bluuebunny/crossref_metadata_2025_split huggingface dataset:
L'idée de pathologie de la société chez Habermas
Authors: Ipperciel Donald 
Published: April 2010

AbstractThough Habermas explicitly rejected psychoanalysis as a model for a critical theory of society, it seems to have continued to shape his thought beyond the publication of Knowledge and Human Interests. The conceptual framework underlying his more recent social theory (Theory of Communicative Action,) would also be indebted to the psychoanalytical paradigm. This thesis is developed through the idea of the pathology of society, which represents the cornerstone of a specifically critical theory of society. In his demonstration, the author establishes a structural relationship between psychical and social organization, and between individual pathology and the diagnostic of modern societies.
Another Look at the Problem of the Unexpected Examination
Authors: Kramer Matthew H. 
Published: April 2010

RésuméLes philosophes, au cours des cinquante dernières années, se sont efforcés de démontrer qu'un professeur peut, d'une manière cohérente et exacte, annoncer à ses étudiants qu'un examen surprise aura lieu lors d'une journée non spécifiée d'une période donnée, le problème étant qu'une telle annonce peut sembler s'annuler elle-même lorsqu'elle est soumise à une induction régressive. Deux grandes approches, l'une épistémique et l'autre logique, one été développées à ce propos. Le présent article adopte une approche logique, mais repose aussi d'une manière cruciale sur une compréhension épistémique du problème, pour essayer de montrer que l'annonce du professeur peut effectivement être cohérente et exacte.
Piaget's Genetic Epistemology and the Problem of Truth
Authors: Greif Gary F. 
Published: April 2010

Piaget's work represents, f?om his own point of view, not only a study of intelligence, but a remedy for philosophical studies of the same subject matter. Philosophy in general, according to Piaget, “does not give us knowledge, as it lacks methods of verification”, that is, it does not give knowledge of anything except the personality of the philosopher “sim-ply meditating in his study by the light of his own reason”. Philosophical reflection can serve a heuristic function, but cannot yield objective knowledge, of truth. Piaget succinctly states this crucial methodologicalposition as follows:Although speculative reflection is a fertile and even necessary heuristic introduction to all inquiry, it can only lead to the elaboration of hypotheses, as sweeping as you like, to be sure, but as long as one does not seek verification by a group of facts established experimentally or by a deduction conforming to an exact algorithm (as in logic), the criterion of truth can only remain subjective, in the manner of an intuitive satisfaction, of “self-evidence,” etc.
Evaluating Pacifism
Authors: Orend Brian 
Published: April 2010

RésuméLe pacifisme a toujours constitué une approche respectable et influente à l'éthique de la guerre et de la paix. On veut ici, à partir de la littérature récente, en proposer une nouvelle évaluation. Plus précisément, l'article a deux objectifs: proposer une présentation rigoureuse et charitable des thèses pacifistes; et avancer, dans la perspective de la théorie contemporaine de la juste guerre, une critique puissante et détaillée des thèses en question.
Reply to “Forrester's Paradox”
Authors: Robinson Richard E. 
Published: April 2010

Forrester claims to have shown that a contradiction can be derived from a set of two apparently innocuous moral (or legal) rules together with standard deontic logic (SDL), a principle for adverbial detachment, and a statement of fact. Let l be a system of laws that has the following as immediate consequences:(1) It is obligatory* that Smith not murder Jones.(2) It is obligatory; that, if Smith murders Jones, then Smith murders Jones gently.
A bicharacteristic formulation of the ideal MHD equations
Authors: GUPTA HARI SHANKER , PRASAD PHOOLAN 
Published: April 2010

AbstractOn a characteristic surface Ω of a hyperbolic system of first-order equations in multi-dimensions (x, t), there exits a compatibility condition which is in the form of a transport equation along a bicharacteristic on Ω. This result can be interpreted also as a transport equation along rays of the wavefront Ωt in x-space associated with Ω. For a system of quasi-linear equations, the ray equations (which has two distinct parts) and the transport equation form a coupled system of underdetermined equations. As an example of this bicharacteristic formulation, we consider two-dimensional unsteady flow of an ideal magnetohydrodynamics gas with a plane aligned magnetic field. For any mode of propagation in this two-dimensional flow, there are three ray equations: two for the spatial coordinates x and y and one for the ray diffraction. In spite of little longer calculations, the final four equations (three ray equations and one transport equation) for the fast magneto-acoustic wave are simple and elegant and cannot be derived in these simple forms by use of a computer program like REDUCE.
Stellar models: firm evidence, open questions and future developments
Authors: Cassisi Santi 
Published: April 2010

AbstractDuring this last decade our knowledge of the evolutionary properties of stars has significantly improved. This result has been achieved thanks to our improved understanding of the physical behavior of stellar matter in the thermal regimes characteristic of the different stellar mass ranges and/or evolutionary stages.This notwithstanding, the current generation of stellar models is still affected by several, not negligible, uncertainties related to our poor knowledge of some thermodynamical processes and nuclear reaction rates, as well as the efficiency of mixing processes. These drawbacks have to be properly taken into account when comparing theory with observations, to derive evolutionary properties of both resolved and unresolved stellar populations.In this paper we review the major sources of uncertainty along the main evolutionary stages, and emphasize their impact on population synthesis techniques.
The delay time distribution of type Ia supernovae: theory and observation
Authors: Vanbeveren Dany , Mennekens Nicki , De Greve Jean-Pierre , De Donder Erwin 
Published: April 2010

AbstractUsing a population number synthesis code, the theoretical time distributions of type Ia supernovae in starburst galaxies are calculated, using competing models for the formation of such events: the single degenerate (a white dwarf accreting matter from a late main sequence or red giant companion) and double degenerate (the merger of two white dwarfs) scenario. The code includes the latest results in determining the progenitors for both models. Examples are the mass stripping effect in the case of the single degenerate scenario and the differentiation between the α- (based on the balance of energy) and γ- (based on the balance of angular momentum) description of energy conversion during common envelope evolution of binaries. The shape and extent of the obtained delay time distributions critically depends on which formation scenario is used. Comparing these results to the latest observed distributions allows to draw conclusions about the constraints put on the theoretical models by these observations. We also specifically investigate the influence of the degree of conservatism during Roche lobe overflow on the delay time distribution. We conclude that the single degenerate scenario alone cannot reproduce the observed delay time distributions, and that most double degenerate type Ia supernovae are formed through a quasi-conservative Roche lobe overflow phase followed by spiral-in, as opposed to a double common envelope evolution.
Surface brightness fluctuations, tracers of stellar mass-loss?
Authors: González-Lópezlira Rosa A. , Bruzual-A. Gustavo , Charlot Stéphane , Ballesteros-Paredes Javier , Loinard Laurent 
Published: April 2010

AbstractWe present optical and IR integrated colors and SBF magnitudes, computed from stellar population synthesis models that include emission from the dusty envelopes surrounding mass-loosing TP-AGB stars. We explore the effects of varying the mass-loss rate by one order of magnitude around the fiducial value, modifying accordingly both the stellar parameters and the output spectra of the TP-AGB stars plus their dusty envelopes. We compare these models to optical and near-IR data of single AGB stars and Magellanic star clusters. Neither broad-band colors nor SBF measurements in the optical or the near-IR can discern global changes in the mass-loss rate of a stellar population. However, we predict that mid-IR SBF measurements can pick out such changes, and actually resolve whether a relation between metallicity and mass-loss exists.
The Future of Stellar Populations Studies in the Milky Way and the Local Group
Authors: Majewski Steven R. 
Published: April 2010

AbstractThe last decade has seen enormous progress in understanding the structure of the Milky Way and neighboring galaxies via the production of large-scale digital surveys of the sky like 2MASS and SDSS, as well as specialized, counterpart imaging surveys of other Local Group systems. Apart from providing snaphots of galaxy structure, these “cartographic” surveys lend insights into the formation and evolution of galaxies when supplemented with additional data (e.g., spectroscopy, astrometry) and when referenced to theoretical models and simulations of galaxy evolution. These increasingly sophisticated simulations are making ever more specific predictions about the detailed chemistry and dynamics of stellar populations in galaxies. To fully exploit, test and constrain these theoretical ventures demands similar commitments of observational effort as has been plied into the previous imaging surveys to fill out other dimensions of parameter space with statistically significant intensity. Fortunately the future of large-scale stellar population studies is bright with a number of grand projects on the horizon that collectively will contribute a breathtaking volume of information on individual stars in Local Group galaxies. These projects include: (1) additional imaging surveys, such as Pan-STARRS, SkyMapper and LSST, which, apart from providing deep, multicolor imaging, yield time series data useful for revealing variable stars (including critical standard candles, like RR Lyrae variables) and creating large-scale, deep proper motion catalogs; (2) higher accuracy, space-based astrometric missions, such as Gaia and SIM-Lite, which stand to provide critical, high precision dynamical data on stars in the Milky Way and its satellites; and (3) large-scale spectroscopic surveys provided by RAVE, APOGEE, HERMES, LAMOST, and the Gaia spectrometer, which will yield not only enormous numbers of stellar radial velocities, but extremely comprehensive views of the chemistry of stellar populations. Meanwhile, previously dust-obscured regions of the Milky Way will continue to be systematically exposed via large infrared surveys underway or on the way, such as the various GLIMPSE surveys from Spitzer's IRAC instrument, UKIDSS, APOGEE, JASMINE and WISE.
Early-type dwarf galaxies in the M81 group
Authors: Lianou Sophia , Grebel Eva K. , Koch Andreas 
Published: April 2010

AbstractThe M81 group is a highly interacting group consisting of a few large galaxies and about 40 dwarfs of both early- and late-type, thus making it an important nearby laboratory to study environmental effects and the role of interactions in the formation and evolution of dwarf galaxies. We are studying the resolved stellar populations of the early-type dwarf galaxies in this group with available HST/ACS data. We will show results on the metallicity distribution functions and on the potential presence of population gradients for these dwarf galaxies.
Dwarf Galaxies in the Local Group
Authors: Tolstoy Eline 
Published: April 2010

AbstractWithin the Local Universe galaxies can be studied in great detail star by star. The Color-Magnitude Diagram synthesis analysis method is well established as the most accurate way to determine the detailed star formation history of galaxies going back to the earliest times. This approach received a significant boost from the exceptional data sets that wide field CCD imagers on the ground and the Hubble Space Telescope could provide. Spectroscopic studies using large ground based telescopes such as VLT, Magellan, Keck and HET have allowed the determination of abundances and kinematics for significant samples of stars in nearby dwarf galaxies. These studies have shown directly how properties can vary spatially and temporally, which gives important constraints to theories of galaxy formation and evolution.
Ground-based proper motions of nearby local group galaxies: A progress report for Fornax
Authors: Méndez Rene A. , Costa Edgardo , Pedreros Mario H. , Moyano Maximiliano , Altmann Martin , Gallart Carme 
Published: April 2010

AbstractDetermining the kinematics of the dwarf Spheroidal galaxies (dSph) satellites of the Milky Way (MW) is crucial to estimate the mass of our galaxy, to understand its formation process and that of its satellites, to explain the origin of stellar streams in the MW's halo that seem to be related to these satellites, and to understand the role of tidal interactions in the evolution and star formation history of low mass galaxies and of the halo of our Galaxy. In what follows we briefly explain a ground-based astrometric project that will have an impact on these issues, and present some preliminary results.
An analysis of the composite stellar population in M32
Authors: Coelho P. , Mendes de Oliveira C. , Cid Fernandes R. 
Published: April 2010

AbstractWe obtained long-slit spectra of high S/N of the galaxy M32 with the GMOS Spectrograph at the Gemini-North telescope. We analysed the integrated spectra by means of spectral fitting in order to extract the mixture of stellar populations that best represents its composite nature. As our main result, we propose that an ancient and an intermediate-age population co-exist in M32, and that the balance between these two populations change between the nucleus and outside one effective radius (1reff) in the sense that the contribution from the intermediate population is larger at the nuclear region. We retrieve a smaller signal of a young population at all radii whose origin is unclear, and may be a contamination from horizontal branch stars, blue stragglers or a true young population previously unidentified (Monachesi et al., this volume). We compare our metallicity distribution function for a region 1 to 2 arcmin from the centre to the one obtained with photometric data by Grillmair et al. Both distributions are broad, but our spectroscopically derived distribution has a significant component with [Z/Z⊙] ≤ −1, which is not found by Grillmair et al.
What drives the star formation in early-type galaxies at late epochs? - the case for minor mergers
Authors: Kaviraj Sugata , Ellis Richard , Yi Sukyoung , Silk Joseph , Schawinski Kevin , Gawiser Eric , van Dokkum Pieter , Urry C. Megan 
Published: April 2010

AbstractMulti-wavelength photometry of early-type galaxies (ETGs) in the COSMOS survey is used to demonstrate that the low-level star formation activity in the ETG population at late epochs (z < 1) is likely to be driven by repeated minor mergers. While relaxed ETGs are almost entirely contained within the UV red sequence, their morphologically disturbed counterparts are largely found in the blue cloud, regardless of luminosity. Since empirically determined major-merger rates in the redshift range z < 1 are a few factors too low to account for the number fraction of disturbed ETGs, this suggests that minor mergers are the principal mechanism that drives star formation activity in ETGs at low and intermediate redshift.
Ecology of galaxy stellar populations from optical spectroscopic surveys
Authors: Gallazzi Anna 
Published: April 2010

AbstractThe age and chemical composition of the stars in present-day galaxies carry important clues about their star formation processes. The latest generation of population synthesis models have allowed to derive age and stellar metallicity estimates for large samples of low-redshift galaxies. After reviewing the main results about the distribution in ages and metallicities as a function of galaxy mass, I will concentrate on recent analysis that aims at disentangling the dependences of stellar populations properties on environment and on galaxy stellar mass. Finally, new models that predict the response of the full spectrum to variations in [α/Fe] will allow us to derive accurate estimates of elements abundance ratios and gain deeper insight into the timescales of star formation cessation.
Stellar populations of local infrared-selected galaxies
Authors: Chen X. Y. , Liang Y. C. , Hammer F. , Zhao Y. H. , Zhong G. H. 
Published: April 2010

AbstractThe stellar populations of 849 local infrared-selected galaxies from SDSS and IRAS (including 419 star-forming galaxies, 326 composite galaxies, 35 Seyfert 2s, and 69 LINERs in 4 spectral classes) are studied by using STARLIGHT. Among the 4 spectral classes, the importance of young populations decreases from star-forming, composite, Seyfert 2 to LINER; and Seyfert 2 and LINER are more metal-rich; ULIGs (ultra luminous infrared galaxies) & LIGs present the youngest populations among 3 infrared luminosity bins; and normal galaxies are more metal-rich. The dominant contributors to masses are all old populations.
Automated morphological classification of galaxies using wavelet transform
Authors: Curty Didier , Cuisinier François C. , Rabaça Carlos R. 
Published: April 2010

AbstractThe wavelet transform acts to segregate objects in function of their size. We apply this method on images of galaxies to decompose them into coefficients representing only objects of the same size. The total fluxes of the wavelet coefficients describe the cumulative power spectrum of spatial frequencies. Based on this spectrum, we propose a new parameter to quantify the galaxy texture. As expected, it remains small and quite invariant for early-type galaxies, while it covers a large range and takes larger values for late-type galaxies. Combined with a second parameter, our determination of the texture is able to successfully separate galaxy types. By thresholding the wavelet coefficients, we detect luminous lumps. In irregular galaxies, their radial distribution seems to show a double peak. This could be the trace of a privileged radial distance of strong star formation regions.
Empirical tests of evolutionary synthesis models
Authors: Gomes Jean Michel , Cid Fernandes R. 
Published: April 2010

AbstractSpectral synthesis of stellar populations has proven to be one of the most powerful methods to decompose the different mixtures of stellar contributions in galaxies, and applications of this technique routinely appear in the literature nowadays. Our group, for instance, the SEAGal (Semi Empirical Analysis of Galaxies) collaboration, has derived the star formation history of all galaxies in the SDSS with the starlight code, obtaining various results of astrophysical interest. As any other fossil method, the results rely heavily on high spectral resolution evolutionary synthesis models. To test this model dependence we run starlight on samples of star-forming and passive galaxies from the SDSS using different sets of models.We explore models using “Padova 1994” and modified “Padova” evolutionary tracks with a different receipt for the asymptotic giant branch phase, as well as different stellar libraries (STELIB versus MILES+Granada). We then compare derived properties such as mean age, mean metallicity, extinction, star-formation and chemical histories. Despite a broad brush agreement, systematic differences emerge from this comparison. The different evolutionary tracks used lead to essentially the same results, at least insofar as optical spectra are concerned. Different stellar libraries, on the other hand, have a much bigger impact. The newer models produce quantifiably better fits and eliminate some pathologies (like suspicious combinations of base elements, systematical spectral residuals in some windows, and, sometimes, negative extinction) of fits derived with STELIB-based models, but there are still some caveats. These empirical tests provide useful feedback for model makers.
Tracers of Star Formation in the Near Infrared
Authors: Martins L. , Ardila A. , Gruenwald R. , de Souza R. 
Published: April 2010

AbstractStarburst features in the optical are nowadays well known, but the use of this knowledge is not always possible (e.g. objects heavily obscured). In this case the near-IR is of unprecedented value. Recent models show that TP-AGB stars should dominate the NIR spectra of populations 0.3 to 2 Gyr old. While the optical spectra is insensitive to the presence of these stars, the near-IR changes dramatically. Not only does the absolute flux in the near-IR is affected, but also peculiar absorption features appear. These features can be used as indicators of 1 Gyr stellar population. In this work we used the IRTF Spex to create the first empirical database of NIR spectra of carefully selected starbursts, to test for the first time and in a consistent way the new stellar population models that account for the TP-AGB. The methodology used is to do stellar population synthesis in the optical and in the NIR, and compare the predictions of both spectral regions. We also compare the strength of important features of the TP-AGB stars, like the CN (1.1 microns) and CO (2.3 microns) bands with optical diagnostics.
Detailed Abundances for Field Stars Surrounding the LMC Cluster Hodge 11
Authors: Mateluna Renee , Geisler Douglas , Villanova Sandro 
Published: April 2010

AbstractWe present results of a detailed model atmosphere abundance analysis for a variety of elements, including Fe, Ca, Si, Ti, Sc, Ni, Cr and Ba for a number of giants in the surrounding field of the LMC cluster H11, obtained from high resolution FLAMES@VLT spectra.
The interacting binary V 393 Scorpii: another clue for Double Periodic Variables
Authors: Mennickent Ronald , Kołaczkowski Zbigniew , Djurasevic Gojko , Michalska Gabriela , Barría Daniela 
Published: April 2010

AbstractWe give a brief report on spectroscopic properties of V 393 Scorpii. Hα emission and shape and radial velocity of He I5875 are modulated with the long cycle. The long cycle is explained as a relaxation cycle in the circumprimary disc, that cumulates the mass transferred from the donor until certain instability produces disc depletion.
The Mg/Fe characterization of the MILES library for stellar populations studies
Authors: Milone André , Sansom Anne E. , Sánchez-Blázquez Patricia 
Published: April 2010

AbstractWe have obtained [Mg/Fe] for around 77% of the stars of the MILES library of stellar spectra in order to include this important information into simple stellar population (SSP) models. The abundance ratios, which were carefully calibrated to a single uniform scale, were obtained through a compilation from high spectral resolution works plus robust spectroscopic analysis at medium resolution. The high resolution data provided an extensive control sample. Average uncertainties (0.06 and 0.12 dex for the high and medium resolution samples respectively) and the good coverage of the stars with [Mg/Fe] over the MILES's parameter space will permit us to semi-empirically build up new SSP models with accurate α-enhancements for ages older than 1 Gyr. This will open new prospects for evolutionary stellar population synthesis.