bluuebunny/crossref_metadata_2025_split huggingface dataset:
Neptune's Latitudinal Variations as Viewed with ALMA
Authors: Tollefson Joshua , Pater Imke de , Luszcz-Cook Statia , DeBoer David 
Published: June 2019

Abstract
We present spatially resolved millimeter maps of Neptune between 95 and 242 GHz taken with the Atacama Large Millimeter/submillimeter Array (ALMA) in 2016–2017. The millimeter weighting functions peak between 1 and 10 bar on Neptune, lying in between the altitudes probed at visible/infrared and centimeter wavelengths. Thus, these observations provide important constraints on the atmospheric structure and dynamics of Neptune. We identify seven well-resolved latitudinal bands of discrete brightness temperature variations, on the order of 0.5–3 K in all three observed ALMA spectral bands. We model Neptune’s brightness temperature using the radiative-transfer code Radio-BEAR and compare how various H2S, CH4, and ortho-/para-H2 abundance profiles can fit the observed temperature variations across the disk. We find that observed variations in brightness temperature with latitude can be explained by variations in the H2S profile that range from sub- to supersaturations at altitudes above the 10 bar pressure level, while variations in CH4 improve the quality of fit near the equator. At the south polar cap, our best-fit model has a depleted deep atmospheric abundance of H2S from 30 to only 1.5 times the protosolar value, while simultaneously depleting the CH4 abundance. This pattern of enhancement and depletion of condensible species is consistent with a global circulation structure where enriched air rises at the midlatitudes (32°–12°S) and north of the equator (2°–20°N), and dry air descends at the poles (90°–66°S) and just south of the equator (12°S–2°N). Our analysis finds more complex structure near the equator than accounted for in previous circulation models.
Red and Reddened: Ultraviolet through Near-infrared Observations of Type Ia Supernova 2017erp*
Authors: Brown Peter J. , Hosseinzadeh Griffin , Jha Saurabh W. , Sand David , Vieira Ethan , Wang Xiaofeng , Dai Mi , Dettman Kyle G. , Mould Jeremy , Uddin Syed , Wang Lifan , Arcavi Iair , Bento Joao , Burns Chris R. , Diamond Tiara , Hiramatsu Daichi , Howell D. Andrew , Hsiao E. Y. , Marion G. H. , McCully Curtis , Milne Peter A. , Mirzaqulov Davron , Ruiter Ashley J. , Valenti Stefano , Xiang Danfeng 
Published: June 2019

Abstract
We present space-based ultraviolet/optical photometry and spectroscopy with the Swift Ultra-Violet/Optical Telescope and Hubble Space Telescope (HST), respectively, along with ground-based optical photometry and spectroscopy and near-infrared spectroscopy of supernova SN 2017erp. The optical light curves and spectra are consistent with a normal SN Ia. Compared to previous photometric samples in the near-ultraviolet (NUV), SN 2017erp has UV colors that are redder than NUV-blue SNe Ia corrected to similar optical colors. The chromatic difference between SNe 2011fe and 2017erp is dominated by the intrinsic differences in the UV rather than the expected dust reddening. This chromatic difference is similar to the SALT2 color law, derived from rest-frame ultraviolet photometry of higher redshift SNe Ia. Differentiating between intrinsic UV diversity and dust reddening can have important consequences for determining cosmological distances with rest-frame ultraviolet photometry. This ultraviolet spectroscopic series is the first from HST of a normal, albeit reddened, NUV-red SN Ia and is important for analyzing SNe Ia with intrinsically redder NUV colors. We show model comparisons suggesting that metallicity could be the physical difference between NUV-blue and NUV-red SNe Ia, with emission peaks from reverse fluorescence near 3000 Å implying a factor of ∼10 higher metallicity in the upper layers of SN 2017erp compared to SN 2011fe. Metallicity estimates are very model dependent, however, and there are multiple effects in the UV. Further models and UV spectra of SNe Ia are needed to explore the diversity of SNe Ia, which show seemingly independent differences in the near-UV peaks and mid-UV flux levels.
Evidence of New Magnetic Transitions in Late-type Dwarfs from Gaia DR2
Authors: Lanzafame Alessandro C. , Distefano Elisa , Barnes Sydney A. , Spada Federico 
Published: June 2019

Abstract
The second Gaia data release contains the identification of 147,535 low-mass (

) rotational modulation variable candidates on (or close to) the main sequence, together with their rotation period and modulation amplitude. The richness, the period and amplitude range, and the photometric precision of this sample make it possible to unveil, for the first time, signatures of different surface inhomogeneity regimes in the amplitude–period density diagram. The modulation amplitude distribution shows a clear bimodality, with an evident gap at periods P ≲ 2 days. The low-amplitude branch, in turn, shows a period bimodality with a main clustering at periods P ≈ 5–10 days and a secondary clustering of ultra-fast rotators at P ≲ 0.5 day. The amplitude–period multimodality is correlated with the position in the period–absolute magnitude (or period–color) diagram, with the low- and high-amplitude stars occupying different preferential locations. Here we argue that such a multimodality provides further evidence of the existence of different regimes of surface inhomogeneities in young and middle-age low-mass stars and we lay out possible scenarios for their evolution, which manifestly include rapid transitions from one regime to another. In particular, the data indicate that stars spinning up close to breakup velocity undergo a very rapid change in their surface inhomogeneities configuration, which is revealed here for the first time. The multimodality can be exploited to identify field stars of age ∼100–600 Myr belonging to the slow-rotator low-amplitude sequence, for which age can be estimated from the rotation period via gyrochronology relationships.
Global Energetics of Solar Flares. VII. Aerodynamic Drag in Coronal Mass Ejections
Authors: Aschwanden Markus J. , Gopalswamy Nat 
Published: June 2019

Abstract
The free energy that is dissipated in a magnetic reconnection process of a solar flare, generally accompanied by a coronal mass ejection (CME), has been considered as the ultimate energy source of the global energy budget of solar flares in previous statistical studies. Here we explore the effects of the aerodynamic drag force on CMEs, which supplies additional energy from the slow solar wind to a CME event, besides the magnetic energy supply. For this purpose, we fit the analytical aerodynamic drag model of Cargill and Vršnak et al. to the height–time profiles r(t) of LASCO/SOHO data in 14,316 CME events observed during the first 8 yr (2010–2017) of the Solar Dynamics Observatory era (ensuring EUV coverage with AIA). Our main findings are (1) a mean solar wind speed of w = 472 ± 414 km s−1, (2) a maximum drag-accelerated CME energy of E
drag ≲ 2 × 1032 erg, (3) a maximum flare-accelerated CME energy of E
flare ≲ 1.5 × 1033 erg, (4) the ratio of the summed kinetic energies of all flare-accelerated CMEs to the drag-accelerated CMEs amounts to a factor of 4, (5) the inclusion of the drag force slightly lowers the overall energy budget of CME kinetic energies in flares from ≈7% to ≈4%, and (6) the arrival times of CMEs at Earth can be predicted with an accuracy of ≈23%.
Gamma-Ray Emission from the Impulsive Phase of the 2017 September 6 X9.3 Flare
Authors: Lysenko Alexandra L. , Anfinogentov Sergey A. , Svinkin Dmitry S. , Frederiks Dmitry D. , Fleishman Gregory D. 
Published: June 2019

Abstract
We report hard X-ray and gamma-ray observations of the impulsive phase of the SOL2017-09-06T11:55 X9.3 solar flare. We focus on a high-energy part of the spectrum, >100 keV, and perform time resolved spectral analysis for a portion of the impulsive phase, recorded by the Konus-Wind experiment, that displayed prominent gamma-ray emission. Given a variety of possible emission components contributing to the gamma-ray emission, we employ a Bayesian inference to build the most probable fitting model. The analysis confidently revealed contributions from nuclear deexcitation lines, electron–positron annihilation line at 511 keV, and a neutron capture line at 2.223 MeV along with two components of the bremsstrahlung continuum. The revealed time evolution of the spectral components is particularly interesting. The low-energy bremsstrahlung continuum shows a soft–hard–soft pattern typical for impulsive flares, while the high-energy one shows a persistent hardening at the course of the flare. The neutron capture line emission shows an unusually short time delay relative to the nuclear deexcitation line component, which implies that the production of neutrons was significantly reduced soon after the event onset. This in turn may imply a prominent softening of the accelerated proton spectrum at the course of the flare, similar to the observed softening of the low-energy component of the accelerated electrons responsible for the low-energy bremsstrahlung continuum. We discuss possible physical scenarios, which might result in the obtained relationships between these gamma-ray components.
Turbulent Diffusion Derived from the Motions of SDO/AIA Coronal Bright Points
Authors: Skokić I. , Brajša R. , Sudar D. , Ruždjak D. , Saar S. H. 
Published: June 2019

Abstract
Diffusion of magnetic elements on the Sun has an important role in current solar dynamo models as a part of the mechanism for redistribution of the magnetic field and as an important part for maintaining the solar activity cycle. The main goal is to determine the character of solar magnetic diffusivity and a value of the diffusion coefficient by analyzing the motions of coronal bright points (CBPs) within the frame of the random walk model. We tracked positions of CBPs in Solar Dynamics Observatory/Atmospheric Imaging Assembly images for a period of 5 months and examined their displacement spectrum. We calculated spectral index and diffusion coefficient from the spectrum and investigated their variation with temporal and spatial scale. For the first time, variations of the spectral index with heliographic latitude and time were analyzed. Our results indicate subdiffusion with the spectral index γ = 0.70 ± 0.01 and the corresponding diffusion coefficient with a value decreasing from 400 to 100 km2 s−1 for temporal scales of 103–105 s and spatial scales of (1.5–7) × 103 km. Seemingly random variations around the mean value of spectral index were found, with peak-to-peak amplitudes <0.30 with time and <0.10 with latitude. The main conclusion is that CBP motions are consistent with a subdiffusion process.
An Older, More Quiescent Universe from Panchromatic SED Fitting of the 3D-HST Survey
Authors: Leja Joel , Johnson Benjamin D. , Conroy Charlie , Dokkum Pieter van , Speagle Joshua S. , Brammer Gabriel , Momcheva Ivelina , Skelton Rosalind , Whitaker Katherine E. , Franx Marijn , Nelson Erica J. 
Published: June 2019

Abstract
Galaxy observations are influenced by many physical parameters: stellar masses, star formation rates (SFRs), star formation histories (SFHs), metallicities, dust, black hole activity, and more. As a result, inferring accurate physical parameters requires high-dimensional models that capture or marginalize over this complexity. Here we reassess inferences of galaxy stellar masses and SFRs using the 14-parameter physical model Prospector-
α built in the Prospector Bayesian inference framework. We fit the photometry of 58,461 galaxies from the 3D-HST catalogs at 0.5 < z < 2.5. The resulting stellar masses are ∼0.1–0.3 dex larger than the fiducial masses while remaining consistent with dynamical constraints. This change is primarily due to the systematically older SFHs inferred with Prospector. The SFRs are ∼0.1–1+ dex lower than UV+IR SFRs, with the largest offsets caused by emission from “old” (t > 100 Myr) stars. These new inferences lower the observed cosmic SFR density by ∼0.2 dex and increase the observed stellar mass growth by ∼0.1 dex, finally bringing these two quantities into agreement and implying an older, more quiescent universe than found by previous studies at these redshifts. We corroborate these results by showing that the Prospector-
α SFHs are both more physically realistic and much better predictors of the evolution of the stellar mass function. Finally, we highlight examples of observational data that can break degeneracies in the current model; these observations can be incorporated into priors in future models to produce new and more accurate physical parameters.
ZTF18aalrxas: A Type IIb Supernova from a Very Extended Low-mass Progenitor
Authors: Fremling C. , Ko H. , Dugas A. , Ergon M. , Sollerman J. , Bagdasaryan A. , Barbarino C. , Belicki J. , Bellm E. , Blagorodnova N. , De K. , Dekany R. , Frederick S. , Gal-Yam A. , Goldstein D. A. , Golkhou V. Z. , Graham M. , Kasliwal M. , Kowalski M. , Kulkarni S. R. , Kupfer T. , Laher R. R. , Masci F. J. , Miller A. A. , Neill J. D. , Perley D. A. , Rebbapragada U. D. , Riddle R. , Rusholme B. , Schulze S. , Smith R. M. , Tartaglia L. , Yan Lin , Yao Y. 
Published: June 2019

Abstract
We investigate ZTF18aalrxas, a double-peaked Type IIb core-collapse supernova (SN) discovered during science validation of the Zwicky Transient Facility. ZTF18aalrxas was discovered while the optical emission was still rising toward the initial cooling peak (0.7 mag over 2 days). Our observations consist of multi-band (ultraviolet and optical) light curves (LCs), and optical spectra spanning from ≈0.7 to ≈180 days past the explosion. We use a Monte-Carlo based non-local thermodynamic equilibrium model that simultaneously reproduces both the 56Ni-powered bolometric LC and our nebular spectrum. This model is used to constrain the synthesized radioactive nickel mass (0.17 M
☉) and the total ejecta mass (1.7 M
☉) of the SN. The cooling emission is modeled using semi-analytical extended envelope models to constrain the progenitor radius (790–1050 R
⊙) at the time of explosion. Our nebular spectrum shows signs of interaction with a dense circumstellar medium (CSM), and this spectrum is modeled and analyzed to constrain the amount of ejected oxygen (0.3–0.5 M
☉) and the total hydrogen mass (≈0.15 M
☉) in the envelope of the progenitor. The oxygen mass of ZTF18aalrxas is consistent with a low (12–13 M
☉) zero-age main-sequence mass progenitor. The LCs and spectra of ZTF18aalrxas are not consistent with massive single-star SN Type IIb progenitor models. The presence of an extended hydrogen envelope of low mass, the presence of a dense CSM, the derived ejecta mass, and the late-time oxygen emission can all be explained in a binary model scenario.
The Globular Cluster Origin of the Milky Way Outer Bulge: Evidence from Sodium Bimodality
Authors: Lee Young-Wook , Kim Jenny J. , Johnson Christian I. , Chung Chul , Jang Sohee , Lim Dongwook , Kang Yijung 
Published: June 2019

Abstract
Recent investigations of the double red clump in the color–magnitude diagram of the Milky Way bulge cast serious doubts on the structure and formation origin of the outer bulge. Unlike previous interpretation based on an X-shaped bulge, stellar evolution models and CN-band observations have suggested that this feature is another manifestation of the multiple stellar population phenomenon observed in globular clusters (GCs). This new scenario requires a significant fraction of the outer bulge stars with chemical patterns uniquely observed in GCs. Here we show from homogeneous high-quality spectroscopic data that the red giant branch stars in the outer bulge (>5.°5 from the Galactic center) are clearly divided into two groups according to Na abundance in the [Na/Fe]−[Fe/H] plane. The Na-rich stars are also enhanced in Al, while the differences in O and Mg are not observed between the two Na groups. The population ratio and the Na and Al differences between the two groups are also comparable with those observed in metal-rich GCs. The only plausible explanation for these chemical patterns and characteristics appears to be that the outer bulge was mostly assembled from disrupted proto-GCs in the early history of the Milky Way.
L’emploi accompagné
Authors: Brouant Philippe 
Published: June 2019

La réadaptation professionnelle constitue un droit pour le citoyen. Pourtant, elle continue à présenter de sérieuses difficultés pour les personnes en situation de handicap psychique à la recherche d’un travail. Philippe Brouant expose la supériorité du modèle consistant à insérer d’emblée et à soutenir en même temps sur l’activité du travail (place and train). Il l’associe au programme d’insertion et de soutien individualisé pour l’emploi accompagné ou IPS : Individual Placement and Support. En résulte l’objectif d’un rétablissement et d’une restauration du pouvoir d’agir et de décider.
Conserver son pouvoir d’agir au travail en milieu ordinaire, avec un handicap psychique
Authors: Chappe Rebecca , Dumont Rémy 
Published: June 2019

Rébecca CHAPPE dirige un cabinet ACTIPH Conseil. Elle a conçu son intervention en association avec Rémy Dumont qu’elle a soutenu. Le titre de son article, « Conserver son pouvoir d’agir au travail en milieu ordinaire, avec un handicap psychique », dit l’essentiel de son propos. Par un accompagnement dans le travail en milieu ordinaire, elle parvient à maintenir l’emploi, en restaurant le pouvoir d’agir et la liberté de choix. Elle expose sa méthode : prise en compte de l’ensemble de la vie quotidienne et du plan d’action dans l’entreprise associant la personne intéressée, ses collègues et l’employeur. Le résultat se manifeste par un effet positif durable pour tous. En prolongement de son article, Rémy Dumont écrit un résumé de son exposé oral. Dans ce témoignage, il indique sa satisfaction, tant pour lui-même que pour l’ensemble de son service. Il a intitulé ce texte : « Conserver son pouvoir d’agir et conserver son emploi ».
Outras Guerras Frias: os embates entre neoliberais e neoconservadores estadunidenses diante da Revolução Nicaraguense
Authors: Moll Neto Roberto 
Published: June 2019

Em meio a Guerra Fria, a Revolução Sandinista abalou os interesses dos Estados Unidos na região da América Central e do Caribe. Durante o Governo Reagan, os Estados Unidos intensificaram as ações de intervenção na região a fim de derrubar o Governo Sandinista. Este artigo pretende demonstrar que, mesmo no campo ortodoxo da política estadunidense, o papel dos Estados Unidos em face da revolução na Nicarágua não estava pré definido exclusivamente em uma visão de mundo única e que, portanto, haviam propostas concorrentes, que, inclusive, compreendiam a realidade na região a partir de dinâmicas próprias, e não apenas em função da Guerra Fria.

Abstract
Other Cold Wars: the clashes between neoliberals and neoconservatives in the face of the Nicaraguan Revolution
In the midst of the Cold War, the Sandinista Revolution shook US objectives in the Central America and Caribbean. During the Reagan Administration, the United States stepped up intervention in the region to overthrow the Sandinista Government. This paper intends to demonstrate that even in the orthodox field of American politics, the role of the United States in the face of the revolution in Nicaragua was not exclusively defined in a single perceptions and that therefore there were competing proposals that even understood the reality in the region from its own dynamics, and not only because of the Cold War.

Resumen
Otras guerras frías: los embates entre neoliberales y neoconservadores estadunidenses ante la Revolución Nicaragüense
En medio de la Guerra Fría, la Revolución Sandinista sacudió los intereses de Estados Unidos en la región de América Central y del Caribe. Durante el Gobierno Reagan, Estados Unidos intensificó las acciones de intervención en la región a fin de derrocar al Gobierno Sandinista. Este artículo pretende demostrar que, incluso en el campo ortodoxo de la política estadounidense, el papel de los Estados Unidos frente a la revolución en Nicaragua no estaba pre definido exclusivamente en una visión de mundo única y que, por lo tanto, había propuestas concurrentes, que incluso comprendían la realidad en la región a partir de dinámicas propias, y no sólo en función de la Guerra Fría.
A construção de uma crise: usos da história por intelectuais argentinos na contestação aos tratados com o Chile nas décadas de 1960 e 1970
Authors: Passetti Gabriel 
Published: June 2019

Em 1978, os governos militares ditatoriais da Argentina e do Chile estavam à beira da guerra por conta do controle sobre três ilhas a leste do canal Beagle. As insatisfações e controvérsias, de ambos os lados, remontavam a tratados quase centenários. O artigo analisa a produção intelectual e os usos da história nas duas décadas antecedentes à “Crise do Beagle”, demonstrando a construção dos pontos de discórdia: o “expansionismo chileno” e a arbitragem internacional e de que forma estes foram aceitos e disseminados entre civis e militares envoltos pelos pensamentos da Guerra Fria.

Abstract
The construction of a crisis: the uses of history by Argentinean intellectuals and the contest of treaties with Chile in the 1960s and 1970s
In 1978, the military dictatorships of Argentina and Chile were close to war. The tension was around the control of three islands east from the Beagle Channel. Insatisfactions and polemics, on both sides, remained to treaties signed one century ago. The paper analyses the intellectual production and the uses of history on the two decades before the “Beagle Crisis”. It presents the construction of the points of conflict: the “Chilean expansionism” and the international arbitrament. It also presents how it was acepted and circulated between civil and the military envolved in the Cold War logics.

Resumen
La construcción de una crisis: usos de la historia por intelectuales argentinos en la contestación a los tratados con Chile en las decadas de 1960 y 1970
En 1978, los gobiernos de las dictaduras militares de Argentina y Chile se preparaban para la guerra por el contról sobre tres islas a este del canal Beagle. Las insatisfaciones y controversias, de ambos los lados, volvian a tratrados casi centenários. El articulo analisa la producción intelectual y los usos de la história en las dos decadas anteriores a la “Crisis del Beagle”, demonstrando la constucción de los puntos de discórdia: el “expansionismo chileno” y la arbitraje internacional y de que forma estos fueron aceptos y disseminados entre civiles y militares que vivian en los pensamientos de la Guerra Fria.
Sec62 Suppresses Foot-and-Mouth Disease Virus Proliferation by Promotion of IRE1α–RIG-I Antiviral Signaling
Authors: Han Shichong , Mao Lejiao , Liao Ying , Sun Shiqi , Zhang Zhihui , Mo Yaxia , Liu Haiyun , Zhi Xiaoying , Lin Shunmei , Seo Ho Seong , Guo Huichen 
Published: June 2019

Abstract
Foot-and-mouth disease virus (FMDV) is highly infectious and causes a major plague in animal farming. Unfolded protein response is one of the major cellular responses to pathogenic infections, which performs a crucial role in cell survival, apoptosis, and antiviral innate immune response. In this study, we showed that FMDV infection activated two unfolded protein response branches (PERK-eIF2α and ATF6 signaling) in both baby hamster kidney cells (BHK-21) and porcine kidney (PK-15) cells, whereas it suppressed the IRE1α-XBP1 signaling by decreasing IRE1α level. Further study revealed IRE1α signaling as an important antiviral innate immune mechanism against FMDV. Sec62, the transport protein, was greatly decreased at the late stages of FMDV infection. By overexpression and knockdown study, we also found that the expression of Sec62 was positively involved in the levels of IRE1α and RIG-I and subsequent activation of downstream antiviral signaling pathways in FMDV-infected PK-15 cells. Taken together, our study demonstrates that Sec62 is an important antiviral factor that upregulates IRE1α–RIG-I–dependent antiviral innate immune responses, and FMDV evades antiviral host defense mechanism by downregulating Sec62-IRE1α/RIG-I.