bluuebunny/crossref_metadata_2025 huggingface dataset:
The benefits of mentoring and coaching in the public sector
Authors: Ganesh Aaron , Bozas Alec , Subban Mogie , Munapo Elias
Published: December 2016

A project at the Frontier Hospital in Queenstown (South Africa) commenced in January 2009, and extended over a period of four months. Two mentoring and coaching workshops were held to create a broad awareness and a common understanding about mentoring and coaching as tools for learning and growth. A study was carried out to determine the effects of mentoring and coaching on managers following attendance of the workshops. The study results revealed that the race and gender of the respondents did not significantly affect mentoring and coaching. The respondents were in unanimous agreement that the programme was beneficial and the functional specialisation of the respondents did not affect their assessment of the mentoring and coaching programme. The study also revealed that mentoring and coaching did improve work performance and that it had far reaching positive effects in improving work-place performance at Frontier Hospital, in South Africa.
Case studies on the success or failure of futures contracts
Authors: Till Hilary
Published: December 2016

Why do some futures contracts succeed and others fail? Although the U.S. futures markets have evolved in a trial-and-error fashion, research suggests key elements have determined whether particular futures contracts succeeded or failed. This knowledge could be useful for new financial centers as they build successful futures markets. This paper shows that there are three elements that determine whether a futures contract succeeds or not: 1. There must be a commercial need for hedging; 2. A pool of speculators must be attracted to a market; and 3. Public policy should not be too adverse to futures trading
Interethnic violence and principles of intercultural education in schools: The case study of Slovenia
Authors: Medaric Zorana , Zadel Maja , Ramesa Martina
Published: December 2016

This paper discusses the main findings of a study on interethnic violence
carried out in the school environment in Slovenia. It examines the
occurrence and perception of different forms of violence and the role of
educators and the commitment of schools to promote nonviolence and the
wellbeing of pupils, which is reached mainly by applying principles of
intercultural education. The quantitative and qualitative findings take
three perspectives into account: (1) pupils? opinions and experiences, (2)
perceptions of educators and (3) perspectives of experts in the area of
(interethnic) peer violence. Special emphasis is placed on the informants?
perceptions of the school environment, their experiences of interethnic
violence and interventions in cases of violence in schools aimed at its
prevention. The paper argues that despite the general acceptance of
principles of intercultural education in Slovenian schools and the recurrent
self-initiatives of individual educators, a coordinated and integrated
approach is needed both for dealing with (interethnic) violence and for
promulgating values of intercultural coexistence in schools.
Pegida in Parliament?: Explaining the Failure of Pegida in Austria
Authors: Hafez Farid
Published: December 2016

This article explains the failure of Pegida Austria as a social movement organization by testing three prominent theories of social movement theory: political opportunity structures, ideology, and resource mobilization. The failure of Pegida to play a role in Austrian politics is ascribed to the dominant role the Freedom Party (FPÖ) already plays in the Austrian parliament, the FPÖ’s issue dominance on anti-immigration and Islamophobia in public discourse, and the relative scarcity of individuals capable of mass mobilization outside the spectrum of political parties. The analysis is based on a crucial-case study that does a comparative content analysis of the FPÖ and Pegida platforms to assess the ideology argument. The political opportunity and human resource arguments are analyzed with process tracing. The findings reveal that all three theories jointly help to explain the failure of Pegida Austria.
Iron oxide/PLGA nanoparticles for magnetically controlled drug release
Authors: Ruggiero M. Rosaria , Geninatti Crich Simonetta , Sieni Elisabetta , Sgarbossa Paolo , Cavallari E. , Stefania Rachele , Dughiero Fabrizio , Aime Silvio
Published: December 2016

Recently, nanoscale stimuli-responsive devices have received much attention thanks to their potential to limit the cytotoxic effect of the therapeutic treatment at the diseased tissue. Among different physical triggers, large alternating magnetic fields enable the conversion of magnetic energy into heat by using magnetic nanoparticles that generate localized hyperthermia, named Magneto Fluid Hyperthermia (MFH). This methodology can be exploited for cancer therapy or/and thermally activated drug release. The small size iron oxide nanoparticles (Fe-NPs), such as SPIO (small iron oxide particles) and USPIO (ultra-small iron oxide particles), currently used for this application have many limitations due to their 1) high intratumor concentration needed due to the low heating power 2) short particle blood-half-life, 3) non-specific distribution, 4) low internalization efficiency. For these reasons many efforts are necessary to make magneto fluid particle hyperthermia (MFH) a competitive tumor therapy for clinical applications. New iron oxide nanoparticles, coated with oleate, with a diameter of 5-18 nm, have been prepared by co-precipitation and incorporated into PLGA-NPs (PLGA=Poly(lactic-co-glycolic acid) in order to improve their biocompatibility and `` in vivo'' stability. Moreover, PLGA-NPs have been loaded with both NPs-Fe and antitumor drugs (Paclitaxel, PTX), an anticancer hydrophobic drug used in the treatment of ovarian and breast cancer, to perform MFH triggered drug release. The PTX and Fe-NPs loaded nanoparticles may be considered as an effective anticancer drug delivery system for Imaging-guided hyperthermic treatment of tumors.
Les Hypocoelus (Coleoptera Eucnemidae) sont-ils des insectes rares ?
Authors: Leseigneur Lucien , Steffen Jean
Published: December 2016

L'étude de populations importantes d' Hypocoelus olexai Palm et H. foveicollis Thomson, espèces réputées rares, montre qu'elles peuvent pulluler dans des conditions favorables. Le suivi méthodique de ces populations au cours de l'été 1989 a permis d'établir une phénologie de ces deux espèces ; on a pu également observer leur comportement et préciser sur un grand nombre d'individus les variations de taille et de coloration.
Panorama historique de la découverte des orchidées sauvages de France
Authors: Jacquet Pierre
Published: December 2016

Comme toute science, la botanique n'existerait pas sans les botanistes, qui l'ont créée, modulée, transformée, complétée, au cours des âges. L'invention de l'imprimerie permet, dès le 16e siècle, une explosion des connaissances de la nature et la dissémination du savoir par des ouvrages spécialisés, encourageant la naissance de vocations et la formation de cénacles de chercheurs de plantes, attachés au même amour de la nature. Après la révolution linnéenne, le 18e et surtout le 19e siècle voient la connaissance de base de notre flore française atteindre une quasi-perfection que le 20e siècle ne remettra pas fondamentalement en cause. C'est, bien modestement, au travers de l'étude d'une petite famille botanique, celle des orchidées de France, que cette évolution est ici considérée. S'il est vrai que des botanistes de tous pays ont largement contribué à la connaissance de notre flore, cette petite étude a pour but de rendre hommage à des savants de culture française, petits ou grands, professionnels ou amateurs, parfois méconnus, qui ont laissé ce nom abrégé ou même cette initiale, que l'on ajoute, sans trop y penser, au nom latin d'une orchidée que l'on veut désigner.
Contribution à l'établissement des catalogues régionaux : Histeridae (Coleoptera)
Authors: Gomy Yves
Published: December 2016

Liste de localités nouvelles concernant 61 espèces d'Histeridae de la faune française.
Tubulicium junci-acuti nov. sp. (Basidiomycotina) en provenance de la Corse
Authors: Boidin Jacques , Gaignon Maurice
Published: December 2016

Description d'un Corticié épithéloïde des gaines du jonc aigu ; choix du genre Tubulicium et clé de celui-ci.
Synopsis des espèces françaises appartenant au genre Mycetophagus Hellwig, 1792 (Coleoptera Mycetophagidae)
Authors: Rogé Jean
Published: December 2016

Clé d'identification illustrée et commentée des Mycetophagus de la faune de France et bref aperçu de leur répartition.
Notes sur la classification des Ranidae (Amphibiens, Anoures)
Authors: Dubois Alain
Published: December 2016

Une nouvelle classification provisoire de la superfamille des Ranoidea, et plus particulièrement de la famille des Ranidae et du genre Rana, est proposée. Le genre Rana est ici subdivisé, principalement sur la base de critères phénétiques, en trente-trois groupes, auxquels est ici provisoirement attribué le rang de sous-genres. Le but principal de cette classification provisoire, qui doit être comprise comme un outil de travail et non pas comme une proposition définitive, est de servir de guide pour de futures études sur la phylogénie de cette famille très vaste et à répartition quasi cosmopolite : cette classification aidera à sélectionner des espèces représentatives de chaque groupe phénétique pour l'étude des états de caractères, et à choisir les hors-groupes appropriés pour l'établissement de la polarité des morphoclines de caractères. Ce n'est que lorsque la phylogénie de la famille dans son ensemble sera résolue qu'il sera possible d'élaborer une classification plus stable, qui s'avérera peut-être très différente de celle qui est présentée ci-dessous.
DEVELOPING ATMOSPHERIC RETRIEVAL METHODS FOR DIRECT IMAGING SPECTROSCOPY OF GAS GIANTS IN REFLECTED LIGHT. I. METHANE ABUNDANCES AND BASIC CLOUD PROPERTIES
Authors: Lupu Roxana E. , Marley Mark S. , Lewis Nikole , Line Michael , Traub Wesley A. , Zahnle Kevin
Published: December 2016

Upcoming space-based coronagraphic instruments in the next decade will perform reflected light spectroscopy and photometry of cool directly imaged extrasolar giant planets. We are developing a new atmospheric retrieval methodology to help assess the science return and inform the instrument design for such future missions, and ultimately interpret the resulting observations. Our retrieval technique employs a geometric albedo model coupled with both a Markov chain Monte Carlo Ensemble Sampler (emcee) and a multimodal nested sampling algorithm (MultiNest) to map the posterior distribution. This combination makes the global evidence calculation more robust for any given model and highlights possible discrepancies in the likelihood maps. As a proof of concept, our current atmospheric model contains one or two cloud layers, methane as a major absorber, and a H2–He background gas. This 6-to-9 parameter model is appropriate for Jupiter-like planets and can be easily expanded in the future. In addition to deriving the marginal likelihood distribution and confidence intervals for the model parameters, we perform model selection to determine the significance of methane and cloud detection as a function of expected signal-to-noise ratio in the presence of spectral noise correlations. After internal validation, the method is applied to realistic spectra of Jupiter, Saturn, and HD 99492c, a model observing target. We find that the presence or absence of clouds and methane can be determined with high confidence, while parameter uncertainties are model dependent and correlated. Such general methods will also be applicable to the interpretation of direct imaging spectra of cloudy terrestrial planets.
K2 DISCOVERS A BUSY BEE: AN UNUSUAL TRANSITING NEPTUNE FOUND IN THE BEEHIVE CLUSTER
Authors: Obermeier Christian , Henning Thomas , Schlieder Joshua E. , Crossfield Ian J. M. , Petigura Erik A. , Howard Andrew W. , Sinukoff Evan , Isaacson Howard , Ciardi David R. , David Trevor J. , Hillenbrand Lynne A. , Beichman Charles A. , Howell Steve B. , Horch Elliott , Everett Mark , Hirsch Lea , Teske Johanna , Christiansen Jessie L. , Lépine Sébastien , Aller Kimberly M. , Liu Michael C. , Saglia Roberto P. , Livingston John , Kluge Matthias
Published: December 2016

Open clusters have been the focus of several exoplanet surveys, but only a few planets have so far been discovered. The Kepler spacecraft revealed an abundance of small planets around small cool stars, therefore, such cluster members are prime targets for exoplanet transit searches. Kepler's new mission, K2, is targeting several open clusters and star-forming regions around the ecliptic to search for transiting planets around their low-mass constituents. Here, we report the discovery of the first transiting planet in the intermediate-age (800 Myr) Beehive cluster (Praesepe). K2-95 is a faint (

)

dwarf from K2's Campaign 5 with an effective temperature of

, approximately solar metallicity and a radius of

. We detected a transiting planet with a radius of

and an orbital period of 10.134 days. We combined photometry, medium/high-resolution spectroscopy, adaptive optics/speckle imaging, and archival survey images to rule out any false-positive detection scenarios, validate the planet, and further characterize the system. The planet’s radius is very unusual as M-dwarf field stars rarely have Neptune-sized transiting planets. The comparatively large radius of K2-95b is consistent with the other recently discovered cluster planets K2-25b (Hyades) and K2-33b (Upper Scorpius), indicating systematic differences in their evolutionary states or formation. These discoveries from K2 provide a snapshot of planet formation and evolution in cluster environments and thus make excellent laboratories to test differences between field-star and cluster planet populations.
RADIAL VELOCITIES AND METALLICITIES OF RED GIANT STARS IN THE OLD OPEN CLUSTER NGC 7762
Authors: Carraro Giovanni , Semenko Eugene A. , Villanova Sandro
Published: December 2016

We present and discuss radial velocity and the very first metallicity measurements for nine evolved stars in the poorly known old open cluster NGC 7762. We isolated eight radial velocity cluster members and one interloper. Radial velocities are in good agreement with previous studies. NGC 7762 turns out to be of solar metallicity within the uncertainties ([Fe/H] = 0.04 ± 0.12). For this metallicity, the cluster age is 2.5 ± 0.2 Gyr, and falls in an age range where only a few old open clusters are known. With respect to previous studies, we find a larger distance, implying the cluster is located

pc from the Sun. For most of the elements we measure solar-scaled abundance ratios. We searched the literature for open clusters of similar age in the solar vicinity and found that NGC 7762 can be considered a twin of Ruprecht 147, a similar age cluster located only 300 pc from the Sun. In fact, as well as age, metallicity and abundance ratios are very close to Ruprecht 147 values within the observational uncertainties.
A TRIP TO THE CATACLYSMIC BINARY ZOO: DETAILED FOLLOW-UP OF 35 RECENTLY DISCOVERED SYSTEMS
Authors: Thorstensen John R. , Alper Erek H. , Weil Kathryn E.
Published: December 2016

We report follow-up studies of 35 recently discovered cataclysmic variables (CVs), 32 of which were found in large, automated synoptic sky surveys. The objects were selected for observational tractability. For 34 of the objects, we present mean spectra and spectroscopic orbital periods, and for one more we give an eclipse-based period. Thirty-two of the period determinations are new, and three of these refine published estimates based on superhump periods. The remaining three of our determinations confirm previously published periods. Twenty of the stars are confirmed or suspected dwarf novae with periods shorter than 3 hr, but we also find three apparent polars (AM Her stars) and six systems with

. Five of these systems have secondary stars visible in their spectra, from which we estimate distances when possible. The orbital period distribution of this sample is very similar to that of previously discovered CVs.
SHEAR ACCELERATION IN EXPANDING FLOWS
Authors: Rieger F. M. , Duffy P.
Published: December 2016

Shear flows are naturally expected to occur in astrophysical environments and potential sites of continuous non-thermal Fermi-type particle acceleration. Here we investigate the efficiency of expanding relativistic outflows to facilitate the acceleration of energetic charged particles to higher energies. To this end, the gradual shear acceleration coefficient is derived based on an analytical treatment. The results are applied to the context of the relativistic jets from active galactic nuclei. The inferred acceleration timescale is investigated for a variety of conical flow profiles (i.e., power law, Gaussian, Fermi–Dirac) and compared to the relevant radiative and non-radiative loss timescales. The results exemplify that relativistic shear flows are capable of boosting cosmic-rays to extreme energies. Efficient electron acceleration, on the other hand, requires weak magnetic fields and may thus be accompanied by a delayed onset of particle energization and affect the overall jet appearance (e.g., core, ridge line, and limb-brightening).
REVISITING THE STRUCTURE AND SPECTRUM OF THE MAGNETIC-RECONNECTION-HEATED CORONA IN LUMINOUS AGNs
Authors: Liu J. Y. , Qiao E. L. , Liu B. F.
Published: December 2016

It is believed that the hard X-ray emission in the luminous active galactic nuclei (AGNs) is from the hot corona above the cool accretion disk. However, the formation of the corona is still debated. Liu et al. investigated the spectrum of the corona heated by the reconnection of the magnetic field generated by dynamo action in the thin disk and emerging into the corona as a result of buoyancy instability. In the present paper, we improve this model to interpret the observed relation of the hard X-ray spectrum becoming softer at higher accretion rate in luminous AGNs. The magnetic field is characterized by

, i.e., the ratio of the sum of gas pressure and radiation pressure to the magnetic pressure in the disk (

). Besides, both the intrinsic disk photons and reprocessed photons by the disk are included as the seed photons for inverse Compton scattering. These improvements are crucial for investigating the effect of magnetic field on the accretion disk corona when it is not clear whether the radiation pressure or gas pressure dominates in the thin disk. We change the value of

in order to constrain the magnetic field in the accretion disk in luminous AGNs. We find that the energy fraction released in the corona (f) gradually increases with the decrease of

for the same accretion rate. When

decreases to less than 50, the structure and spectrum of the disk corona are independent of accretion rate, which is similar to the hard spectrum found in Liu et al. Comparing with the observational results of the hard X-ray bolometric correction factor in a sample of luminous AGNs, we suggest that the value of

is about 100–200 for α = 0.3, and the energy fraction f should be larger than 30% for hard X-ray emission.
THE BURSTY STAR FORMATION HISTORIES OF LOW-MASS GALAXIES AT 0.4 < z < 1 REVEALED BY STAR FORMATION RATES MEASURED FROM Hβ AND FUV
Authors: Guo Yicheng , Rafelski Marc , Faber S. M. , Koo David C. , Krumholz Mark R. , Trump Jonathan R. , Willner S. P. , Amorín Ricardo , Barro Guillermo , Bell Eric F. , Gardner Jonathan P. , Gawiser Eric , Hathi Nimish P. , Koekemoer Anton M. , Pacifici Camilla , Pérez-González Pablo G. , Ravindranath Swara , Reddy Naveen , Teplitz Harry I. , Yesuf Hassen
Published: December 2016

We investigate the burstiness of star formation histories (SFHs) of galaxies at 0.4 < z < 1 by using the ratio of star formation rates (SFRs) measured from Hβ and FUV (1500 Å) (Hβ-to-FUV ratio). Our sample contains 164 galaxies down to stellar mass (M
*) of 108.5
M
⊙ in the CANDELS GOODS-N region, where Team Keck Redshift Survey Keck/DEIMOS spectroscopy and Hubble Space Telescope/WFC3 F275W images from CANDELS and Hubble Deep UV Legacy Survey are available. When the ratio of Hβ- and FUV-derived SFRs is measured, dust extinction correction is negligible (except for very dusty galaxies) with the Calzetti attenuation curve. The Hβ-to-FUV ratio of our sample increases with M
* and SFR. The median ratio is ∼0.7 at M
* ∼ 108.5
M
⊙ (or SFR ∼ 0.5 M
⊙ yr−1) and increases to ∼1 at M
* ∼ 1010
M
⊙ (or SFR ∼ 10 M
⊙ yr−1). At M
* < 109.5
M
⊙, our median Hβ-to-FUV ratio is lower than that of local galaxies at the same M
*, implying a redshift evolution. Bursty SFH on a timescale of a few tens of megayears on galactic scales provides a plausible explanation for our results, and the importance of the burstiness increases as M
* decreases. Due to sample selection effects, our Hβ-to-FUV ratio may be an upper limit of the true value of a complete sample, which strengthens our conclusions. Other models, e.g., non-universal initial mass function or stochastic star formation on star cluster scales, are unable to plausibly explain our results.
THE ASTEROID BELT AS A RELIC FROM A CHAOTIC EARLY SOLAR SYSTEM
Authors: Izidoro André , Raymond Sean N. , Pierens Arnaud , Morbidelli Alessandro , Winter Othon C. , Nesvorny` David
Published: December 2016

The orbital structure of the asteroid belt holds a record of the solar system’s dynamical history. The current belt only contains ∼10−3 Earth masses yet the asteroids’ orbits are dynamically excited, with a large spread in eccentricity and inclination. In the context of models of terrestrial planet formation, the belt may have been excited by Jupiter’s orbital migration. The terrestrial planets can also be reproduced without invoking a migrating Jupiter; however, as it requires a severe mass deficit beyond Earth’s orbit, this model systematically under-excites the asteroid belt. Here we show that the orbits of the asteroids may have been excited to their current state if Jupiter’s and Saturn’s early orbits were chaotic. Stochastic variations in the gas giants’ orbits cause resonances to continually jump across the main belt and excite the asteroids’ orbits on a timescale of tens of millions of years. While hydrodynamical simulations show that the gas giants were likely in mean motion resonance at the end of the gaseous disk phase, small perturbations could have driven them into a chaotic but stable state. The gas giants’ current orbits were achieved later, during an instability in the outer solar system. Although it is well known that the present-day solar system exhibits chaotic behavior, our results suggest that the early solar system may also have been chaotic.
HIGH-RESOLUTION OBSERVATIONS OF MOLECULAR LINES IN ARP 220: KINEMATICS, MORPHOLOGY, AND LIMITS ON THE APPLICABILITY OF THE AMMONIA THERMOMETER
Authors: Zschaechner Laura K. , Ott Jürgen , Walter Fabian , Meier David S. , Momjian Emmanuel , Scoville Nick
Published: December 2016

We observe Arp 220, the nearest ultra-luminous infrared galaxy, over 4 GHz in the K and Ka bands, providing constraints for the kinematics and morphology, and identifying molecular species on scales resolving both nuclei (0.″6 or 230 pc). We detect multiple molecular species, including hydroxyl (OH

) in both cores, and tentatively detect H2O(615-523) at ∼21.84 GHz in both nuclei, indicating the likely presence of maser emission. The observed frequency range also contains metastable ammonia transitions from (J, K) = (1, 1)–(5, 5), as well as the (9, 9) inversion line; together, they are a well-known thermometer of dense molecular gas. Furthermore, the non-metastable (4, 2) and (10, 9), and possibly the (3, 1), lines are also detected. We apply a standard temperature analysis to Arp 220; however, the analysis is complicated in that standard local thermal equilibrium (LTE) assumptions do not hold. There are indications that a substantial fraction of ammonia could be in the non-metastable transitions, as opposed to only the metastable ones. Thus, the non-metastable transitions could be essential to constraining the temperature. We compare all of these data to ALMA observations of this source, confirming the outflow previously observed by other tracers in both nuclei.
THE IMPRINT OF RADIAL MIGRATION ON THE VERTICAL STRUCTURE OF GALAXY DISKS
Authors: Vera-Ciro Carlos , D’Onghia Elena , Navarro Julio F.
Published: December 2016

We use numerical simulations to examine the effects of radial migration on the vertical structure of galaxy disks. The simulations follow three exponential disks of different mass but similar circular velocity, radial scalelength, and (constant) scale height. The disks develop different non-axisymmetric patterns, ranging from feeble, long-lived multiple arms to strong, rapidly evolving few-armed spirals. These fluctuations induce radial migration through secular changes in the angular momentum of disk particles, mixing the disk radially and blurring pre-existing gradients. Migration primarily affects stars with small vertical excursions, regardless of spiral pattern. This “provenance bias” largely determines the vertical structure of migrating stars: inward migrators thin down as they move in, whereas outward migrators do not thicken up but rather preserve the disk scale height at their destination. Migrators of equal birth radius thus develop a strong scale-height gradient, not by flaring out as commonly assumed, but by thinning down as they spread inward. Similar gradients have been observed for low-[α/Fe] mono-abundance populations (MAPs) in the Galaxy, but our results argue against interpreting them as a consequence of radial migration. This is because outward migration does not lead to thickening, implying that the maximum scale height of any population should reflect its value at birth. In contrast, Galactic MAPs have scale heights that increase monotonically outward, reaching values that greatly exceed those at their presumed birth radii. Given the strong vertical bias affecting migration, a proper assessment of the importance of radial migration in the Galaxy should take carefully into account the strong radial dependence of the scale heights of the various stellar populations.
STATISTICAL TESTS OF GALACTIC DYNAMO THEORY
Authors: Chamandy Luke , Shukurov Anvar , Russ Taylor A.
Published: December 2016

Mean-field galactic dynamo theory is the leading theory to explain the prevalence of regular magnetic fields in spiral galaxies, but its systematic comparison with observations is still incomplete and fragmentary. Here we compare predictions of mean-field dynamo models to observational data on magnetic pitch angle and the strength of the mean magnetic field. We demonstrate that a standard

dynamo model produces pitch angles of the regular magnetic fields of nearby galaxies that are reasonably consistent with available data. The dynamo estimates of the magnetic field strength are generally within a factor of a few of the observational values. Reasonable agreement between theoretical and observed pitch angles generally requires the turbulent correlation time τ to be in the range of 10–

, in agreement with standard estimates. Moreover, good agreement also requires that the ratio of the ionized gas scale height to root-mean-square turbulent velocity increases with radius. Our results thus widen the possibilities to constrain interstellar medium parameters using observations of magnetic fields. This work is a step toward systematic statistical tests of galactic dynamo theory. Such studies are becoming more and more feasible as larger data sets are acquired using current and up-and-coming instruments.
THE CRAB PULSAR AT CENTIMETER WAVELENGTHS. II. SINGLE PULSES
Authors: Hankins T. H. , Eilek J. A. , Jones G.
Published: December 2016

We have carried out new, high-frequency, high-time-resolution observations of the Crab pulsar. Combining these with our previous data, we characterize bright single pulses associated with the Main Pulse, both the Low-Frequency and High-Frequency Interpulses, and the two  High-Frequency Components. Our data include observations at frequencies ranging from 1 to 43 GHz with time resolutions down to a fraction of a nanosecond. We find that at least two types of emission physics are operating in this pulsar. Both Main Pulses and Low-Frequency Interpulses, up to ∼10 GHz, are characterized by nanoshot emission—overlapping clumps of narrowband nanoshots, each with its own polarization signature. High-Frequency Interpulses, between 5 and 30 GHz, are characterized by spectral band emission—linearly polarized emission containing ∼30 proportionately spaced spectral bands. We cannot say whether the longer-duration High-Frequency Components pulses are due to a scattering process, or if they come from yet another type of emission physics.
LABORATORY MEASUREMENTS COMPELLINGLY SUPPORT A CHARGE-EXCHANGE MECHANISM FOR THE “DARK MATTER” ∼3.5 keV X-Ray LINE
Authors: Shah Chintan , Dobrodey Stepan , Bernitt Sven , Steinbrügge René , López-Urrutia José R. Crespo , Gu Liyi , Kaastra Jelle
Published: December 2016

The reported observations of an unidentified X-ray line feature at ∼3.5 keV have driven a lively discussion about its possible dark matter origin. Motivated by this, we have measured the K-shell X-ray spectra of highly ionized bare sulfur ions following charge exchange with gaseous molecules in an electron beam ion trap, as a source of or a contributor to this X-ray line. We produced S16+ and S15+ ions and let them capture electrons in collision with those molecules with the electron beam turned off while recording X-ray spectra. We observed a charge-exchange-induced X-ray feature at the Lyman series limit (3.47 ± 0.06 keV). The inferred X-ray energy is in full agreement with the reported astrophysical observations and supports the novel scenario proposed by Gu et al.
THE COS-HALOS SURVEY: ORIGINS OF THE HIGHLY IONIZED CIRCUMGALACTIC MEDIUM OF STAR-FORMING GALAXIES
Authors: Werk Jessica K. , Prochaska J. Xavier , Cantalupo Sebastiano , Fox Andrew J. , Oppenheimer Benjamin , Tumlinson Jason , Tripp Todd M. , Lehner Nicolas , McQuinn Matthew
Published: December 2016

The total contribution of diffuse halo gas to the galaxy baryon budget strongly depends on its dominant ionization state. In this paper, we address the physical conditions in the highly ionized circumgalactic medium (CGM) traced by

absorption lines observed in COS-Halos spectra. We analyze the observed ionic column densities, absorption-line widths and relative velocities, along with the ratios of

/

for 39 fitted Voigt profile components of O vi. We compare these quantities with the predictions given by a wide range of ionization models. Photoionization models that include only extragalactic UV background radiation are ruled out; conservatively, the upper limits to

/

and measurements of

imply unphysically large path lengths ≳100 kpc. Furthermore, very broad

absorption (b > 40 km s−1) is a defining characteristic of the CGM of star-forming L* galaxies. We highlight two possible origins for the bulk of the observed

: (1) highly structured gas clouds photoionized primarily by local high-energy sources or (2) gas radiatively cooling on large scales behind a supersonic wind. Approximately 20% of circumgalactic O vi does not align with any low-ionization state gas within ±50 km s−1 and is found only in halos with

< 1012

. We suggest that this type of unmatched O vi absorption traces the hot corona itself at a characteristic temperature of

K. We discuss the implications of these very distinct physical origins for the dynamical state, gas cooling rates, and total baryonic content of L* gaseous halos.
INDICATION OF THE BLACK HOLE POWERED JET IN M87 BY VSOP OBSERVATIONS
Authors: Asada Keiichi , Nakamura Masanori , Pu Hung-Yi
Published: December 2016

In order to study the collimation and acceleration mechanism of relativistic jets, the jet streamline of M87 at milliarcsecond scale is extensively investigated with images from VSOP observations at 1.6 and 5 GHz. Thanks to the higher angular resolution of VSOP, especially in the direction transverse to the jet, we resolved the jet streamline into three ridgelines at the scale of milli arcseconds. While the properties of the outer two ridgelines are in good agreement with those measured in previous observations and can be expressed by one power-law line with a power law index of 1.7, an inner ridgeline is clearly observed for the first time. We compared the measured size with the outermost streamline expected by Blandford & Znajek's parabolic solutions, which are anchored at the event horizon, with different black hole spin parameters. We revealed that the observed inner ridgeline is narrower than the prediction, suggesting the origin of the inner ridgeline to be part of a spine originating from the spinning black hole. The inner ridgeline becomes very dim at large distances from the central engine at 5 GHz. We considered two possible cases for this; Doppler beaming and/or radiative cooling. Either case seems to be reasonable for its explanation, and future multi-frequency observations will discriminate those two possibilities.
THE DETECTION OF DIFFUSE EXTENDED STRUCTURE IN 3C 273: IMPLICATIONS FOR JET POWER
Authors: Punsly Brian , Kharb Preeti
Published: December 2016

We present deep Very Large Array imaging of 3C 273 in order to determine the diffuse, large scale radio structure of this famous radio-loud quasar. Diffuse extended structure (radio lobes) is detected for the first time in these observations as a consequence of high dynamic range in the 327.5 and 1365 MHz images. This emission is used to estimate a time averaged jet power, 7.2 × 1043 erg s−1 < 

 < 3.7 × 1044 erg s−1. Brightness temperature arguments indicate consistent values of the time variability Doppler factor and the compactness Doppler factor for the inner jet, δ ≳ 10. Thus, the large apparent broadband bolometric luminosity of the jet, ∼3 × 1046 erg s−1, corresponds to a modest intrinsic luminosity ≳1042 erg s−1, or ∼1% of

. In summary, we find that 3C 273 is actually a “typical” radio-loud quasar contrary to suggestions in the literature. The modest

is near the peak of the luminosity distribution for radio-loud quasars and it is consistent with the current rate of dissipation emitted from millimeter wavelengths to gamma rays. The extreme core-jet morphology is an illusion from a near pole-on line of sight to a highly relativistic jet that produces a Doppler enhanced glow that previously swamped the lobe emission. 3C 273 apparently has the intrinsic kpc scale morphology of a classical double radio source, but it is distorted by an extreme Doppler aberration.
ULTRAVIOLET HALOS AROUND SPIRAL GALAXIES. I. MORPHOLOGY
Authors: Hodges-Kluck Edmund , Cafmeyer Julian , Bregman Joel N.
Published: December 2016

We examine ultraviolet halos around a sample of highly inclined galaxies within 25 Mpc to measure their morphology and luminosity. Despite contamination from galactic light scattered into the wings of the point-spread function, we find that ultraviolet (UV) halos occur around each galaxy in our sample. Around most galaxies the halos form a thick, diffuse disk-like structure, but starburst galaxies with galactic superwinds have qualitatively different halos that are more extensive and have filamentary structure. The spatial coincidence of the UV halos above star-forming regions, the lack of consistent association with outflows or extraplanar ionized gas, and the strong correlation between the halo and galaxy UV luminosity suggest that the UV light is an extragalactic reflection nebula. UV halos may thus represent 106–107
M
⊙ of dust within 2–10 kpc of the disk, whose properties may change with height in starburst galaxies.
THE ROLE OF STAR FORMATION AND AGN IN DUST HEATING OF Z = 0.3–2.8 Galaxies. II. INFORMING IR AGN FRACTION ESTIMATES THROUGH SIMULATIONS
Authors: Roebuck Eric , Sajina Anna , Hayward Christopher C. , Pope Alexandra , Kirkpatrick Allison , Hernquist Lars , Yan Lin
Published: December 2016

A key question in extragalactic studies is the determination of the relative roles of stars and active galactic nuclei (AGNs) in powering dusty galaxies at z ∼ 1–3 where the bulk of star formation and AGN activity took place. In Paper I, we present a sample of 336 24 μm selected (Ultra)Luminous Infrared Galaxies, (U)LIRGs, at

–2.8, where we focus on determining the AGN contribution to the IR luminosity. Here, we use hydrodynamic simulations with dust radiative transfer of isolated and merging galaxies to investigate how well the simulations reproduce our empirical IR AGN fraction estimates and determine how IR AGN fractions relate to the UV-mm AGN fraction. We find that: (1) IR AGN fraction estimates based on simulations are in qualitative agreement with the empirical values when host reprocessing of the AGN light is considered; (2) for star-forming galaxy (SFG)–AGN composites our empirical methods may be underestimating the role of AGN, as our simulations imply

AGN fractions,

higher than previous estimates; (3) 6% of our empirically classified SFGs have AGN fractions ≳50%. While this is a small percentage of SFGs, if confirmed it would imply that the true number density of AGNs may be underestimated; (4) this comparison depends on the adopted AGN template—those that neglect the contribution of warm dust lower the empirical fractions by up to two times; and (5) the IR AGN fraction is only a good proxy for the intrinsic UV-mm AGN fraction when the extinction is high (

or up to and including coalescence in a merger).
ASSOCIATION OF 3He-RICH SOLAR ENERGETIC PARTICLES WITH LARGE-SCALE CORONAL WAVES
Authors: Bučík Radoslav , Innes Davina E. , Mason Glenn M. , Wiedenbeck Mark E.
Published: December 2016

Small, 3He-rich solar energetic particle (SEP) events have been commonly associated with extreme-ultraviolet (EUV) jets and narrow coronal mass ejections (CMEs) that are believed to be the signatures of magnetic reconnection, involving field lines open to interplanetary space. The elemental and isotopic fractionation in these events are thought to be caused by processes confined to the flare sites. In this study, we identify 32 3He-rich SEP events observed by the Advanced Composition Explorer, near the Earth, during the solar minimum period 2007–2010, and we examine their solar sources with the high resolution Solar Terrestrial Relations Observatory (STEREO) EUV images. Leading the Earth, STEREO-A has provided, for the first time, a direct view on 3He-rich flares, which are generally located on the Sun’s western hemisphere. Surprisingly, we find that about half of the 3He-rich SEP events in this survey are associated with large-scale EUV coronal waves. An examination of the wave front propagation, the source-flare distribution, and the coronal magnetic field connections suggests that the EUV waves may affect the injection of 3He-rich SEPs into interplanetary space.
SUPERNOVAE POWERED BY MAGNETARS THAT TRANSFORM INTO BLACK HOLES
Authors: Moriya Takashi J. , Metzger Brian D. , Blinnikov Sergei I.
Published: December 2016

Rapidly rotating, strongly magnetized neutron stars (NSs; magnetars) can release their enormous rotational energy via magnetic spin-down, providing a power source for bright transients such as superluminous supernovae (SNe). On the other hand, particularly massive (so-called supramassive) NSs require a minimum rotation rate to support their mass against gravitational collapse, below which the NS collapses to a black hole (BH). We model the light curves (LCs) of SNe powered with magnetars that transform into BHs. Although the peak luminosities can reach high values in the range of superluminous SNe, their post maximum LCs can decline very rapidly because of the sudden loss of the central energy input. Early BH transformation also enhances the shock breakout signal from the magnetar-driven bubble relative to the main SN peak. Our synthetic LCs of SNe powered by magnetars transforming to BHs are consistent with those of some rapidly evolving bright transients recently reported by Arcavi et al.
CORONAL DYNAMIC ACTIVITIES IN THE DECLINING PHASE OF A SOLAR CYCLE
Authors: Jang Minhwan , Woods T. N. , Hong Sunhak , Choe G. S.
Published: December 2016

It has been known that some solar activity indicators show a double-peak feature in their evolution through a solar cycle, which is not conspicuous in sunspot number. In this Letter, we investigate the high solar dynamic activity in the declining phase of the sunspot cycle by examining the evolution of polar and low-latitude coronal hole (CH) areas, splitting and merging events of CHs, and coronal mass ejections (CMEs) detected by SOHO/LASCO C3 in solar cycle 23. Although the total CH area is at its maximum near the sunspot minimum, in which polar CHs prevail, it shows a comparable second maximum in the declining phase of the cycle, in which low-latitude CHs are dominant. The events of CH splitting or merging, which are attributed to surface motions of magnetic fluxes, are also mostly populated in the declining phase of the cycle. The far-reaching C3 CMEs are also overpopulated in the declining phase of the cycle. From these results we suggest that solar dynamic activities due to the horizontal surface motions of magnetic fluxes extend far in the declining phase of the sunspot cycle.
AN ACTIVE, ASYNCHRONOUS COMPANION TO A REDBACK MILLISECOND PULSAR
Authors: Staden André D. van , Antoniadis John
Published: December 2016

PSR J1723−2837 is a “redback” millisecond pulsar (MSP) with a low-mass companion in a 14.8 hr orbit. The system’s properties closely resemble those of “transitional” MSPs that alternate between spin-down and accretion-powered states. In this Letter, we report on long-term photometry of the 15.5 mag companion to the pulsar. We use our data to illustrate that the star experiences sporadic activity, which we attribute to starspots. We also find that the companion is not tidally locked and infer

for the ratio between the rotational and orbital periods. Finally, we place constraints on various parameters, including the irradiation efficiency and pulsar mass. We discuss similarities with other redback MSPs and conclude that starspots may provide the most likely explanation for the often seen irregular and asymmetric optical light curves.
L’unité dans la diversité
Authors: Lamy Pascal , Pinel Jean-Pierre
Published: December 2016

L’entretien porte d’abord sur les spécificités des rapports à la conflictualité tels qu’ils se déploient dans les espaces nationaux, européens et internationaux. Il dégage leurs rapports à la structure organisationnelle et à la culture intériorisée par les acteurs. Il traite en suite de l’actualité de la situation européenne, dont le Brexit est un symptôme. Il caractérise les défauts de récits susceptibles de mobiliser l’imaginaire des Européens et pointe les paradoxes fondateurs et actuels qui pèsent sur la construction de l’Union européenne. Il se clôt sur les singularités de la situation française en éclairant les sources de la profonde dépression qui la traverse.
À propos de L’individu ingouvernable
Authors: Gori Roland , Tapia Claude
Published: December 2016

De cet entretien-débat à propos du dernier ouvrage de Roland Gori, ressort principalement la dénonciation vigoureuse par celui-ci des excès du néo-libéralisme lequel contiendrait en germes des dérives néo-fascistes de nature à corrompre le système et les valeurs démocratiques. Cette dénonciation s’accompagne d’une mise en cause de la sur-modernité, terreau, selon lui, favorable à l’exacerbation de l’individualisme et du narcissisme chez une fraction importante des membres de notre société ; celle-ci affectée par le technicisme ambiant et les pressions à l’uniformité, signes annonciateurs d’une évolution vers une organisation totalitaire, susceptible de dégénérer en « désert politique ». Un certain consensus s’est établi au cours du débat sur l’idée d’un primat de l’éthique et de l’humain et sur la préservation et même la stimulation des forces de résistance aussi bien aux conditionnements émanant de l’univers techno-libéral qu’aux menaces des fascismes meurtriers et des réseaux d’information interconnectés déshumanisants. S’il fallait relever un décalage entre les points de vue exprimés, celui-ci ne concernerait que l’évaluation de la nocivité de certains aspects de la sur-modernité et l’étendue des domaines culturels ou sociaux affectés par un ultralibéralisme incontrôlé. Émerge, enfin, de l’entretien une égale conviction concernant la pérennité de la fonction émancipatrice et humanisante de la psychanalyse.
Histoire et temporalité chez une patiente schizophrène « institutionnalisée »
Authors: Kapsambelis Vassilis
Published: December 2016

L’évocation détaillée de l’histoire d’une patiente schizophrène grave et du travail thérapeutique avec elle permet d’interroger un certain nombre de manifestations cliniques, qui semblent constituer des reviviscences, sous forme de fausses reconnaissances, de traces mnésiques de son passé. Ces reviviscences, qui sollicitent donc fortement l’activité perceptive, y compris au sens hallucinatoire, se manifestent en lieu et place du souvenir, alors que ce dernier semble nécessaire à la constitution d’une temporalité et d’une histoire personnelle. Le travail thérapeutique a consisté à ce que ces reviviscences soient progressivement ramenées à une meilleure connaissance, de la part de l’équipe soignante, des personnes et situations impliquées dans les reviviscences, ce qui, à son tour, a donné accès à une narrativité qui s’est progressivement mise en place au fur et à mesure que les manifestations psychotiques diminuaient.
Conflictualité et travail de l’intermédiaire… dans un chantier d’insertion par le travail
Authors: Beucler Quentin
Published: December 2016

Dans le secteur de l’insertion, chargé de constituer une passerelle entre marge et norme, la qualité des formations intermédiaires apparaît comme centrale, autant au niveau intra-, inter- que transsubjectif. Cet article aborde la question de la conflictualité de ces formations intermédiaires. En explorant plusieurs aspects d’une recherche dans un chantier d’insertion, est décrit le cas d’une institution ayant du mal à se constituer dans son rôle d’intermédiaire. Si une défense phallique face à la déliaison semble se partager majoritairement entre salariés en insertion, les échanges entre professionnels sont en revanche a-conflictuels. Sont alors abordés la manière dont sont perturbés le préconscient et l’interpersonnel pour le chercheur comme pour les professionnels dans leur travail auprès des personnes accueillies.
Le psychanalyste et le fracas terroriste
Authors: Kac Ohana Nicole
Published: December 2016

Dans le contexte terroriste actuel, cette réflexion porte sur nos possibilités de fonctionnement en tant que psychanalystes, en particulier sur notre écoute, nécessairement modifiée, transformée voire « transformationnelle ». Les identifications à l’agresseur, notamment les théories du complot, montrent l’attraction voire l’incorporation de leur omnipotence. L’intrication, parfois le télescopage du trauma collectif avec l’histoire personnelle des patients est discutée.
Naissances de la sexualité
Authors: André Jacques
Published: December 2016

Naissances de la sexualité , en trois temps. Le premier, préhistorique, rappelle que la sexualité humaine naît de son émancipation vis-à-vis de l’instinct, quand se dissocient sexualité et reproduction, sans doute en relation avec l’acquisition du langage articulé. Le deuxième temps est freudien, il correspond à l’invention du couple sexualité infantile – inconscient et à la dissociation cette fois entre sexuel et génital. Le troisième temps est moins temps qu’un mouvement, celui qui ramène la sexualité d’aujourd’hui plus vers la pulsion que vers l’objet.