bluuebunny/crossref_metadata_2025 huggingface dataset:
Baryon Number Transfer Could Delay Quark–Hadron Transition in Cosmology
Authors: Bonometto Silvio , Mainini Roberto
Published: December 2016

In the early Universe, strongly interacting matter was a quark–gluon plasma. Both lattice computations and heavy ion collision experiments, however, tell us that, in the absence of chemical potentials, no plasma survives at T < ∼ 150 MeV. The cosmological Quark–Hadron transition, however, seems to have been a crossover; cosmological consequences envisaged when it was believed to be a phase transition no longer hold. In this paper, we discuss whether even a crossover transition can leave an imprint that cosmological observations can seek or, vice versa, if there are questions cosmology should address to QCD specialists. In particular, we argue that it is still unclear how baryons (not hadrons) could form at the cosmological transition. A critical role should be played by diquark states, whose abundance in the early plasma needs to be accurately evaluated. We estimate that, if the number of quarks belonging to a diquark state, at the beginning of the cosmological transition, is < ∼ 1 : 10 6 , its dynamics could be modified by the process of B-transfer from plasma to hadrons. In turn, by assuming B-transfer to cause just mild perturbations and, in particular, no entropy input, we study the deviations from the tracking regime, in the frame of SCDEW models. We find that, in some cases, residual deviations could propagate down to primeval nuclesynthesis.
Note exégétique sur le fragment 2 de Parménide (DK 28 B2)
Authors: Castelnérac Benoît
Published: December 2016

Cette analyse textuelle du fr. 2 de Parménide (DK 28 B2) a pour principal objectif de démontrer que le verbe νοῆσαι (l. 2) doit être lu comme un infinitif actif ayant pour complément les propositions subordonnées introduites respectivement par ὅπως à la li. 3 et ὡς à la li. 5. Il est en outre suggéré que le De arte (II, 1-2), du corpus hippocratique, ainsi qu’un passage du Parménide de Platon (136a-c) ont des points communs avec le fr. 2.
Comment peut-on influencer le déroulement d’un procès ? La circulation de la parole autour des tribunaux
Authors: Bartzoka Alexandra
Published: December 2016

Les Athéniens avaient construit un système légal destiné à réglementer les relations entre les composantes de la cité et à faire respecter ses lois. Mais, au-delà de ce cadre réglementé, il existait un mécanisme aux frontières de la formalité et de l’informalité qui intervenait pour déterminer si une action allait être traduite devant la justice ou pour influencer le jugement même d’un procès. On se propose d’examiner ici la diversité de ces relations développées à l’occasion d’un procès, sur la base des sources attiques, qui sont riches en exemples révélant la façon dont les informations pouvaient circuler autour des cours de justice.
Du nouveau sur la mort de Cléopâtre : au croisement de l’histoire des textes et de l’histoire de l’art
Authors: Boudon-Millot Véronique
Published: December 2016

Un nouveau témoignage tiré du traité pseudo-galénique Sur la thériaque à Pison (De theriaca ad Pisonem, Kühn XIV, 210-294) permet de restituer une nouvelle version des circonstances mystérieuses de la mort de la reine d’Égypte, Cléopâtre VII Philopator. Les sources antiques (parmi lesquelles Strabon est la plus ancienne) s’accordent en général pour affirmer que Cléopâtre se donna la mort en s’exposant à la morsure d’un cobra. Et quand ils mentionnent l’emplacement de la morsure, les auteurs anciens la situent au bras. L’iconographie du Moyen Âge et de la Renaissance a cependant privilégié la version de la morsure au sein, en vertu d’une tradition réputée inconnue de la littérature antique. Quelques lignes perdues en grec à un endroit où le texte est lacunaire, mais qui ont heureusement été préservées dans une traduction arabe permettent cependant d’affirmer que, d’après l’auteur du traité pseudo-galénique, Cléopâtre non seulement offrit son sein à la morsure du serpent, mais qui plus est son sein gauche, parce qu’elle savait parfaitement que le coeur se situe dans la partie gauche de la poitrine.
Flavius Philostrate biographe de Philostrate de Lemnos : fragments de vie d’un sophiste exemplaire ?
Authors: Robiano Patrick
Published: December 2016

Cet article vise à montrer, à travers les Vies de sophistes, qu’il faut prêter attention à Philostrate de Lemnos, sophiste brillant, auteur notamment d’une Lettre sur la manière d’écrire des lettres, publiée erronément par Kayser comme la Dialexis I de Flavius Philostrate. Il vise aussi à montrer comment Flavius Philostrate construit, à la manière d’un puzzle, l’image d’un sophiste presque exemplaire qui n’a pas toujours eu, cependant, la reconnaissance qu’il méritait et qu’il réhabilite en l’inscrivant, grâce à une composition subtile, dans le réseau des grands sophistes qu’il a distingués pour illustrer la Seconde Sophistique. L’épigraphie s’avère un outil précieux pour comprendre le milieu dans lequel vécut Philostrate de Lemnos.
Passions et raison dans les Prologues de Démosthène
Authors: Gotteland Sophie
Published: December 2016

Tout au long de ses Prologues, Démosthène souligne la place que tiennent les passions (πάθη) dans le débat politique et le danger qu’elles présentent pour la démocratie. Présentant ses rivaux comme des êtres de passions, gouvernés par l’ambition, la malveillance et les rancunes personnelles, critiquant une assemblée elle-même dominée par les émotions et sensible à ceux qui flattent ses désirs, il dénonce l’absence de délibérations rationnelles et d’un véritable exercice de la raison. Cette analyse de la place des passions dans le débat politique lui permet également de définir, à l’inverse, ce que doit être la parole du conseiller et de faire l’éloge de sa propre pratique oratoire. La position de Démosthène n’est pourtant pas dénuée d’une apparente ambiguïté. Bien qu’il présente le parfait orateur comme un être de raison, bien qu’il demande à son auditoire de modeler son comportement sur le sien, il n’hésite pas, en effet, à faire parfois lui aussi appel aux sentiments. L’expression de ses émotions est alors revendiquée comme la meilleure preuve de son dévouement à la cité.
La désignation de suppléants par tirage au sort (ἐπιλαχών) dans l’Athènes classique
Authors: Laffon Amarande
Published: December 2016

The procedure for appointment of substitutes is known through rare instances of the verb ἐπιλαγχάνω. The bibliography is mainly based on Harpocration’s late testimony, and tends to present it as a regular practice. Literary sources and epigraphic documents such as defective lists of bouleutai invite to take a much more balanced position.
La date de la première célébration des Amphiareia-Romaia d’Oropos
Authors: Kalliontzis Yannis
Published: December 2016

Le présent article a pour but de proposer une nouvelle date pour l’association des Romaia à la fête des Amphiareia d’Oropos. Jusqu’à présent cette association a été considérée comme postérieure à 86 av. J.-C. et aux guerres mithridatiques, mais un nouvel examen du premier catalogue des vainqueurs aux Amphiareia-Romaia permet de proposer une date au milieu du iie siècle av. J.-C. La nouvelle date de la première célébration des Amphiareia-Romaia influence l’interprétation de l’utilisation du nom dynastique Antioche du Kydnos par la cité de Tarse en Cilicie et la chronologie de plusieurs inscriptions agonistiques de Béotie et d’autres régions de la Grèce.
FAST SAUSAGE MODES IN MAGNETIC TUBES WITH CONTINUOUS TRANSVERSE PROFILES: EFFECTS OF A FINITE PLASMA BETA
Authors: Chen Shao-Xia , Li Bo , Xiong Ming , Yu Hui , Guo Ming-Zhe
Published: December 2016

While standing fast sausage modes in flare loops are often invoked to interpret quasi-periodic pulsations (QPPs) in solar flares, it is unclear as to how they are influenced by the combined effects of a continuous transverse structuring and a finite internal plasma beta (

). We derive a generic dispersion relation governing linear sausage waves in straight magnetic tubes for which plasma pressure is not negligible, and the density and temperature inhomogeneities of essentially arbitrary form take place in a layer of arbitrary width. Focusing on fast modes, we find that

only weakly influences

, the critical longitudinal wavenumber separating the leaky from trapped modes. Likewise, for both trapped and leaky modes, the periods P in units of the transverse fast time depend only weakly on

, which is compatible with the fact that the effective wave vectors of fast sausage modes are largely perpendicular to the background magnetic field. However, a weak

dependence of the damping times τ is seen only when the length-to-radius ratio L/R is ∼50% larger than some critical value

, which itself rather sensitively depends on the density contrast, profile steepness, as well as on how the transverse structuring is described. In the context of QPPs, we conclude that the much simpler zero-beta theory can be employed for trapped modes, as long as one sees the deduced internal Alfvén speed as actually being the fast speed. In contrast, effects due to a finite beta in flare loops should be considered when leaky modes are exploited.
THE MERGING GALAXY CLUSTER A520—A BROKEN-UP COOL CORE, A DARK SUBCLUSTER, AND AN X-RAY CHANNEL
Authors: H. S. Wang Qian , Markevitch Maxim , Giacintucci Simona
Published: December 2016

We present results from a deep Chandra X-ray observation of a merging galaxy cluster A520. A high-resolution gas temperature map reveals a long trail of dense, cool clumps—apparently the fragments of a cool core that has been stripped from the infalling subcluster by ram pressure. The clumps should still be connected by the stretched magnetic field lines. The observed temperature variations imply that thermal conductivity is suppressed by a factor

across the presumed direction of the magnetic field (as found in other clusters), and is also suppressed along the field lines by a factor of several. Two massive clumps in the periphery of A520, visible in the weak-lensing mass map and the X-ray image, have apparently been completely stripped of gas during the merger, but then re-accreted the surrounding high-entropy gas upon exit from the cluster. The mass clump that hosted the stripped cool core is also reaccreting hotter gas. An X-ray hydrostatic mass estimate for the clump that has the simplest geometry agrees with the lensing mass. Its current gas mass to total mass ratio is very low, 1.5%–3%, which makes it a “dark subcluster.” We also found a curious low X-ray brightness channel (likely a low-density sheet in projection) going across the cluster along the direction of an apparent secondary merger. The channel may be caused by plasma depletion in a region of an amplified magnetic field (with plasma

). The shock in A520 will be studied in a separate paper.
THE SPIRAL WAVE INSTABILITY INDUCED BY A GIANT PLANET. I. PARTICLE STIRRING IN THE INNER REGIONS OF PROTOPLANETARY DISKS
Authors: Bae Jaehan , Nelson Richard P. , Hartmann Lee
Published: December 2016

We have recently shown that spiral density waves propagating in accretion disks can undergo a parametric instability by resonantly coupling with and transferring energy into pairs of inertial waves (or inertial-gravity waves when buoyancy is important). In this paper, we perform inviscid three-dimensional global hydrodynamic simulations to examine the growth and consequence of this instability operating on the spiral waves driven by a Jupiter-mass planet in a protoplanetary disk. We find that the spiral waves are destabilized via the spiral wave instability (SWI), generating hydrodynamic turbulence and sustained radially alternating vertical flows that appear to be associated with long wavelength inertial modes. In the interval

, where R
p denotes the semimajor axis of the planetary orbit (assumed to be 5 au), the estimated vertical diffusion rate associated with the turbulence is characterized by

. For the disk model considered here, the diffusion rate is such that particles with sizes up to several centimeters are vertically mixed within the first pressure scale height. This suggests that the instability of spiral waves launched by a giant planet can significantly disperse solid particles and trace chemical species from the midplane. In planet formation models where the continuous local production of chondrules/pebbles occurs over Myr timescales to provide a feedstock for pebble accretion onto these bodies, this stirring of solid particles may add a time constraint: planetary embryos and large asteroids have to form before a gas giant forms in the outer disk, otherwise the SWI will significantly decrease the chondrule/pebble accretion efficiency.
A SPECTROSCOPIC SEARCH FOR CHEMICALLY STRATIFIED WHITE DWARFS IN THE SLOAN DIGITAL SKY SURVEY
Authors: Manseau P. M. , Bergeron P. , Green E. M.
Published: December 2016

We present a detailed search and analysis of chemically stratified hybrid (traces of helium and hydrogen) white dwarfs in the Sloan Digital Sky Survey (SDSS). Only one stratified white dwarf, PG 1305–017, was known prior to this analysis. The main objective is to confirm the existence of several new stratified objects. We first describe our new generation of stratified model atmospheres, where a thin hydrogen layer floats in diffusive equilibrium on top of a more massive helium layer. We then present the results of our search for hot (

T

eff

 > 30,000 K) white dwarfs with a hybrid spectral type among the ∼38,000 white dwarf spectra listed in the SDSS. A total of 51 spectra were retained in our final sample, which we analyze using spectroscopic fits to both chemically homogeneous and stratified model atmospheres. We identify 14 new stratified white dwarfs in the SDSS sample. From these results, we draw several conclusions regarding the physical processes that might explain the presence of helium in the atmospheres of all the stars in our sample.
THE POSSIBLE DETECTION OF A BINARY COMPANION TO A TYPE IBN SUPERNOVA PROGENITOR
Authors: Maund J. R. , Pastorello A. , Mattila S. , Itagaki K. , Boles T.
Published: December 2016

We present late-time observations of the site of the Type Ibn supernova (SN) 2006jc, acquired with the Hubble Space Telescope Advanced Camera for Surveys. A faint blue source is recovered at the SN position, with brightness

,

and

mag, although there is no detection in a contemporaneous narrow-band

image. The spectral energy distribution of the late-time source is well-fit by a stellar-like spectrum (

and

), subject to only a small degree of reddening—consistent with that estimated for SN 2006jc itself at early-times. The lack of further outbursts after the explosion of SN 2006jc suggests that the precursor outburst originated from the progenitor. The possibility of the source being a compact host cluster is ruled out on the basis of the source’s faintness; however, the possibility that the late-time source may be an unresolved light echo originating in a shell or sphere of pre-SN dust (within a radius

) is also discussed. Irrespective of the nature of the late-time source, these observations rule out a luminous blue variable as a companion to the progenitor of SN 2006jc.
NUMERICAL AND ANALYTICAL SOLUTIONS OF NEUTRINO-DOMINATED ACCRETION FLOWS WITH A NON-ZERO TORQUE BOUNDARY CONDITION AND ITS APPLICATIONS IN GAMMA-RAY BURSTS
Authors: Xie Wei , Lei Wei-Hua , Wang Ding-Xiong
Published: December 2016

A stellar-mass black hole (BH) surrounded by a neutrino-dominated accretion flow (NDAF) has been discussed in a number of works as the central engine of gamma-ray bursts (GRBs). It is widely believed that NDAF cannot liberate enough energy for bright GRBs. However, these works have been based on the assumption of a “no torque” boundary condition, which is invalid when the disk is magnetized. In this paper, we present both numerical and analytical solutions for NDAFs with non-zero boundary stresses and reexamine their properties. We find that an NDAF with such a boundary torque can be powerful enough to account for those bright short GRBs, energetic long GRBs, and ultra-long GRBs. The disk becomes viscously unstable, which makes it possible to interpret the variability of GRB prompt emission and the steep decay phase in the early X-ray afterglow. Finally, we study the gravitational waves radiated from a processing BH-NDAF. We find that the effects of the boundary torque on the strength of the gravitational waves can be ignored.
DAMPING OF ALFVÉN WAVES BY TURBULENCE AND ITS CONSEQUENCES: FROM COSMIC-RAY STREAMING TO LAUNCHING WINDS
Authors: Lazarian A.
Published: December 2016

This paper considers turbulent damping of Alfvén waves in magnetized plasmas. We identify two cases of damping, one related to damping of cosmic-ray streaming instability, the other related to damping of Alfvén waves emitted by a macroscopic wave source, e.g., a stellar atmosphere. The physical difference between the two cases is that in the former case the generated waves are emitted with respect to the local direction of the magnetic field, and in the latter, waves are emitted with respect to the mean field. The scaling of damping is different in the two cases. We explore effects of turbulence in the regimes from sub-Alfvénic to super-Alfvénic to obtain analytical expressions for the damping rates and define the ranges of applicability of these expressions. In describing the damping of the streaming instability, we find that for sub-Alfvénic turbulence, the range of cosmic-ray energies influenced by weak turbulence is unproportionally large compared to the range of scales where weak turbulence is present. On the contrary, the range of cosmic-ray energies affected by strong Alfvénic turbulence is rather limited. A number of astrophysical applications of the process ranging from launching of stellar and galactic winds to propagation of cosmic rays in galaxies and clusters of galaxies is considered. In particular, we discuss how to reconcile the process of turbulent damping with the observed isotropy of the Milky Way cosmic rays.
THE MEASUREMENT, TREATMENT, AND IMPACT OF SPECTRAL COVARIANCE AND BAYESIAN PRIORS IN INTEGRAL-FIELD SPECTROSCOPY OF EXOPLANETS
Authors: Greco Johnny P. , Brandt Timothy D.
Published: December 2016

The recovery of an exoplanet’s atmospheric parameters from its spectrum requires accurate knowledge of the spectral errors and covariances. Unfortunately, the complex image processing used in high-contrast integral-field spectrograph (IFS) observations generally produces spectral covariances that are poorly understood and often ignored. In this work, we show how to measure the spectral errors and covariances and include them self-consistently in parameter retrievals. By combining model exoplanet spectra with a realistic noise model generated from the Gemini Planet Imager (GPI) early science data, we show that ignoring spectral covariance in high-contrast IFS data can both bias inferred parameters and lead to unreliable confidence regions on those parameters. This problem is made worse by the common practice of scaling the χ
2 per degree of freedom to unity; the input parameters then fall outside the 95% confidence regions in as many as ∼80% of noise realizations. The biases we observe can approach the typical levels of precision achieved in high-contrast spectroscopy. Accounting for realistic priors in fully Bayesian retrievals can also have a significant impact on the inferred parameters. Plausible priors on effective temperature and surface gravity can vary by an order of magnitude across the confidence regions appropriate for objects with weak age constraints; priors for objects with good age constraints are dominated by modeling uncertainties. Our methods are directly applicable to existing high-contrast IFSs including GPI and SPHERE, as well as upcoming instruments like CHARIS and, ultimately, WFIRST-AFTA.
MAPPING THE MOST MASSIVE OVERDENSITY THROUGH HYDROGEN (MAMMOTH). I. METHODOLOGY
Authors: Cai Zheng , Fan Xiaohui , Peirani Sebastien , Bian Fuyan , Frye Brenda , McGreer Ian , Prochaska J. Xavier , Lau Marie Wingyee , Tejos Nicolas , Ho Shirley , Schneider Donald P.
Published: December 2016

Modern cosmology predicts that a galaxy overdensity (e.g., protocluster) will be associated with a large intergalactic medium gas reservoir, which can be traced by Lyα forest absorption. We have undertaken a systematic study of the relation between Coherently Strong intergalactic Lyα Absorption systems (CoSLAs), which have the highest optical depth (τ) in the τ distribution, and mass overdensities on the scales of ∼10–20 h
−1 comoving Mpc. On such large scales, our cosmological simulations show a strong correlation between the effective optical depth (τ
eff) of the CoSLAs and the three-dimensional mass overdensity. In spectra with moderate signal-to-noise ratio, however, the profiles of CoSLAs can be confused with individual high column density absorbers. For z > 2.6, where the corresponding Lyβ is redshifted to the optical, we have developed a selection technique to distinguish between these two alternatives. We have applied this technique to ∼6000 sight lines provided by Sloan Digital Sky Survey III quasar survey at z = 2.6–3.3 with a continuum-to-noise ratio greater than 8, and we present a sample of five CoSLA candidates with τ
eff on 15 h
−1 Mpc greater than 4.5× the mean optical depth. At lower redshifts of z < 2.6, where the background quasar density is higher, the overdensity can be traced by intergalactic absorption groups using multiple sight lines with small angular separations. Our overdensity searches fully use the current and next generation of Lyα forest surveys, which cover a survey volume of >1 (h
−1 Gpc)3. Systems traced by CoSLAs will yield a uniform sample of the most massive overdensities at z > 2 to provide stringent constraints to models of structure formation.
NLTE ANALYSIS OF HIGH-RESOLUTION H-BAND SPECTRA. I. NEUTRAL SILICON*
Authors: Zhang Junbo , Shi Jianrong , Pan Kaike , Prieto Carlos Allende , Liu Chao
Published: December 2016

We investigated the reliability of our silicon atomic model and the influence of non-local thermodynamical equilibrium (NLTE) on the formation of neutral silicon (Si i) lines in the near-infrared (near-IR) H-band. We derived the differential Si abundances for 13 sample stars with high-resolution H-band spectra from the Apache Point Observatory Galactic Evolution Experiment (APOGEE), as well as from optical spectra, both under local thermodynamical equilibrium (LTE) and NLTE conditions. We found that the differences between the Si abundances derived from the H-band and from optical lines for the same stars are less than 0.1 dex when the NLTE effects are included, and that NLTE reduces the line-to-line scatter in the H-band spectra for most sample stars. These results suggest that our Si atomic model is appropriate for studying the formation of H-band Si lines. Our calculations show that the NLTE corrections of the Si i
H-band lines are negative, i.e., the final Si abundances will be overestimated in LTE. The corrections for strong lines depend on surface gravity, and tend to be larger for giants, reaching ∼−0.2 dex in our sample, and up to ∼−0.4 dex in extreme cases of APOGEE targets. Thus, the NLTE effects should be included in deriving silicon abundances from H-band Si i lines, especially for the cases where only strong lines are available.
PSR J1301+0833: A KINEMATIC STUDY OF A BLACK-WIDOW PULSAR
Authors: Romani Roger W. , Graham Melissa L. , Filippenko Alexei V. , Zheng WeiKang
Published: December 2016

We have obtained spectroscopic measurements of the P

s
= 1.8 ms, P

B
= 6.5 hr black-widow (BW) pulsar PSR J1301+0833 as part of a program to investigate optical companions of wind-shrouded pulsars. The derived radial-velocity amplitude (

) and inclination (

) imply a neutron star mass

, smaller (for similar fit assumptions) than that of the well-studied original BW pulsar PSR J1959+2048, which shares similar values of P

s
and P

B
. This fit, which assumes

, indicates a small heated region on the (anomalously faint) companion. With a free distance and full surface heating the best fit is statistically acceptable, but the large inferred

is inconsistent with the observed pulsar proper motion. Improved photometry and heating models will be needed to refine these measurements.
HIGH-ENERGY NON-THERMAL AND THERMAL EMISSION FROM GRB 141207A DETECTED BY FERMI
Authors: Arimoto Makoto , Asano Katsuaki , Ohno Masanori , Veres Péter , Axelsson Magnus , Bissaldi Elisabetta , Tachibana Yutaro , Kawai Nobuyuki
Published: December 2016

A bright long gamma-ray burst GRB 141207A was observed by the Fermi Gamma-ray Space Telescope and detected by both instruments onboard. The observations show that the spectrum in the prompt phase is not well described by the canonical empirical Band function alone, and that an additional power-law component is needed. In the early phase of the prompt emission, a modified blackbody with a hard low-energy photon index (α = +0.2 to +0.4) is detected, which suggests a photospheric origin. In a finely time-resolved analysis, the spectra are also well fitted by the modified blackbody combined with a power-law function. We discuss the physical parameters of the photosphere such as the bulk Lorentz factor of the relativistic flow and the radius. We also discuss the physical origin of the extra power-law component observed during the prompt phase in the context of different models such as leptonic and hadronic scenarios in the internal shock regime and synchrotron emission in the external forward shock. In the afterglow phase, the temporal and spectral behaviors of the temporally extended high-energy emission and the fading X-ray emission detected by the X-Ray Telescope on-board Swift are consistent with synchrotron emission in a radiative external forward shock.
QUIESCENT PROMINENCES IN THE ERA OF ALMA: SIMULATED OBSERVATIONS USING THE 3D WHOLE-PROMINENCE FINE STRUCTURE MODEL
Authors: Gunár Stanislav , Heinzel Petr , Mackay Duncan H. , Anzer Ulrich
Published: December 2016

We use the detailed 3D whole-prominence fine structure model to produce the first simulated high-resolution ALMA observations of a modeled quiescent solar prominence. The maps of synthetic brightness temperature and optical thickness shown in the present paper are produced using a visualization method for synthesis of the submillimeter/millimeter radio continua. We have obtained the simulated observations of both the prominence at the limb and the filament on the disk at wavelengths covering a broad range that encompasses the full potential of ALMA. We demonstrate here extent to which the small-scale and large-scale prominence and filament structures will be visible in the ALMA observations spanning both the optically thin and thick regimes. We analyze the relationship between the brightness and kinetic temperature of the prominence plasma. We also illustrate the opportunities ALMA will provide for studying the thermal structure of the prominence plasma from the cores of the cool prominence fine structure to the prominence–corona transition region. In addition, we show that detailed 3D modeling of entire prominences with their numerous fine structures will be important for the correct interpretation of future ALMA observations of prominences.
DISCOVERY OF A REDBACK MILLISECOND PULSAR CANDIDATE: 3FGL J0212.1+5320
Authors: Li Kwan-Lok , Kong Albert K. H. , Hou Xian , Mao Jirong , Strader Jay , Chomiuk Laura , Tremou Evangelia
Published: December 2016

We present a multiwavelength study of the unidentified Fermi object, 3FGL J0212.1+5320. Within the 95% error ellipse, Chandra detects a bright X-ray source (i.e.,

erg cm−2 s−1) that has a low-mass optical counterpart (

and

K). A clear ellipsoidal modulation is shown in optical/infrared at 20.87 hr. The gamma-ray properties of 3FGL J0212.1+5320 are all consistent with that of a millisecond pulsar (MSP), suggesting that it is a γ-ray redback (RB) MSP binary with a low-mass companion filling ⪆64% of the Roche lobe. If confirmed, it will be an RB binary with one of the longest orbital periods known. Spectroscopic data taken in 2015 from the Lijiang observatory show no evidence of strong emission lines, revealing that the accretion is currently inactive (the rotation-powered pulsar state). This is consistent with the low X-ray luminosities (

erg s−1) and the possible X-ray modulation seen by Chandra and Swift. Considering that the X-ray luminosity and the high X-ray-to-γ-ray flux ratio (8%) are both comparable to those of the two known γ-ray transitional MSPs, we suspect that 3FGL J0212.1+5320 could be a potential target to search for future transition to the accretion active state.
THE EXOPLANET MASS-RATIO FUNCTION FROM THE MOA-II SURVEY: DISCOVERY OF A BREAK AND LIKELY PEAK AT A NEPTUNE MASS
Authors: Suzuki D. , Bennett D. P. , Sumi T. , Bond I. A. , Rogers L. A. , Abe F. , Asakura Y. , Bhattacharya A. , Donachie M. , Freeman M. , Fukui A. , Hirao Y. , Itow Y. , Koshimoto N. , Li M. C. A. , Ling C. H. , Masuda K. , Matsubara Y. , Muraki Y. , Nagakane M. , Onishi K. , Oyokawa H. , Rattenbury N. , Saito To. , Sharan A. , Shibai H. , Sullivan D. J. , Tristram P. J. , Yonehara A. ,   (the MOA collaboration)
Published: December 2016

We report the results of the statistical analysis of planetary signals discovered in MOA-II microlensing survey alert system events from 2007 to 2012. We determine the survey sensitivity as a function of planet–star mass ratio, q, and projected planet–star separation, s, in Einstein radius units. We find that the mass-ratio function is not a single power law, but has a change in slope at q ∼ 10−4, corresponding to ∼20 M
⊕ for the median host-star mass of ∼0.6

. We find significant planetary signals in 23 of the 1474 alert events that are well-characterized by the MOA-II survey data alone. Data from other groups are used only to characterize planetary signals that have been identified in the MOA data alone. The distribution of mass ratios and separations of the planets found in our sample are well fit by a broken power-law model of the form

for q > q
br and

for q < q
br, where q
br is the mass ratio of the break. We also combine this analysis with the previous analyses of Gould et al. and Cassan et al., bringing the total sample to 30 planets. This combined analysis yields

, n = −0.93 ± 0.13,

, and

for q
br ≡ 1.7 × 10−4. The unbroken power-law model is disfavored with a p-value of 0.0022, which corresponds to a Bayes factor of 27 favoring the broken power-law model. These results imply that cold Neptunes are likely to be the most common type of planets beyond the snow line.
SPECTROSCOPY FROM THE HUBBLE SPACE TELESCOPE COSMIC ORIGINS SPECTROGRAPH OF THE SOUTHERN NOVA-LIKE BB DORADUS IN AN INTERMEDIATE STATE
Authors: Godon Patrick , Sion Edward M. , Gänsicke Boris T. , Hubeny Ivan , de Martino Domitilla , Pala Anna F. , Rodríguez-Gil Pablo , Szkody Paula , Toloza Odette
Published: December 2016

We present a spectral analysis of the spectrum from the Hubble Space Telescope Cosmic Origins Spectrograph (HST/COS) of the southern VY Scl nova-like variable BB Doradus, obtained as part of a Cycle 20 HST/COS survey of accreting white dwarfs (WDs) in cataclysmic variables. BB Dor was observed with COS during an intermediate state with a low mass accretion rate, thereby allowing an estimate of the WD temperature. The results of our spectral analysis show that the WD is a significant far-ultraviolet (FUV) component of the spectrum with a temperature of about 35,000–50,000 K, assuming a WD mass of

(

). The disk, with a mass accretion rate of

, contributes about 1/5 to 1/2 of the FUV flux.
ZOMBIE VORTEX INSTABILITY. II. THRESHOLDS TO TRIGGER INSTABILITY AND THE PROPERTIES OF ZOMBIE TURBULENCE IN THE DEAD ZONES OF PROTOPLANETARY DISKS
Authors: Marcus Philip S. , Pei Suyang , Jiang Chung-Hsiang , Barranco Joseph A.
Published: December 2016

In Zombie Vortex Instability (ZVI), perturbations excite critical layers in stratified, rotating shear flow (as in protoplanetary disks (PPDs)), causing them to generate vortex layers, which roll up into anticyclonic zombie vortices and cyclonic vortex sheets. The process is self-sustaining as zombie vortices perturb new critical layers, spawning a next generation of zombie vortices. Here, we focus on two issues: the minimum threshold of perturbations that trigger self-sustaining vortex generation, and the properties of the late-time zombie turbulence on large and small scales. The critical parameter that determines whether ZVI is triggered is the magnitude of the vorticity on the small scales (and not velocity); the minimum Rossby number needed for instability is

for

, where N is the Brunt–Väisälä frequency. While the threshold is set by vorticity, it is useful to infer a criterion on the Mach number; for Kolmogorov noise, the critical Mach number scales with Reynolds number:

. In PPDs, this is

. On large scales, zombie turbulence is characterized by anticyclones and cyclonic sheets with typical Rossby number ∼0.3. The spacing of the cyclonic sheets and anticyclones appears to have a “memory” of the spacing of the critical layers. On small scales, zombie turbulence has no memory of the initial conditions and has a Kolmogorov-like energy spectrum. While our earlier work was in the limit of uniform stratification, we have demonstrated that ZVI works for non-uniform Brunt–Väisälä frequency profiles that may be found in PPDs.
LIFETIME OF A COSMIC-RAY SPOT
Authors: Globus Noemie , Eichler David
Published: December 2016

We investigate the existence, angular sizes, and durations of ultrahigh-energy cosmic-ray (UHECR) hotspots as observed at Earth after the UHECRs propagate through the Galactic magnetic field. We show that, during a period of observation of typically 5 years, cosmic-ray hotspots with rigidities

∼

10

19

V from sources whose propagation distances are smaller than 10 kpc are steady, while those much further may change position in the observer’s sky due to motion of the Earth. (Note that the propagation distance—the total length of the trajectory connecting source to Earth—is always greater than the distance to the source.) However, this effect can be observed only if the spread in rigidity of the UHECRs is small enough; we show that for an energy bin width of 10%, typical of CR observatories, the effect of Earth motion over 5 years would be undetectable.
ROLE OF THE CORONAL ALFVÉN SPEED IN MODULATING THE SOLAR-WIND HELIUM ABUNDANCE
Authors: Wang Y.-M.
Published: December 2016

The helium abundance He/H in the solar wind is relatively constant at ∼0.04 in high-speed streams, but varies in phase with the sunspot number in slow wind, from ∼0.01 at solar minimum to ∼0.04 at maximum. Suggested mechanisms for helium fractionation have included frictional coupling to protons and resonant interactions with high-frequency Alfvénic fluctuations. We compare He/H measurements during 1995–2015 with coronal parameters derived from source-surface extrapolations of photospheric field maps. We find that the near-Earth helium abundance is an increasing function of the magnetic field strength and Alfvén speed v
A in the outer corona, while being only weakly correlated with the proton flux density. Throughout the solar cycle, fast wind is associated with short-term increases in v
A near the source surface; resonance with Alfvén waves, with v
A and the relative speed of α-particles and protons decreasing with increasing heliocentric distance, may then lead to enhanced He/H at 1 au. The modulation of helium in slow wind reflects the tendency for the associated coronal Alfvén speeds to rise steeply from sunspot minimum, when this wind is concentrated around the source-surface neutral line, to sunspot maximum, when the source-surface field attains its peak strengths. The helium abundance near the source surface may represent a balance between collisional decoupling from protons and Alfvén wave acceleration.
Le lieu d’ enterrement de Priscillien
Authors: Piay Augusto Diego
Published: December 2016

Depuis que Louis Duchesne avança l’idée que les restes de Priscillien pourraient reposer dans le sépulcre de l’apôtre Jacques, plusieurs spécialistes ont proposé de nombreux lieux qui auraient pu accueillir cette dépouille. Mais les solutions proposées au fil du temps manquaient de rigueur scientifique et, à plusieurs reprises, un site énigmatique daté du iv e  siècle ou la présence d’un sépulcre datant de cette période ont été considérés comme des arguments suffisants pour voir dans ces endroits le lieu d’enterrement de Priscillien. Cependant, jusque-là, le problème n’a pas été abordé avec objectivité et les faibles références documentaires ainsi que le silence de l’archéologie ont semblé constituer d’insurmontables obstacles...
S'exprimer et se faire comprendre
Authors: Écotière Marie-Anne , Poujol Anne-Laure , Scelles Régine
Published: December 2016

La technique d’analyse des entretiens de recherche, menés auprès de personnes qui ont une déficience intellectuelle, pose inévitablement la question de la prise en compte des signes de la déficience dans l’analyse et l’interprétation des entretiens. Cette question est ici travaillée à partir des entretiens de recherche menés avec Jean, adulte rencontré dans un établissement et service d’aide par le travail ( esat ), et avec Jimmy, adolescent rencontré en institut médico-professionnel ( impro ). Les éléments principaux à prendre en compte sont : l’implication importante du chercheur à travers ses interventions et sa subjectivité ; la rythmicité du discours ; les temps d’accordage et de désaccordage ; la connaissance préalable de l’interviewé comme repère dans l’analyse littérale ; l’appui sur des outils tels que l’analyse thématique ou la mise en figuration du récit pour sortir d’un vécu d’impuissance du chercheur par rapport à une pauvreté apparente du contenu des entretiens.
Rêve et fantasme
Authors: Lacombe Alain
Published: December 2016

Résumé Quel est le rapport entre le rêve et le fantasme et en quoi se différencient-ils dans leur lien au réel ?
El Modelo de Gestión del Conocimiento Motivacional: propuesta de aplicación en el sector bibliotecario
Authors: López-Fernández Daniel , Alarcón Pedro P. , Tovar Edmundo , Alonso Santiago
Published: December 2016

En los entornos laborales, cuidar elementos como los estilos de supervisión, las relaciones interpersonales o la satisfacción por el trabajo incide positivamente en la motivación del trabajador, y consecuentemente, en su rendimiento y bienestar. Para lograrlo se pueden aplicar modelos de gestión de conocimiento como el que se presenta en este artículo, el cual genera de manera científica y sistemática diagnósticos motivacionales y recomendaciones de mejora de especial utilidad para managers y departamentos de recursos humanos. El modelo propuesto permite su particularización a diferentes colectivos profesionales, incluidos los relacionados con servicios bibliotecarios y de documentación. La adecuación, fiabilidad y utilidad del modelo propuesto se ha comprobado empíricamente mediante varios casos de estudio conducidos con 92 estudiantes y 166 profesionales. Los resultados favorables que se han cosechado permiten concluir que el modelo es eficaz y útil para evaluar y mejorar la motivación.
¿Publicar o perecer? El caso de las Ciencias Sociales y las Humanidades en Latinoamérica
Authors: Aguado-López Eduardo , Becerril-García Arianna
Published: December 2016

Se busca conocer el comportamiento de las Ciencias Sociales y Humanidades en Latinoamérica respecto a la colaboración científica; se contrastan para ello las tendencias que registra Scopus (2003-2013) a través del análisis de Plume y Van Weijen (2014), y redalyc.org (2005-2014), con un universo de estudio de 220.200 artículos científicos. Se tiene que la cantidad de formas de autor se incrementó a un mayor ritmo que la cantidad de artículos publicados, donde los que inducen el comportamiento al alza son aquellos vinculados a estrategias de trabajo colaborativo y se tiende a una colaboración hacia el exterior. Estudiar las características de la producción científica actual orilla a analizar la colaboración como una de las propiedades que conforman el quehacer científico, dado que es una de las formas en que los científicos latinoamericanos hacen frente al principio “publicar o perecer”, con el cual operan los sistemas de evaluación al desempeño científico.
Un panorama académico de dos caras: retrato de los documentos altamente citados en Google Scholar (1950-2013)
Authors: Martín-Martín Alberto , Orduna-Malea Enrique , Ayllón Juan M. , Delgado López-Cózar Emilio
Published: December 2016

El principal objetivo de este trabajo es identificar el conjunto de documentos altamente citados en Google Scholar y definir sus características nucleares (tipología documental, idioma, disponibilidad en abierto, fuentes y número de versiones), bajo la hipótesis de que la amplia cobertura del buscador podría proporcionar un retrato diferente de este conjunto documental a la ofrecida por las bases de datos tradicionales. Para ello, se ha realizado una consulta por año (desde 1950 hasta 2013) identificando los 1000 documentos más citados y obteniendo una muestra final de 64.000 registros (el 40% de los cuales proporcionaban un enlace al texto completo). Los resultados muestran que el documento altamente citado “promedio” es un artículo de revista o libro (éstos constituyen el 62% del top 1% de los documentos más citados de la muestra), escrito en inglés (92.5%) y disponible online en PDF (86% de la muestra). Aun así, se debe indicar la existencia de errores especialmente en la detección de documentos duplicados y en la correcta vinculación de citas. En todo caso, la muestra manejada (documentos altamente citados) minimiza los efectos de dichas limitaciones. Dada la alta presencia de libros (manuales) y, en menor medida, de otras tipologías documentales (como congresos o informes), se concluye que Google Scholar ofrece una visión original y diferente del conjunto de documentos académicos más influyentes (medidos desde la perspectiva de la contabilización de citas), conformado no sólo por material estrictamente científico (artículos en revistas), sino académico en sentido amplio.
L’art, la littérature et le vivant
Authors: Dahan-Gaida Laurence
Published: December 2016

Cet article explore les liens qui, depuis l’Antiquité, lient les savoirs du vivant à l’esthétique, entendue à la fois comme science du beau, comme science des formes et comme théorie de la réception des œuvres d’art. Sans prétendre à l’exhaustivité ou à la continuité historique, il braque le projecteur sur des penseurs – scientifiques, poètes ou artistes - qui ont marqué l’histoire des relations entre les deux domaines : Goethe, Darwin, Köhler, Valéry, René Thom, Botho Strauss…
De la biologie à l’écologie
Authors: Séginger Gisèle
Published: December 2016

Les textes sur la nature des années 1850-1860 ont parfois accrédité la thèse d’un Michelet spiritualiste et d’une écologie-religion. Or, on peut se demander au contraire si Michelet ne projette pas de révolutionner les structures de l’imaginaire pour dépasser la question religieuse et créer un nouveau légendaire, écologique, laïque et républicain, fondé sur des savoirs du vivant.
Hérédité et atavisme criminel dans les romans d’Hector Malot
Authors: Kiriow Ivan
Published: December 2016

Cet article étudie l’investissement littéraire du thème de l’hérédité dans plusieurs romans d’Hector Malot, en particulier sa représentation de la figure du criminel héréditaire ou « atavique », inspirée de la théorie du criminel-né développée par Cesare Lombroso. Nous verrons aussi comment la réception critique du roman Conscience (1888) et le dialogue entre les disciplines (critique littéraire, philosophie et théories biologiques de l’hérédité) a enrichi et transformé l’approche de cette thématique chez le romancier.
Clr-a: A Novel Immune-Related C-Type Lectin-like Molecule Exclusively Expressed by Mouse Gut Epithelium
Authors: Rutkowski Emilia , Leibelt Stefan , Born Christina , Friede Miriam E. , Bauer Stefan , Weil Sandra , Koch Joachim , Steinle Alexander
Published: December 2016

The mouse gut epithelium represents a constitutively challenged environment keeping intestinal commensal microbiota at bay and defending against invading enteric pathogens. The complex immunoregulatory network of the epithelial barrier surveillance also involves NK gene complex (NKC)–encoded C-type lectin-like molecules such as NKG2D and Nkrp1 receptors. To our knowledge, in this study, we report the first characterization of the orphan C-type lectin-like molecule Clr-a encoded by the Clec2e gene in the mouse NKC. Screening of a panel of mouse tissues revealed that Clec2e transcripts are restricted to the gastrointestinal tract. Using Clr-a–specific mAb, we characterize Clr-a as a disulfide-linked homodimeric cell surface glycoprotein. Of note, a substantial fraction of Clr-a molecules are retained intracellularly, and analyses of Clr-a/Clr-f hybrids attribute intracellular retention to both the stalk region and parts of the cytoplasmic domain. Combining quantitative PCR analyses with immunofluorescence studies revealed exclusive expression of Clr-a by intestinal epithelial cells and crypt cells throughout the gut. Challenge with polyinosinic-polycytidylic acid results in a rapid and strong downregulation of intestinal Clr-a expression in contrast to the upregulation of Clr-f, a close relative of Clr-a, that also is specifically expressed by the intestinal epithelium and acts as a ligand of the inhibitory Nkrp1g receptor. Collectively, we characterize expression of the mouse NKC-encoded glycoprotein Clr-a as strictly associated with mouse intestinal epithelium. Downregulation upon polyinosinic-polycytidylic acid challenge and expression by crypt cells clearly distinguish Clr-a from the likewise intestinal epithelium-restricted Clr-f, pointing to a nonredundant function of these highly related C-type lectin-like molecules in the context of intestinal immunosurveillance.
Stratigraphy of the Lower Proterozoic (Aphebian), Great Slave Supergroup, East Arm of Great Slave Lake, District of Mackenzie
Authors: Hoffman P F
Published: December 2016

The Aphebian-age Great Slave Supergroup (formerly the Great Slave Group) is divided into four groups. The Sosan Group (formerly the Sosan Formation), composed predominantly of non-marine sandstones, is divided into four formations that are defined in this report.
The Kahochella Group (formerly the Kahochella Formation), composed predominantly of marine shales, is divided into four formations that are also defined in this report. The Pethei Group (formerly the Pethei Formation) is composed of two lithologically distinct sequences. On the north side of the
East Arm synclinorium, where littoral marine limestones and dolomites predominate, the group is divided into five formations defined in this report, whereas on the south side of the synclinorium , where deep water marine shales, greywackes and limestones predominate , the group is divided into four
formations, only the oldest of which occurs to the north. The Christie Bay Group, composed predominantly of non -marine and marine red beds, is divided into the Stark Formation, Tochatwi Formation and Pearson Formation of earlier reports, and one additional formation defined in this report. The
thickness, distribution, lithology, contact relations and origin of each formation is discussed briefly and a type section established. The Union Island Group, also of Aphebian age, underlies the Great Slave Supergroup unconformably. Quartz diorite laccoliths, the age relations of which were
formerly in dispute, intrude the lower Stark Formation and all older rocks.