bluuebunny/crossref_metadata_2025_split huggingface dataset:
Learning Multi-human Optical Flow
Authors: Ranjan Anurag , Hoffmann David T. , Tzionas Dimitrios , Tang Siyu , Romero Javier , Black Michael J. 
Published: January 2020

AbstractThe optical flow of humans is well known to be useful for the analysis of human action. Recent optical flow methods focus on training deep networks to approach the problem. However, the training data used by them does not cover the domain of human motion. Therefore, we develop a dataset of multi-human optical flow and train optical flow networks on this dataset. We use a 3D model of the human body and motion capture data to synthesize realistic flow fields in both single- and multi-person images. We then train optical flow networks to estimate human flow fields from pairs of images. We demonstrate that our trained networks are more accurate than a wide range of top methods on held-out test data and that they can generalize well to real image sequences. The code, trained models and the dataset are available for research.
The structure–activity relationship review of the main bioactive constituents of Morus genus plants
Authors: Yan Jiejing , Ruan Jingya , Huang Peijian , Sun Fan , Zheng Dandan , Zhang Yi , Wang Tao 
Published: January 2020

Abstract
Morus genus plants are mainly distributed in the temperate to tropical areas over the world and include 17 species and two subspecies. Due to their excellent pharmacological activity, security in food additives and high value in the national economy, Morus genus plants have drawn more and more attention in recent years. In the light of the references published over the last few decades, flavonoids, benzofurans, stilbenes, and Diels–Alder adducts have been reported to be the main bioactive constituents of Morus genus plants. This review summarizes the compounds with excellent bioactivities isolated from Morus genus plants as well as their structure–activity relationships (SARs), which might be useful for the further research and development of Morus genus plants.

Graphic abstract

The aromatic heterocycles with excellent bioactivities isolated from Morus genus plants as well as their structure–activity relationships (SARs) were summarized.
Nutrient recycling: from waste to crop
Authors: Hidalgo D. , Corona F. , Martín-Marroquín J. M. 
Published: January 2020

AbstractWithin the transition to a bio-based economy from a fossil reserve-based world, we face the vital dare of closing nutrient cycles and moving to a more practical and balanced resource management, taking into account not only the economical but also the environmental perspective. The manufacture and transportation of mineral fertilizers are activities that require large amounts of fossil energy. Therefore, the dependence that agriculture has on fertilizers based on mineral reserves (mainly P, N, and K) should be considered as a very serious threat to human food security and climate change. On the other hand, the existing forecast on phosphorus reserves is pessimistic. According to the latest published figures on population growth and estimated demand for nutrients in the future, depletion of this material is expected to occur within a maximum of 300 years. At the same time, the agricultural demand that exists for mineral fertilizers is constantly growing. The main reason is the increase in the world population, together with the increase in meat consumption and the popularity of energy crops. Despite these negative perspectives, the processing or elimination of waste streams causes uncontrolled dispersion in the environment of a large amount of minerals. Thus, a new global effort is needed to draw a new scenario where improved nutrient use efficiency and, at the same time, reduced nutrient losses provide the bases for a more circular economy, to produce more necessary inputs, as food or energy, as the same time as decreasing environmental impact. This paper will show the process options which can “upcycle” and recover residual nutrients to high-quality end-products, defined by efficient nutrient use and will reveal the key issues to face with novel biofertilizer products and changing policies.
BIBLICAL LAW IN GRECO-ROMAN ATTIRE: THE CASE OF LEVIRATE MARRIAGE IN LATE ANTIQUE CHRISTIAN LEGAL TRADITIONS
Authors: Monnickendam Yifat 
Published: January 2020

AbstractWhat happened to biblical law when transferred into late antique Christianity? How can answering this question provide a paradigm that helps us understand the rise and development of late antique Christian legal traditions? In the first centuries of the Common Era, the Christian legal tradition began to evolve in Roman, Greek, rabbinic, and biblical contexts. Focusing on the biblical institution of levirate marriage, this article offers a paradigm that elucidates how Christians might have adopted, adapted, and sometimes rejected their legal heritage; it may illuminate the overall development of Christian legal discourse. Following a short survey of the rabbinic adaptation of biblical levirate marriage and the Roman and Christian rulings regarding this practice, I analyze the Christian exegetical and theological discourse on levirate marriage, focusing on the acceptance or rejection of levirate marriage as a whole and adaptations to the biblical institution. This analysis demonstrates the disparity between the rabbinic discourse, the Christian and Roman rulings, and the theological and exegetical discourse. It shows how Christians remodeled their biblical heritage according to Greek and Roman legal concepts, namely the Roman adoption and the Greekepiklerate, and treated it as part of inheritance law and child-parent relationships, whereas the rabbis used different adaptations and treated it as part of matrimonial law and sexual relationships. This discussion therefore recontextualizes the legal discourse, positioning the Christian approach to levirate marriage as a complex case of legal transplant and adaptation of a legal heritage.
M 1–92 revisited: the chemistry of a common envelope nebula?
Authors: Alcolea Javier , Agúndez Marcelino , Bujarrabal Valentín , Castro Carrizo Arancha , Desmurs Jean-François , Sánchez-Contreras Carmen , Santander-García Miguel 
Published: January 2020

AbstractWe report on new molecular-line observations of the bipolar pre-planetary nebula M 1–92. The new IRAM 30 m MRT and NOEMA data shows the presence of shock induced chemistry in the nebula. From the derived [17O]/[18O] ratio, we suggest that the sudden mass loss event responsible for the formation of the nebula 1200 yr ago may also have resulted in the premature end of the AGB phase of the central star.
Binary evolution and double sequences of blue stragglers in globular clusters
Authors: Jiang Dengkai , Chen Xuefei , Li Lifang , Han Zhanwen 
Published: January 2020

AbstractBinary evolution can produce different blue-straggler binaries, for example, blue stragglers with a bright, red component, or with a faint, blue component. In globular clusters, these blue-straggler binaries are generally observed as a single star, because two components can not be distinguished. Therefore, these blue-straggler binaries can be located in different regions of the color-magnitude diagram of globular clusters, e.g. blue sequence and red sequence observed in M30. We suggest that binary evolution can contribute to the blue stragglers in both of the sequences. Some blue stragglers in the blue sequence may have a faint white dwarf companion, while the red sequence includes some binaries experiencing mass transfer. It should be noted that the red sequence may also have other binaries, for example, the binaries just finished the mass transfer, and the binaries including a blue straggler (the accretors) that have evolved away from the blue sequence.
Populations of accreting white dwarfs
Authors: Chen Hai-Liang , Woods Tyrone E. , Yungelson Lev , Gilfanov Marat , Han Zhanwen 
Published: January 2020

AbstractUsing a hybrid binary population synthesis approach, we modelled the formation and evolution of populations of accreting white dwarfs (WDs) for differing star formation histories. We found that the delay time distribution of SNe Ia in the single degenerate scenario is inconsistent with observations. Additionally, we found that our predicted X-ray and UV emission of populations of accreting WDs are consistent with the X-ray luminosities of early-type galaxies observed by Chandra and the HeII 4686 Å/Hβ line ratio measured in stacked SDSS spectra of passively evolving galaxies. Moreover, we found that the majority of current novae in elliptical-like galaxies have low-mass WDs, long decay times, long recurrence periods and are relatively faint. In contrast, the majority of current novae in spiral-like galaxies have massive WDs, short decay times, short recurrence periods and are relatively bright. Our predicted distribution of mass-loss timescales in an M31-like galaxy is consistent with observations for Andromeda.
Kepler K2: A Search for Very Red Stellar Objects
Authors: Hartig E. , Hinkle K. H. , Lebzelter T. 
Published: January 2020

AbstractAnalyzing 41 targets data of the Kepler K2 Campaign 2 mission suspected to be Long Period Variables (LPVs), we developed a method for the prediction of periods longer than the observation period of 77.48d using the 3500 data points provided by K2. The ‘Self-Flat-Field’ method (K2SFF or SFF) of the ‘ Kepler K2 High Level Science Product’ (K2HLSP) corrected the instrumental effects best.
The Impact of AGB Stars on Galaxies
Authors: Boyer Martha L. 
Published: January 2020

AbstractAt the end of their evolution, asymptotic giant branch (AGB) stars undergo strong pulsation, mass loss, and dust production. Their mass loss results in substantial chemical and dust enrichment of the interstellar medium. Dust evolution models and isotope abundances in presolar grains suggest that AGB stars play a key role in both dust evolution and the star formation process. They are also the brightest stars in galaxies, potentially dominating in the near-infrared. As a result, AGB stars have a significant influence on the evolution and appearance of their host galaxies and thus must be accounted for when interpreting a galaxy’s integrated light. I will highlight new results that describe the impact AGB stars have on galaxies, including how AGB stars are used to probe galaxy evolution.
The End: Witnessing the Death of Extreme Carbon Stars
Authors: Sloan G. C. , Kraemer K. E. , McDonald I. , Zijlstra A. A. 
Published: January 2020

AbstractA Last affiliation changed 3 to 4 against MS. Please check and confirm if it is fine. small number of the sample of 184 carbon stars in the Magellanic Clouds show signs that they are in the act of evolving off of the asymptotic giant branch. Most carbon stars grow progressively redder in all infrared colors and develop stronger pulsation amplitudes as their circumstellar dust shells become optically thicker. The reddest sources, however, have unexpectedly low pulsation amplitudes, and some even show blue excesses that could point to deviations from spherical symmetry as they eject the last of their envelopes. Previously, all dusty carbon-rich AGB stars have been labeled “extreme,” but that term should be reserved for the truly extreme carbon stars. These objects may well hold the clues needed to disentangle what actually happens when a star ejects the last of its envelope and evolves off of the AGB.
AGB stars in Gaia DR2
Authors: Lebzelter Thomas , Mowlavi Nami , Marigo Paola , Lecoeur-Taibi Isabelle , Trabucchi Michele , Pastorelli Giada , Wood Peter ,   Collaboration
Published: January 2020

AbstractGaia Data Release 2 (DR2; April 25, 2018) provides astrometric and photometric data for more than a billion stars - among them many AGB stars. As part of DR2 the light curves of several hundreds of thousand variable stars, including many long-period variable (LPV) candidates, are made available. The publication of the light curves and LPV-specific attributes in addition to the standard DR2 products offers a unique opportunity to study AGB stars. In this contribution, we present the first results for AGB stars based on the analysis of the Gaia data performed after their release. As an immediate result of the Gaia DR2 LPV database we introduce a new photometric index capable of efficiently distinguishing AGB stars of different masses and chemical properties.
Metallic Line Doubling in the Spectra of the Variable Star R Scuti
Authors: Chafouai K. , Benhida A. , Sefyani F. , Ghout A. , Benkhaldoun Z. , Mathias P. , Gillet D. , El Jariri Y. 
Published: January 2020

AbstractIn this work, we present spectroscopic results of the variable star R Scuti, obtained during the campaign of measures led in 2016 at the Oukaimeden observatory in Morrocco. High resolution spectra (R ≍ 12 000) were obtained between 4289 Å and 7125 Å. This intensive observing campaign spanned over 26 nights from June to November 2016.
The discovery of an asymmetric detached shell around the “fresh” carbon AGB star TX Psc
Authors: Brunner M. , Mečina M. , Maercker M. , Dorfi E. A. , Kerschbaum F. , Olofsson H. , Rau G. 
Published: January 2020

AbstractWe present ALMA observations of the circumstellar envelope around the AGB carbon star TX Psc in molecular CO(2–1) emission, and detect a previously unknown detached shell with filamentary structure and elliptical shape. Up to now, all observed detached shells are found around carbon AGB stars and are of remarkable spherical symmetry. The elliptical shell around TX Psc is the first clear exception to that rule, with TX Psc being classified as rather ’’fresh’’ carbon star, that most likely has only experienced very few thermal pulses yet. We investigate and discuss the 3D structure of the CSE and its most likely formation scenarios, as well as the link of this peculiar detached shell to the AGB evolutionary status of TX Psc.
Morpho-Kinematics of the Circumstellar Environments around Post-AGB Stars
Authors: Ueta Toshiya , Izumiura Hideyuki , Yamamura Issei , Otsuka Masaaki 
Published: January 2020

AbstractWe observed two proto-planetary nebulae, HD 56126 representing a source with an elliptical circumstellar shell, and IRAS 16594−4656 representing a source with a bipolar circumstellar shell, with ALMA in the 12CO and 13CO J=3−2 lines and neighboring continuum to see how the morpho-kinematics of CO gas and dust emission properties in their circumstellar environments differ.
Herschel Planetary Nebula Survey Plus (HerPlaNS+)
Authors: Ueta Toshiya , Aleman Isabel , Otsuka Masaaki , Exter Katrina ,   the HerPlaNS consortium
Published: January 2020

AbstractWe present the current status update of the Herschel Planetary Nebula Survey Plus project (HerPlaNS+) based on the original General Observer HerPlaNS survey program during the OT1 cycle and the follow-up exhaustive archival search of PN observations using the PACS and SPIRE instruments on-board the Herschel Space Observatory.
Understanding jets in post-AGB close binaries
Authors: Bollen Dylan , Kamath Devika , Van Winckel Hans , De Marco Orsola 
Published: January 2020

AbstractWe have discovered jets in post-AGB binaries. The orbital motion allows us to carry out tomography of the jet as light from the primary star shines through the jet cone. Jets play a major role in many astrophysical environments, from young stellar objects to galaxies. They are also used to study the energetics of accretion phenomena in systems such as red transients and stellar mergers. We use high-resolution, optical, time-series spectra to constrain theories of jet launching, and the impact of jets on the evolution of these post-AGB binaries.
Accretion in common envelope evolution
Authors: Chamandy Luke , Frank Adam , Blackman Eric G. , Carroll-Nellenback Jonathan , Liu Baowei , Tu Yisheng , Nordhaus Jason , Chen Zhuo , Peng Bo 
Published: January 2020

AbstractCommon envelope evolution (CEE) occurs in some binary systems involving asymptotic giant branch (AGB) or red giant branch (RGB) stars, and understanding this process is crucial for understanding the origins of various transient phenomena. CEE has been shown to be highly asymmetrical and global 3D simulations are needed to help understand the dynamics. We perform and analyze hydrodynamic CEE simulations with the adaptive mesh refinement (AMR) code AstroBEAR, and focus on the role of accretion onto the companion star. We bracket the range of accretion rates by comparing a model that removes mass and pressure using a subgrid accretion prescription with one that does not. Provided a pressure-release valve, such as a bipolar jet, is available, super-Eddington accretion could be common. Finally, we summarize new results pertaining to the energy budget, and discuss the overall implications relating to the feasibility of unbinding the envelope in CEE simulations.
Modelling gas and dust around carbon stars in the Large Magellanic Cloud
Authors: Srinivasan Sundar , Chen I.-K. , Scicluna P. , Cami J. , Kemper F. 
Published: January 2020

AbstractIn order to investigate the effect of dust production on the molecular absorption, we model the dust continuum and the 7.5 and 13.7 μm acetylene absorption features in the Spitzer IRS spectra of 148 carbon stars in the Large Magellanic Cloud (LMC). Our preliminary investigation does not find a strong correlation between the dust-production rate and the column density of acetylene for the LMC sample. However, we will construct more models at high optical depths and probe a larger range of dust properties for more robust results.
Resolved stellar populations: the outlook for JWST and ELT
Authors: Tolstoy Eline 
Published: January 2020

AbstractThe study of the resolved stellar populations in nearby galaxies and star clusters through the analysis of colour-magnitude diagrams provides the most detailed and quantitative determination of the star formation histories of these systems. The properties of different age populations provide an insight into distinct physical processes taking place during the entire history of the stellar system. The detection of the oldest main sequence turn-offs is currently restricted to stellar systems within the Local Group due to the limitations in spatial resolution and flux sensitivity of available telescopes. Individual stars need to be detected and accurately distinguished from their neighbours. To improve this situation we need to build new telescopes with larger primary mirrors that can deliver a very stable image quality at the diffraction limit. Over the next decade we can look forward to new larger telescope in space: the James Webb Space Telescope, currently scheduled to be launched in 2021; and several large telescope projects, the largest of which is the 39m ESO extremely large telescope on Cerro Armazones in Chile, currently scheduled to start operations in 2024.
Infrared Studies of the Variability and Mass Loss of Some of the Dustiest Asymptotic Giant Branch Stars in the Magellanic Clouds
Authors: Sargent B. , Srinivasan S. , Boyer M. , Feast M. , Whitelock P. , Marengo M. , Groenewegen M. A. T. , Meixner M. , Hora J. L. , Otsuka M. 
Published: January 2020

AbstractThe asymptotic giant branch (AGB) stars with the reddest colors have the largest amounts of circumstellar dust. AGB stars vary in their brightness, and studies show that the reddest AGB stars tend to have longer periods than other AGB stars and are more likely to be fundamental mode pulsators than other AGB stars. Such stars are difficult to study, as they are often not detected at optical wavelengths. Therefore, they must be observed at infrared wavelengths. Using the Spitzer Space Telescope, we have observed a sample of very dusty AGB stars in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) over Cycles 9 through 12 during the Warm Spitzer mission. For each cycle’s program, we typically observed a set of AGB stars at both 3.6 and 4.5 μm wavelength approximately monthly for most of a year. We present results from our analysis of the data from these programs.
AGB stars in binaries and the common envelope interaction
Authors: De Marco Orsola 
Published: January 2020

AbstractOne may argue that, today, proceedings articles are not useful. Results belong in refereed papers and even reviews are best in publications that are long enough to do justice to the topic reviewed. In this short review, reflecting a presentation that was given at the IAU343 symposium, Why Galaxies Care about AGB Stars, I have therefore endeavoured to include some practical snippets that, while remaining true to the presentation, also provide a quick look up reference. After a reminder of how few AGB stars actually interact with a companion, and a pictorial summary of the types of interactions that can happen, I list the rapidly growing body of 3D common envelope simulations. Next, I highlight shortfalls and successes of simulations, and then spend some time comparing the two simulations of planetary nebulae from common envelope interactions to date. Finally, I summarise a handful of results pertaining to common envelope interactions between giants and planets.
The mass-loss characteristics of AGB stars An observational view
Authors: Ramstedt Sofia 
Published: January 2020

AbstractThe massive outflows of gas and dust which characterize giant stars on the Asymptotic Giant Branch (AGB), build cool circumstellar envelopes readily observed at infrared (IR) and sub-millimeter wavelengths. The observations will give the amount of matter lost by the star, the wind velocity (in the case of spectral line observations), and, when the spatial resolution is sufficient, the wind evolution over time. To gain detailed insight into the mass-loss process, we study the nearby (closer than 1 kpc) stars. Through these investigations we aim to determine the best constrained wind properties available. By combining this with theoretical results, mass-loss estimates for more distant sources can also be significantly improved. ALMA has opened up new opportunities to study the winds of AGB stars. The DEATHSTAR project (www.astro.uu.se/deathstar) has mapped the circumstellar CO emission from so far ∼50 nearby M- and C-type AGB stars. The data will initially be used to give a definitive mass-loss prescription for the sample sources, but the large-bandwidth observations opens for many different legacy projects. The current status and results are presented.
Abundances of C, N, and O in AGB Giants and Model Atmospheres
Authors: Aringer B. , Marigo P. , Nowotny W. , Girardi L. , Mečina M. , Nanni A. 
Published: January 2020

AbstractBased on hydrostatic models we discuss the effects of molecular opacities and abundance changes concerning C, N or O on the atmospheric structures, spectra and photometric properties of C/M AGB giants.
Forecast Skill of Minimum and Maximum Temperatures on Subseasonal‐to‐Seasonal Timescales Over South Africa
Authors: Phakula Steven , Landman Willem A. , Engelbrecht Christien J. , Makgoale Thabo 
Published: January 2020

AbstractForecast skill of three subseasonal‐to‐seasonal models and their ensemble mean outputs are evaluated in predicting the surface minimum and maximum temperatures at subseasonal timescales over South Africa. Three skill scores (correlation of anomaly, root‐mean‐square error, and Taylor diagrams) are used to evaluate the models. It is established that the subseasonal‐to‐seasonal models considered here have skill in predicting both minimum and maximum temperatures at subseasonal timescales. The correlation of anomaly indicates that the multimodel ensemble outperforms the individual models in predicting both minimum and maximum temperatures for the day 1–14, day 11–30, and full calendar month timescales during December months. The Taylor diagrams suggest that the European Centre for Medium‐Range Weather Forecasts model and MM performs better for the day 11–30 timescale for both minimum and maximum temperatures. In general, the models perform better for minimum than maximum temperatures in terms of root‐mean‐square error. In fact, the skill difference in terms of correlation of anomalies (CORA) is small.