modeling turbulent combustion. To address this issue, simple treatments to prevent spurious reignition are developed and implemented. Simulations incorporating these treatments are shown to produce excellent agreement with the experimentally measured data, including the global combustion efficiency.