bluuebunny/crossref_metadata_2025_split huggingface dataset:
ON THE PROPERTIES OF SLOW MHD SAUSAGE WAVES WITHIN SMALL-SCALE PHOTOSPHERIC MAGNETIC STRUCTURES
Authors: Freij N. , Dorotovič I. , Morton R. J. , Ruderman M. S. , Karlovský V. , Erdélyi R. 
Published: January 2016

ABSTRACT
The presence of magnetoacoustic waves in magnetic structures in the solar atmosphere is well-documented. Applying the technique of solar magneto-seismology (SMS) allows us to infer the background properties of these structures. Here, we aim to identify properties of the observed magnetoacoustic waves and study the background properties of magnetic structures within the lower solar atmosphere. Using the Dutch Open Telescope and Rapid Oscillations in the Solar Atmosphere instruments, we captured two series of high-resolution intensity images with short cadences of two isolated magnetic pores. Combining wavelet analysis and empirical mode decomposition (EMD), we determined characteristic periods within the cross-sectional (i.e., area) and intensity time series. Then, by applying the theory of linear magnetohydrodynamics (MHD), we identified the mode of these oscillations within the MHD framework. Several oscillations have been detected within these two magnetic pores. Their periods range from 3 to 20 minutes. Combining wavelet analysis and EMD enables us to confidently find the phase difference between the area and intensity oscillations. From these observed features, we concluded that the detected oscillations can be classified as slow sausage MHD waves. Furthermore, we determined several key properties of these oscillations such as the radial velocity perturbation, the magnetic field perturbation, and the vertical wavenumber using SMS. The estimated range of the related wavenumbers reveals that these oscillations are trapped within these magnetic structures. Our results suggest that the detected oscillations are standing harmonics, and this allows us to estimate the expansion factor of the waveguides by employing SMS. The calculated expansion factor ranges from 4 to 12.
TIME DEPENDENT NONEQUILIBRIUM IONIZATION OF TRANSITION REGION LINES OBSERVED WITH IRIS
Authors: Martínez-Sykora Juan , Pontieu Bart De , Hansteen Viggo H. , Gudiksen Boris 
Published: January 2016

ABSTRACT
The properties of nonstatistical equilibrium ionization of silicon and oxygen ions are analyzed in this work. We focus on five solar targets (quiet Sun; coronal hole; plage; quiescent active region, AR; and flaring AR) as observed with the Interface Region Imaging Spectrograph (IRIS). IRIS is best suited for this work owing to the high cadence (up to 0.5 s), high spatial resolution (up to 0.″32), and high signal-to-noise ratios for O iv λ1401 and Si iv λ1402. We find that the observed intensity ratio between lines of three times ionized silicon and oxygen ions depends on their total intensity and that this correlation varies depending on the region observed (quiet Sun, coronal holes, plage, or active regions) and on the specific observational objects present (spicules, dynamic loops, jets, microflares, or umbra). In order to interpret the observations, we compare them with synthetic profiles taken from 2D self-consistent radiative MHD simulations of the solar atmosphere, where the statistical equilibrium or nonequilibrium treatment of silicon and oxygen is applied. These synthetic observations show vaguely similar correlations to those in the observations, i.e., between the intensity ratios and their intensities, but only in the nonequilibrium case do we find that (some of) the observations can be reproduced. We conclude that these lines are formed out of statistical equilibrium. We use our time-dependent nonequilibrium ionization simulations to describe the physical mechanisms behind these observed properties.
OBSERVATIONAL SIGNATURES OF CORONAL LOOP HEATING AND COOLING DRIVEN BY FOOTPOINT SHUFFLING
Authors: Dahlburg R. B. , Einaudi G. , Taylor B. D. , Ugarte-Urra I. , Warren H. P. , Rappazzo A. F. , Velli M. 
Published: January 2016

ABSTRACT
The evolution of a coronal loop is studied by means of numerical simulations of the fully compressible three-dimensional magnetohydrodynamic equations using the HYPERION code. The footpoints of the loop magnetic field are advected by random motions. As a consequence, the magnetic field in the loop is energized and develops turbulent nonlinear dynamics characterized by the continuous formation and dissipation of field-aligned current sheets: energy is deposited at small scales where heating occurs. Dissipation is nonuniformly distributed so that only a fraction of the coronal mass and volume gets heated at any time. Temperature and density are highly structured at scales that, in the solar corona, remain observationally unresolved: the plasma of our simulated loop is multithermal, where highly dynamical hotter and cooler plasma strands are scattered throughout the loop at sub-observational scales. Numerical simulations of coronal loops of 50,000 km length and axial magnetic field intensities ranging from 0.01 to 0.04 T are presented. To connect these simulations to observations, we use the computed number densities and temperatures to synthesize the intensities expected in emission lines typically observed with the Extreme Ultraviolet Imaging Spectrometer on Hinode. These intensities are used to compute differential emission measure distributions using the Monte Carlo Markov Chain code, which are very similar to those derived from observations of solar active regions. We conclude that coronal heating is found to be strongly intermittent in space and time, with only small portions of the coronal loop being heated: in fact, at any given time, most of the corona is cooling down.
THE ENIGMATIC AND EPHEMERAL M DWARF SYSTEM KOI 6705: CHESHIRE CAT OR WILD GOOSE?
Authors: Eric Gaidos  , Mann Andrew W. , Ansdell Megan 
Published: January 2016

ABSTRACT
We confirm a 0.995 day periodic planetary transit-like signal, KOI 6705.01, in the Kepler light curve of the star KIC 6423922. Optical and infrared spectra show that this star is a mid M-type dwarf with an effective temperature

K, metallicity [Fe/H] = −0.08 ± 0.10, radius

R
⊙, and mass = 0.28 ± 0.05M
⊙. The star is

pc away and its space motion, rotation period, and lack of Hα emission indicate it is an older member of the “thin disk” population. On the other hand, the star exhibits excess infrared emission suggesting a dust disk more typical of a very young star. If the KOI 6705.01 signal is produced by a planet, the transit depth of 60 ppm means its radius is only

R
⊕, or about the size of the Moon. However, the duration (

hr) and time variation of KOI 6705.01 are anomalous: the signal was undetected in the first two years of the mission and increased through the latter two years. These characteristics require implausible orbits and material properties for any planet and rule out such an explanation, although a dust cloud is possible. We excluded several false positive scenarios including background stars, scattered light from stars that are nearby on the sky, and electronic cross-talk between detector readout channels. We find the most likely explanation to be that KOI 6705.01 is a false positive created by charge transfer inefficiency in a detector column on which KIC 6423922 and a 1.99 day eclipsing binary both happened to fall.
LUMINOSITY DEPENDENCE AND REDSHIFT EVOLUTION OF STRONG EMISSION-LINE DIAGNOSTICS IN STAR-FORMING GALAXIES*
Authors: Cowie L. L. , Barger A. J. , Songaila A. 
Published: January 2016

ABSTRACT
We examine the redshift evolution of standard strong emission-line diagnostics for Hβ-selected star-forming galaxies using the local SDSS sample and a new

sample obtained from Hubble Space Telescope WFC3 grism and Keck DEIMOS and MOSFIRE data. We use the SDSS galaxies to show that there is a systematic dependence of the strong emission-line properties on Balmer-line luminosity, which we interpret as showing that both the N/O abundance and the ionization parameter increase with increasing line luminosity. Allowing for the luminosity dependence tightens the diagnostic diagrams and the metallicity calibrations. The combined SDSS and high-redshift samples show that there is no redshift evolution in the line properties once the luminosity correction is applied, i.e., all galaxies with a given

) have similar strong emission-line distributions at all the observed redshifts. We argue that the best metal diagnostic for the high-redshift galaxies may be a luminosity-adjusted version of the [N ii]6584/Hα metallicity relation.
GLOBULAR CLUSTER SYSTEMS IN BRIGHTEST CLUSTER GALAXIES. II. NGC 6166
Authors: Harris William E. , Blakeslee John P. , Whitmore Bradley C. , Gnedin Oleg Y. , Geisler Douglas , Rothberg Barry 
Published: January 2016

ABSTRACT
We present new deep photometry of the globular cluster system (GCS) around NGC 6166, the central supergiant galaxy in Abell 2199. Hubble Space Telescope data from the Advanced Camera for Surveys and WFC3 cameras in F475W and F814W are used to determine the spatial distribution of the GCS, its metallicity distribution function (MDF), and the dependence of the MDF on galactocentric radius and on GC luminosity. The MDF is extremely broad, with the classic red and blue subpopulations heavily overlapped, but a double-Gaussian model can still formally match the MDF closely. The spatial distribution follows a Sérsic-like profile detectably to a projected radius of at least R
gc = 250 kpc. To that radius, the total number of clusters in the system is N
GC = 39000 ± 2000, the global specific frequency is S

N
= 11.2 ± 0.6, and 57% of the total are blue, metal-poor clusters. The GCS may fade smoothly into the intracluster medium (ICM) of A2199; we see no clear transition from the core of the galaxy to the cD halo or the ICM. The radial distribution, projected ellipticity, and mean metallicity of the red (metal-richer) clusters match the halo light extremely well for

, both of them varying as

. By comparison, the blue (metal-poor) GC component has a much shallower falloff

and a more nearly spherical distribution. This strong difference in their density distributions produces a net metallicity gradient in the GCS as a whole that is primarily generated by the population gradient. With NGC 6166 we appear to be penetrating into a regime of high enough galaxy mass and rich enough environment that the bimodal two-phase description of GC formation is no longer as clear or effective as it has been in smaller galaxies.
ISOTROPY CONSTRAINTS ON POWERFUL SOURCES OF ULTRAHIGH-ENERGY COSMIC RAYS AT 1019 eV
Authors: Takami Hajime , Murase Kohta , Dermer Charles D. 
Published: January 2016

ABSTRACT
Anisotropy in the arrival direction distribution of ultrahigh-energy cosmic rays (UHECRs) produced by powerful sources is numerically evaluated. We show that nondetection of significant anisotropy at

eV at present and in future experiments imposes general upper limits on UHECR proton luminosity of steady sources as a function of source redshifts. The upper limits constrain the existence of typical steady

eV UHECR sources in the local universe and limit their local density to

Mpc

assuming average intergalactic magnetic fields less than

G. This isotropy, being stronger than that measured at the highest energies, may indicate the transient generation of UHECRs. Our calculations are applied for extreme high-frequency-peaked BL Lacertae objects 1ES 0229+200, 1ES 1101–232, and 1ES 0347–121, to test the UHECR-induced cascade model, in which beamed UHECR protons generate TeV radiation in transit from sources. While the magnetic-field structure surrounding the sources affects the required absolute cosmic-ray luminosity of the blazars, the magnetic-field structure surrounding the Milky Way directly affects the observed anisotropy. If these magnetic fields are weak enough, significant UHECR anisotropy from these blazars is detectable by the Pierre Auger Observatory unless the maximum energy of UHECR protons is below 1019 eV. Furthermore, if these are the sources of UHECRs above 1019 eV, a local magnetic structure surrounding the Milky Way is needed to explain the observed isotropy at

eV, which may be incompatible with large magnetic structures around all galaxies for the UHECR-induced cascade model to work with reasonable jet powers.
A HARD GAMMA-RAY FLARE FROM 3C 279 IN 2013 DECEMBER
Authors: Paliya Vaidehi S. , Diltz Chris , Böttcher Markus , Stalin C. S. , Buckley David 
Published: January 2016

ABSTRACT
The blazar 3C 279 exhibited twin γ-ray flares of similar intensity in 2013 December and 2014 April. In this work, we present a detailed multi-wavelength analysis of the 2013 December flaring event. Multi-frequency observations reveal the uncorrelated variability patterns with X-ray and optical–UV fluxes peaking after the γ-ray maximum. The broadband spectral energy distribution (SED) at the peak of the γ-ray activity shows a rising γ-ray spectrum but a declining optical–UV flux. This observation along with the detection of uncorrelated variability behavior rules out the one-zone leptonic emission scenario. We, therefore, adopt two independent methodologies to explain the SED: a time-dependent lepto-hadronic modeling and a two-zone leptonic radiative modeling approach. In the lepto-hadronic modeling, a distribution of electrons and protons subjected to a randomly orientated magnetic field produces synchrotron radiation. Electron synchrotron is used to explain the IR to UV emission while proton synchrotron emission is used to explain the high-energy γ-ray emission. A combination of both electron synchrotron self-Compton emission and proton synchrotron emission is used to explain the X-ray spectral break seen during the later stage of the flare. In the two-zone modeling, we assume a large emission region emitting primarily in IR to X-rays and γ-rays to come primarily from a fast-moving compact emission region. We conclude by noting that within a span of four months, 3C 279 has shown the dominance of a variety of radiative processes over each other and this reflects the complexity involved in understanding the physical properties of blazar jets in general.
A GeV SOURCE IN THE DIRECTION OF SUPERNOVA REMNANT CTB 37B
Authors: Xin Yu-Liang , Liang Yun-Feng , Li Xiang , Yuan Qiang , Liu Si-Ming , Wei Da-Ming 
Published: January 2016

ABSTRACT
Supernova remnants (SNRs) are the most attractive candidates for the acceleration sites of Galactic cosmic rays. We report the detection of GeV γ-ray emission with the Pass 8 events recorded by the Fermi Large Area Telescope (Fermi-LAT) in the vicinity of the shell-type SNR CTB 37B that is likely associated with the TeV γ-ray source HESS J1713–381. The photon spectrum of CTB 37B is consistent with a power law with an index of 1.89 ± 0.08 in the energy range of 0.5–500 GeV, and the measured flux connects smoothly with that of HESS J1713–381 at a few hundred GeV. No significant spatial extension and time variation are detected. The multi-wavelength data can be well fitted with either a leptonic model or a hadronic one. However, parameters of both models suggest more efficient particle acceleration than typical SNRs. Meanwhile, the X-ray and γ-ray spectral properties of CTB 37B show that it is an interesting source bridging young SNRs dominated by non-thermal emission and old SNRs interacting with molecular clouds.
Checklist of the subfamily Adoncholaiminae Gerlach and Riemann, 1974 (Nematoda: Oncholaimida: Oncholaimidae) of the world: genera, species, distribution, and reference list for taxonomists and ecologists
Authors: Shimada Daisuke 
Published: January 2016

Adoncholaiminae is one of the seven subfamilies in the free-living aquatic nematode family Oncholaimidae. Nematodes in Adoncholaiminae are found from various water environment of the world. However, a checklist of all Adoncholaiminae species including full literature, especially information of experimental (not taxonomic) works, has not been updated for more than 40 years.
A revised checklist of the subfamily Adoncholaiminae of the world is provided. It contains 31 valid and 13 invalid species names in four genera with synonyms, collection records, and full literature from 1860's to 2015 for each species. A literature survey of total 477 previous papers was conducted in this work, and 362 of them are newly added to checklist.
New records of chalcidid (Hymenoptera: Chalcididae) pupal parasitoids from India
Authors: Gowri Prakash , Manickavasagam Sagadai , Kanagarajan Rasappan 
Published: January 2016

Chalcidids are one of the most important parasitoids of pupae of agriculturally important pests belonging to orders like Lepidoptera, Diptera, Coleoptera and Hymenoptera. Such an important group has not been studied consistently by any team of workers from any country apart from the notable contributions by Boucek, Steffan, Delvare and Narendran. (Boucek 1988, Steffan 1973, Delvare 1992 and Narendran 1989). On a personal note, Dr. John S Noyes of Natural History Museum London agrees with this view as expressed with the second author and hence we felt that we can initiate further work on this group within India. We currently hold hundreds of unidentified specimens of this family in our department collection confirming that we will have much work to do over a long period of time.
New distribution records of Chalcididae from Andhra Pradesh (Brachymeria megaspila, B. minuta, Dirhinus anthracia and D. auratus), Bihar (B. podagrica, B. excarinata, B. hearseyi, D. anthracia, D. auratus, D. pilifer, Epitranus erythrogaster and Psilochalcis carinigena), Karnataka (B. apicicornis), Manipur (B. euploeae, D. auratus and E. erythrogaster), Mizoram (B. euploeae and D. anthracia), Nagaland (B. euploeae), Himachal Pradesh (B. alternipes), and Tamil Nadu (B. apicicornis, D. anthracia, D. deplanatus, D. pilifer, D. bakeri, E. observator, E. elongatulus, P. keralensis and P. soudanensis) and union territories Andaman & Nicobar Islands (B. podagrica, B. excarinata, E. erythrogaster and P. carinigena) and Pudhucherry (B. albicrus, D. anthracia, D. auratus, E. erythrogaster and P. kerelensis) are documented from the unidentified material mentioned above.
Séduire à l’ère du numérique : une séduction polymorphe à l’adolescence
Authors: Tordo Frédéric 
Published: January 2016

La séduction est un procédé visant à susciter délibérément l’admiration, l’attirance, voire l’amour d’un individu. À l’adolescence, le numérique est un révélateur des différentes formes de la séduction. La plupart du temps, l’adolescent séduit l’autre, ou est séduit par lui, par une image, mais il est aussi régulièrement trompé par un individu qui se présente autrement que ce qu’il est, jouant avec les outils caractéristiques de la communication numérique. Aussi, le numérique féconde la séduction en son double sens : attirer un autre vers soi, mais aussi le conduire ailleurs, le tromper ou le détourner. La « séduction numérique » est alors polymorphe dans ses expressions, dans la mesure où elle est gouvernée par des exigences différentes : sexuelle, amoureuse, mais encore traumatique et narcissique.
Les voi(x)es de la séduction
Authors: Ferveur Christophe 
Published: January 2016

De la séduction biblique originelle à la situation psychothérapique, le « grain » de la voix, sa matière, mobilise les enjeux complexes de la séduction, à la fois dans ce qu’il offre d’expressivité pour habiter une parole affectée, mais aussi dans ses potentialités d’évocation du trauma. Se laisser séduire, goûter au plaisir de l’écoute entre le son et le sens, est toujours promesse d’entendre autrement ce qui se dit sans se dire.
Pluralité des ressources pour l’action dans les processus de transition formation-emploi chez les enseignants du secondaire
Authors: Perez-Roux Thérèse , Lanéelle Xavière 
Published: January 2016

La recherche s’inscrit dans une perspective sociologique à visée compréhensive. Elle s’intéresse aux processus de construction de la professionnalité enseignante, aux dynamiques d’insertion professionnelle et aux ressources plurielles mobilisées par les néo-enseignants du secondaire. La méthodologie de l’enquête est double : quantitative avec un questionnaire mis en ligne entre février et avril 2013 (n=160), qualitative avec 12 entretiens semi-directifs conduits avec des fonctionnaires-stagiaires de différentes disciplines. Les résultats mettent en lumière un système de ressources mobilisant normes institutionnelles relayées par la formation initiale et continue, cultures professionnelles plus ou moins partagées et formes de soutien dans lesquelles le rapport au tuteur prend une place essentielle. On constate que « l’idéal du métier » sert à orienter l’activité. Les élèves, bien que parfois déroutants, constituent aussi une ressource essentielle.
Les ressources exploitées par les enseignants d’EPS au cours de leur première année d’expérience professionnelle : Analyse et perspectives pour la formation
Authors: Adé David , Gal-Petitfaux Nathalie , Serres Guillaume 
Published: January 2016

Cette recherche étudie l’activité de cinq enseignants fonctionnaires stagiaires (FS) en Éducation physique et sportive au cours de leur première année de prise de fonction dans le but d’identifier les ressources qu’ils mobilisent pour appréhender leur situation professionnelle. Elle a été conduite dans le cadre théorique et méthodologique du cours d’action (Theureau, 2004, 2006 et 2009). Deux types de données ont été recueillis : des données d’expérience sous la forme de « Web Récit » et des données de verbalisation lors d’entretiens de remise en situation. Les résultats mettent en avant la grande diversité des ressources mobilisées, dont une pluralité de formes d’expérience jouant aussi ce rôle de ressources. La nature et les modalités d’usage de ces ressources montrent que les FS accordent un primat aux savoirs subordonnés à leur action professionnelle. Sur cette base, des pistes pour la formation sont envisagées.
Le genre dans la crise, ou ce qui arrive aux « femmes » dans les temps difficiles
Authors: Avdela Efi , Morichon Danielle 
Published: January 2016

L’article soutient à partir du cas grec que la crise économique actuelle, tout en affectant de manière disproportionnée les femmes, rend le genre invisible. En se focalisant sur les « femmes qui travaillent », Efi Avdela montre que cela n’a pas toujours été le cas : durant l’entre-deux-guerres, par exemple, les contenus attribués à la différence des sexes étaient politisés et le genre était visible. Le manque actuel de visibilité du genre consacre son sens en tant que différence naturelle, dissimulant les structures de pouvoir genrées qui répartissent et légitiment les conséquences sociales et politiques de la crise. Enfin, l’auteure soutient qu’il existe une relation entre l’invisibilité du genre et la place marginale des études sur le genre dans une grande partie des sciences sociales de la Grèce contemporaine.