bluuebunny/crossref_metadata_2025_split huggingface dataset:
Effects of the single supplementation and multiple doses of Passiflora incarnata L. on human anxiety: A Clinical Trial, Double-blind, Placebo-controlled, Randomized
Authors: Avelino da Silva Janilson , De Carvalho da Costa Maria José , Rodrigues da Alves Maria da Conceição , Fernandes da Braga João Euclides , Bezerra Luna da Lima Caliandra Maria , De Morais da Pordeus Liana Clébia 
Published: January 2017

Object: This study aimed to investigate the effects of Passiflora incarnata L. on anxiety in humans.
Method: The individuals were randomly assigned to one of the following groups: Placebo or experimental, n =30, single dose, as well as Placebo or Experimental, n =15, multiple dose. The experimental human anxiety was induced by simulated public speaking test in the following phases: Basal (B), stressful (A), speech 1 (S1), speech 2 (S2) and Final (F). We evaluated the Systolic Blood Pressure (SBP), and Diastolic (DBP), Heart Rate (HR), Electrical Conductance of Skin and extremities temperature (ET) and filled The state-trait anxiety inventory (STAI S e T).
Results: During the single dose, the HR was reduced at the end of the speech (86±2,0 to 74±3,0 bpm) the experimental group compared to the placebo group (p<0,05); the STAI-S did not change. In the delineation of multiple doses, SBP was reduced, in mmHg, in the experimental group compared to the placebo group during all phases. Experimental: 106±1,0 (B), 111±1,0 (A), 121±2,0 (S1), 115±3 (S2), 104±2,0 (F) e Placebo: 121±3,0; 127±3,0; 130±3,0; 130±4,5; 117±3,0 (p<0,05).
Conclusions: It is suggested that supplementation using Passiflora incarnata L. Capsules (500 mg) decreased cardiovascular signals both in single and in multiple doses, associated with the stress of public speaking.
Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C
Authors: Margutti Raffaella , Kamble A. , Milisavljevic D. , Zapartas E. , de Mink S. E. , Drout M. , Chornock R. , Risaliti G. , Zauderer B. A. , Bietenholz M. , Cantiello M. , Chakraborti S. , Chomiuk L. , Fong W. , Grefenstette B. , Guidorzi C. , Kirshner R. , Parrent J. T. , Patnaude D. , Soderberg A. M. , Gehrels N. C. , Harrison F. 
Published: January 2017

Abstract
We present multi-wavelength observations of SN 2014C during the first 500 days. These observations represent the first solid detection of a young extragalactic stripped-envelope SN out to high-energy X-rays ∼40 keV. SN 2014C shows ordinary explosion parameters (E
k ∼ 1.8 × 1051 erg and M
ej ∼ 1.7 M
⊙). However, over an ∼1 year timescale, SN 2014C evolved from an ordinary hydrogen-poor supernova into a strongly interacting, hydrogen-rich supernova, violating the traditional classification scheme of type-I versus type-II SNe. Signatures of the SN shock interaction with a dense medium are observed across the spectrum, from radio to hard X-rays, and revealed the presence of a massive shell of ∼1 M
⊙ of hydrogen-rich material at ∼6 × 1016 cm. The shell was ejected by the progenitor star in the decades to centuries before collapse. This result challenges current theories of massive star evolution, as it requires a physical mechanism responsible for the ejection of the deepest hydrogen layer of H-poor SN progenitors synchronized with the onset of stellar collapse. Theoretical investigations point at binary interactions and/or instabilities during the last nuclear burning stages as potential triggers of the highly time-dependent mass loss. We constrain these scenarios utilizing the sample of 183 SNe Ib/c with public radio observations. Our analysis identifies SN 2014C-like signatures in ∼10% of SNe. This fraction is reasonably consistent with the expectation from the theory of recent envelope ejection due to binary evolution if the ejected material can survive in the close environment for 103–104 years. Alternatively, nuclear burning instabilities extending to core C-burning might play a critical role.
Preconditioning of Interplanetary Space Due to Transient CME Disturbances
Authors: Temmer M. , Reiss M. A. , Nikolic L. , Hofmeister S. J. , Veronig A. M. 
Published: January 2017

Abstract
Interplanetary space is characteristically structured mainly by high-speed solar wind streams emanating from coronal holes and transient disturbances such as coronal mass ejections (CMEs). While high-speed solar wind streams pose a continuous outflow, CMEs abruptly disrupt the rather steady structure, causing large deviations from the quiet solar wind conditions. For the first time, we give a quantification of the duration of disturbed conditions (preconditioning) for interplanetary space caused by CMEs. To this aim, we investigate the plasma speed component of the solar wind and the impact of in situ detected interplanetary CMEs (ICMEs), compared to different background solar wind models (ESWF, WSA, persistence model) for the time range 2011–2015. We quantify in terms of standard error measures the deviations between modeled background solar wind speed and observed solar wind speed. Using the mean absolute error, we obtain an average deviation for quiet solar activity within a range of 75.1–83.1 km s−1. Compared to this baseline level, periods within the ICME interval showed an increase of 18%–32% above the expected background, and the period of two days after the ICME displayed an increase of 9%–24%. We obtain a total duration of enhanced deviations over about three and up to six days after the ICME start, which is much longer than the average duration of an ICME disturbance itself (∼1.3 days), concluding that interplanetary space needs ∼2–5 days to recover from the impact of ICMEs. The obtained results have strong implications for studying CME propagation behavior and also for space weather forecasting.
Triggered O Star Formation in M20 via Cloud–Cloud Collision: Comparisons between High-resolution CO Observations and Simulations
Authors: Torii K. , Hattori Y. , Hasegawa K. , Ohama A. , Haworth T. J. , Shima K. , Habe A. , Tachihara K. , Mizuno N. , Onishi T. , Mizuno A. , Fukui Y. 
Published: January 2017

Abstract
Understanding high-mass star formation is one of the top-priority issues in astrophysics. Recent observational studies have revealed that cloud–cloud collisions may play a role in high-mass star formation in several places in the Milky Way and the Large Magellanic Cloud. The Trifid Nebula M20 is a well-known Galactic H ii region ionized by a single O7.5 star. In 2011, based on the CO observations with NANTEN2, we reported that the O star was formed by the collision between two molecular clouds ∼0.3 Myr ago. Those observations identified two molecular clouds toward M20, traveling at a relative velocity of

. This velocity separation implies that the clouds cannot be gravitationally bound to M20, but since the clouds show signs of heating by the stars there they must be spatially coincident with it. A collision is therefore highly possible. In this paper we present the new CO J = 1–0 and J = 3–2 observations of the colliding clouds in M20 performed with the Mopra and ASTE telescopes. The high-resolution observations revealed that the two molecular clouds have peculiar spatial and velocity structures, i.e., a spatially complementary distribution between the two clouds and a bridge feature that connects the two clouds in velocity space. Based on a new comparison with numerical models, we find that this complementary distribution is an expected outcome of cloud–cloud collisions, and that the bridge feature can be interpreted as the turbulent gas excited at the interface of the collision. Our results reinforce the cloud–cloud collision scenario in M20.
The Origin of the Near-infrared Excess in SN Ia 2012dn: Circumstellar Dust around the Super-Chandrasekhar Supernova Candidate
Authors: Nagao Takashi , Maeda Keiichi , Yamanaka Masayuki 
Published: January 2017

Abstract
The nature of progenitors of the so-called super-Chandrasekhar candidate Type Ia supernovae (SC-SNe Ia) has been actively debated. Recently, Yamanaka et al. reported a near-infrared (NIR) excess for SN 2012dn and proposed that the excess originates from an echo by circumstellar (CS) dust. In this paper, we examine a detailed distribution of the CS dust around SN 2012dn and investigate implications of the CS dust echo scenario for general cases of SC-SNe Ia. We find that a disk/bipolar CS medium configuration reproduces the NIR excess fairly well, where the radial density distribution is given by a stationary mass loss. The inner radius of the CS dust is 0.04 pc. The mass-loss rate of the progenitor system is estimated to be

and

M
⊙ yr−1 for the disk and bipolar CS medium configurations, respectively, which adds further support for the single-degenerate scenario. Our models limit SN 2009dc, another SC-SN Ia, to have a dust mass less than 0.16 times that of SN 2012dn. While this may merely indicate some variation on the CS environment among SC-SNe Ia, this could raise another interesting possibility. There could be two classes among SC-SNe Ia: the brighter SC-SNe Ia in a clean environment (SN 2009dc) and the fainter SC-SNe Ia in a dusty environment (SN 2012dn).
iPTF Discovery of the Rapid “Turn-on” of a Luminous Quasar
Authors: Gezari S. , Hung T. , Cenko S. B. , Blagorodnova N. , Yan Lin , Kulkarni S. R. , Mooley K. , Kong A. K. H. , Cantwell T. M. , Yu P. C. , Cao Y. , Fremling C. , Neill J. D. , Ngeow C.-C. , Nugent P. E. , Wozniak P. 
Published: January 2017

Abstract
We present a radio-quiet quasar at z = 0.237 discovered “turning on” by the intermediate Palomar Transient Factory (iPTF). The transient, iPTF 16bco, was detected by iPTF in the nucleus of a galaxy with an archival Sloan Digital Sky Survey spectrum with weak narrow-line emission characteristic of a low-ionization nuclear emission-line region (LINER). Our follow-up spectra show the dramatic appearance of broad Balmer lines and a power-law continuum characteristic of a luminous (

erg s−1) type 1 quasar 12 yr later. Our photometric monitoring with PTF from 2009–2012 and serendipitous X-ray observations from the XMM-Newton Slew Survey in 2011 and 2015 constrain the change of state to have occurred less than 500 days before the iPTF detection. An enhanced broad Hα/[O iii] λ5007 line ratio in the type 1 state relative to other changing-look quasars also is suggestive of the most rapid change of state yet observed in a quasar. We argue that the >10 increase in Eddington ratio inferred from the brightening in UV and X-ray continuum flux is more likely due to an intrinsic change in the accretion rate of a preexisting accretion disk than an external mechanism such as variable obscuration, microlensing, or the tidal disruption of a star. However, further monitoring will be helpful in better constraining the mechanism driving this change of state. The rapid “turn-on” of the quasar is much shorter than the viscous infall timescale of an accretion disk and requires a disk instability that can develop around a

black hole on timescales less than 1 yr.
Internal Gravity Waves in the Magnetized Solar Atmosphere. I. Magnetic Field Effects
Authors: Vigeesh G. , Jackiewicz J. , Steiner O. 
Published: January 2017

Abstract
Observations of the solar atmosphere show that internal gravity waves are generated by overshooting convection, but are suppressed at locations of magnetic flux, which is thought to be the result of mode conversion into magnetoacoustic waves. Here, we present a study of the acoustic-gravity wave spectrum emerging from a realistic, self-consistent simulation of solar (magneto)convection. A magnetic field free, hydrodynamic simulation and a magnetohydrodynamic (MHD) simulation with an initial, vertical, homogeneous field of 50 G flux density were carried out and compared with each other to highlight the effect of magnetic fields on the internal gravity wave propagation in the Sun’s atmosphere. We find that the internal gravity waves are absent or partially reflected back into the lower layers in the presence of magnetic fields and argue that the suppression is due to the coupling of internal gravity waves to slow magnetoacoustic waves still within the high-β region of the upper photosphere. The conversion to Alfvén waves is highly unlikely in our model because there is no strongly inclined magnetic field present. We argue that the suppression of internal waves observed within magnetic flux concentrations may also be due to nonlinear breaking of internal waves due to vortex flows that are ubiquitously present in the upper photosphere and the chromosphere.
Application of the Nonballistic Model to the Black Hole Candidate XTE J1752-223 and the Quasar NRAO 150
Authors: Zheng T. Y. , Gong B. P. 
Published: January 2017

Abstract
Optical and radio observations of the black hole candidate XTE J1752-223 have exhibited a slightly curved motion of the jet components, which is associated with its radio light curve. In addition, observations of the quasar NRAO 150 have revealed a core–jet structure wobbling with a high angular speed. In this paper, the phenomena displayed in these two different sources are interpreted as the precession of a bent jet. In such a scenario, hot spots reproduced at different separations from the core precess on the same precession cone, in which different components correspond to different propagation times to the observer. By fitting the kinematics of the components of XTE J1752-223 and its light curve with a curved pattern of precession period 314 days, we find that the propagation time can make an earlier event appear later, and the jet axis can oscillate during its precession. Simulating the quasar NRAO 150 with the same scenario reveals that the knots at larger separation from the core precess at a slower speed than those closer in. A possible mechanism relating to the cooling time of a component is proposed. These three new results are of importance in understanding the physics underlying the curved jet as well as the activity of the central engine of different black hole systems.
AR Sco: A Precessing White Dwarf Synchronar?
Authors: Katz J. I. 
Published: January 2017

Abstract
The emission of the white dwarf–M dwarf binary AR Sco is driven by the rapid synchronization of its white dwarf, rather than by accretion. Synchronization requires a magnetic field ∼100 Gauss at the M dwarf and

Gauss at the white dwarf, larger than the fields of most intermediate polars but within the range of fields of known magnetic white dwarfs. The spindown power is dissipated in the atmosphere of the M dwarf, within the near zone of the rotating white dwarf’s field, by magnetic reconnection, accelerating particles that produce the observed synchrotron radiation. The displacement of the optical maximum from conjunction may be explained either by dissipation in a bow wave as the white dwarf’s magnetic field sweeps past the M dwarf or by a misaligned white dwarf rotation axis and oblique magnetic moment. In the latter case the rotation axis precesses with a period of decades, predicting a drift in the orbital phase of the optical maximum. Binaries whose emission is powered by synchronization may be termed synchronars, in analogy to magnetars.
Testing Metal-poor Stellar Models and Isochrones with HST Parallaxes of Metal-poor Stars
Authors: Chaboyer B. , McArthur B. E. , O’Malley E. , Benedict G. F. , Feiden G. A. , Harrison T. E. , McWilliam A. , Nelan E. P. , Patterson R. J. , Sarajedini A. 
Published: January 2017

Abstract

Hubble Space Telescope (HST) fine guidance sensor observations were used to obtain parallaxes of eight metal-poor ([Fe/H] < −1.4) stars. The parallaxes of these stars determined by the new Hipparcos reduction average 17% accuracy, in contrast to our new HST parallaxes, which average 1% accuracy and have errors on the individual parallaxes ranging from 85 to 144 μas. These parallax data were combined with HST Advanced Camera for Surveys photometry in the F606W and F814W filters to obtain the absolute magnitudes of the stars with an accuracy of 0.02–0.03 mag. Six of these stars are on the main sequence (MS) (with −2.7 < [Fe/H] < −1.8) and are suitable for testing metal-poor stellar evolution models and determining the distances to metal-poor globular clusters (GCs). Using the abundances obtained by O’Malley et al., we find that standard stellar models using the VandenBerg & Clem color transformation do a reasonable job of matching five of the MS stars, with HD 54639 ([Fe/H] = −2.5) being anomalous in its location in the color–magnitude diagram. Stellar models and isochrones were generated using a Monte Carlo analysis to take into account uncertainties in the models. Isochrones that fit the parallax stars were used to determine the distances and ages of nine GCs (with −2.4 ≤ [Fe/H] ≤ −1.9). Averaging together the age of all nine clusters led to an absolute age of the oldest, most metal-poor GCs of 12.7 ± 1.0 Gyr, where the quoted uncertainty takes into account the known uncertainties in the stellar models and isochrones, along with the uncertainty in the distance and reddening of the clusters.
Galaxy Environment in the 3D-HST Fields: Witnessing the Onset of Satellite Quenching at z ∼ 1–2
Authors: Fossati M. , Wilman D. J. , Mendel J. T. , Saglia R. P. , Galametz A. , Beifiori A. , Bender R. , Chan J. C. C. , Fabricius M. , Bandara K. , Brammer G. B. , Davies R. , Förster Schreiber N. M. , Genzel R. , Hartley W. , Kulkarni S. K. , Lang P. , Momcheva I. G. , Nelson E. J. , Skelton R. , Tacconi L. J. , Tadaki K. , Übler H. , van Dokkum P. G. , Wisnioski E. , Whitaker K. E. , Wuyts E. , Wuyts S. 
Published: January 2017

Abstract
We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-Hubble Space Telescope (HST)/CANDELS deep fields. Leveraging the spectroscopic and grism redshifts from the 3D-HST survey, multiwavelength photometry from CANDELS, and wider field public data for edge corrections, we derive densities in fixed apertures to characterize the environment of galaxies brighter than

mag in the redshift range

. By linking observed galaxies to a mock sample, selected to reproduce the 3D-HST sample selection and redshift accuracy, each 3D-HST galaxy is assigned a probability density function of the host halo mass, and a probability that it is a central or a satellite galaxy. The same procedure is applied to a z = 0 sample selected from Sloan Digital Sky Survey. We compute the fraction of passive central and satellite galaxies as a function of stellar and halo mass, and redshift, and then derive the fraction of galaxies that were quenched by environment specific processes. Using the mock sample, we estimate that the timescale for satellite quenching is

it is longer at lower stellar mass or lower redshift, but remarkably independent of halo mass. This indicates that, in the range of environments commonly found within the 3D-HST sample (

), satellites are quenched by exhaustion of their gas reservoir in the absence of cosmological accretion. We find that the quenching times can be separated into a delay phase, during which satellite galaxies behave similarly to centrals at fixed stellar mass, and a phase where the star formation rate drops rapidly (

Gyr), as shown previously at z = 0. We conclude that this scenario requires satellite galaxies to retain a large reservoir of multi-phase gas upon accretion, even at high redshift, and that this gas sustains star formation for the long quenching times observed.
Origin and Properties of Quiet-time 0.11–1.28 MeV Nucleon−1 Heavy-ion Population Near 1 au
Authors: Dayeh M. A. , Desai M. I. , Mason G. M. , Ebert R. W. , Farahat A. 
Published: January 2017

Abstract
Using measurements from the Advanced Composition Explorer/Ultra-Low Energy Isotope Spectrometer near 1 au, we surveyed the composition and spectra of heavy ions (He-through-Fe) during quiet times from 1998 January 1 to 2015 December 31 at suprathermal energies between ∼0.11 and ∼1.28 MeV nucleon−1. The selected time period covers the maxima of solar cycles 23 and 24 and the extended solar minimum in between. We find the following. (1) The number of quiet hours in each year correlates well with the sunspot number, year 2009 was the quietest for about 82% of the time. (2) The composition of the quiet-time suprathermal heavy-ion population (3He, C-through-Fe) correlates well with the level of solar activity, exhibiting SEP-like composition signatures during solar maximum, and CIR- or solar wind-like composition during solar minimum. (3) The heavy-ion (C–Fe) spectra exhibit suprathermal tails at energies of 0.11–0.32 MeV nucleon−1 with power-law spectral indices ranging from 1.40 to 2.97. Fe spectra soften (steepen, i.e., spectral index increases) smoothly with increasing energies compared with Fe, indicating a rollover behavior of Fe at higher energies (0.45–1.28 MeV nucleon−1). (4) Spectral indices of Fe and O do not appear to exhibit clear solar cycle dependence. (2) and (3) imply that during IP quiet times and at energies above ∼0.1 MeV nucleon−1, the IP medium is dominated by material from prior solar and interplanetary events. We discuss the implications of these extended observations in the context of the current understanding of the suprathermal ion population near 1 au.
Le chaînon manquant ? Les modèles institutionnels pour expliquer l’évolution du 1 % le plus riche
Authors: Zorn Nicolas 
Published: January 2017

Depuis le milieu des années 1980, la part des revenus captée par le 1 % le plus riche des pays développés a connu deux tendances distinctes ; les pays anglophones ont vécu une hausse importante alors que les pays non anglophones ont plutôt connu une hausse modérée et parfois même un recul. Les facteurs institutionnels (sans lien avec l’aspect linguistique) permettent le mieux d’expliquer ces différentes évolutions. Or, l’importance des institutions dans l’économie serait avant tout de nature combinatoire. Comme le soulignent les théories des modèles/variétés de capitalisme, une même institution n’aura pas nécessairement le même impact dans un contexte institutionnel différent, et deux combinaisons différentes d’institutions peuvent produire des effets similaires. Nous postulons que les modèles institutionnels permettent d’expliquer l’évolution du 1 % le plus riche. Ce texte examine la compatibilité des facteurs institutionnels identifiés par la littérature avec quatre théories de modèles institutionnels différenciant les pays anglophones des autres pays développés. Cette approche ajoute un élément important dans la compréhension de l’évolution des hauts revenus.
Recent Economic Developments and the Implications for Fiscal Policy in Open Economy Macroeconomics
Authors: Zeyneloğlu İrem , Koenig Gilbert 
Published: January 2017

Cet article présente et commente les apports récents de la macroéconomie internationale à l’analyse de la politique budgétaire face à trois évolutions économiques de ces dernières années : l’intégration internationale croissante des marchés, la crise de la dette publique et l’émergence d’une union monétaire, comme celle de l’Europe. Ces apports se placent dans le cadre de modèles d’équilibre général à deux pays. Le processus d’intégration internationale croissante des marchés financiers et des marchés de biens a suscité des travaux qui reconsidèrent l’impact de ce processus sur les incidences économiques de la politique budgétaire. En second lieu, la crise de la dette publique qui se manifeste dans la plupart des pays développés a conduit à une analyse de la politique budgétaire fondée sur une meilleure gestion des dépenses publiques et à la spécification d’une expansion budgétaire qui internalise la nécessité de préserver le caractère soutenable du déficit et de l’endettement public. En troisième lieu, la création de l’Union monétaire européenne et la récente crise économique globale ont suscité l’intérêt pour les gains potentiels que peuvent générer la stabilisation et la coopération budgétaires et stimulé les recherches sur la combinaison optimale des politiques budgétaires et monétaires dans un cadre dynamique et stochastique.