bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Cultural Revolution as a Crisis of Representation
Authors: Thornton Patricia M. 
Published: October 2016

AbstractThe May 16 Notification, which set the agenda for the Cultural Revolution, named the movement's key targets as those “representatives of the bourgeoisie who have sneaked into the Party, the government, the army, and all spheres of culture.” The ensuing uprising of students and workers, many of whom claimed to be the loyal “representatives” of revolutionary and radical forces at the grassroots of society, exposed the fulminating crisis of political representation under CCP rule. This article considers the Cultural Revolution as a manifestation of a continuing crisis of representation within revolutionary socialism that remains unresolved to the present day, as demonstrated by the tepid popular response to Jiang Zemin's “three represents” and widespread contemporary concerns about the Party's “representativeness” (daibiaoxing代表性) in the wake of market reform. Although the Cultural Revolution enabled both public debate of and political experimentation with new forms of representative politics, the movement failed to resolve the crisis. The Party's lingering disquiet regarding issues of representation thus remains one legacy of the Cultural Revolution.
Multiple solutions for a critical fractional elliptic system involving concave–convex nonlinearities
Authors: Chen Wenjing , Deng Shengbing 
Published: October 2016

We are concerned with the multiplicity of solutions to the system driven by a fractional operator with homogeneous Dirichlet boundary conditions. Namely, using fibering maps and the Nehari manifold, we obtain multiple solutions to the following fractional elliptic system:where Ω is a smooth bounded set in ℝn, n > 2s, with s ∈ (0, 1); (–Δ)s is the fractional Laplace operator;, λ, μ > 0 are two parameters; the exponent n/(n – 2s) ⩽ q < 2; α > 1, β > 1 satisfy is the fractional critical Sobolev exponent.
How can UNESCO World Heritage Criteria be applied to the “Windows to the Universe” Sites?
Authors: Cotte Michel 
Published: October 2016

AbstractThis communication proposes a methodical approach trying to link the concept of “Windows to the Universe” to the uses of the Criteria defined by the World Heritage Convention (UNESCO 1972). The first issue is well advanced today after more than 10 years of active studies and preservation projects such as “Starlight Reserves” by specialists of astronomy, archaeoastronomy and environmental sciences. The second issue is related to a UNESCO Convention ruled by the WH Committee that has led to the recognition of around 1000 World Heritage sites over 40 years. The official booklet Operational Guidelines for the Implementation of the World Heritage Convention (latest edition 2015) (UNESCO 2015) summarizes conceptual ideas and methodological recommendations for WH nominations. In practice the WH Committee's decisions rely on the scientific and professional evaluation of each site by UNESCO's advisory bodies: ICOMOS for cultural heritage and IUCN for natural heritage.The first goal of this presentation is to establish appropriate understanding of a very specific conceptual approach (Windows to the Universe) in the context of a very large UN Convention (the World Heritage List) related both to cultural and natural heritage in general. The second goal is to give a readable understanding of the WH requirements coming from the strict evaluation of the “Outstanding Universal Value” (OUV) of a given place, including the choice of WH Criteria expressing OUV with respect to the format of the Guidelines. Furthermore, and due to concepts coming from two very different fields, the communication aims to present a practical methodology in the case of a possible WH nomination: how to understand relationships between different classes of value and how to demonstrate OUV and justify the choice of Criteria for the place. Beyond potential WH projects, obviously limited in number, the communication tries to propose an efficient and general methodology for assessing the value and creating understanding of places having a “Windows to the Universe” facet.
Astronomical Heritage and Aboriginal People: Conflicts and Possibilities
Authors: López Alejandro Martín 
Published: October 2016

AbstractIn this presentation we address issues relating to the astronomical heritage of contemporary aboriginal groups and other minorities. We deal specially with intangible astronomical heritage and its particularities. Also, we study (from ethnographic experience with Aboriginal groups, Creoles and Europeans in the Argentine Chaco) the conflicts referring to the different ways in which the natives' knowledge and practice are categorized by the natives themselves, by scientists, state politicians, professional artists and NGOs. Furthermore, we address several cases that illustrate these kinds of conflicts. We aim to analyze the complexities of patrimonial policies when they are applied to practices and representations of contemporary communities involved in power relations with national states and the global system. The essentialization of identities, the folklorization of representations and practices, and the fossilization of aboriginal peoples are some of the risks of applying the label “cultural heritage” without a careful consideration of each specific case.In particular we suggest possible ways in which the international scientific community could collaborate to improve the agenda of national states instead of reproducing colonial prejudices. In this way, we aim to contribute to the promotion of respect for ethnic and religious minorities.
Evolution of Scholarly Publishing and Library Services in Astronomy Its Impact, Challenges, and Opportunities
Authors: Wesley Hema , Sheshadri Geetha 
Published: October 2016

AbstractScholarly publishing and its procedures have evolved rapidly, forcefully, and incredibly. Technical advances in the production and promotion of science content have dramatically augmented the visibility and reach, deepened the impact and intensified the thrust of science journal content. These changes range from checking text on perforated tapes to pit stop; from hot metal types to CTP; and from Gutenberg to colour digital printers. Intrinsic and inextricable to this revolutionary aspect of evolution in scholarly publishing is the evolution of library services in astronomy which catapulted library resources from preprints on shelves to customised digital repositories and from communicating observational data through postal telegrams to Tablets. What impact does this unique blend of revolutionary advances have on science and society, what are the consequent challenges, and what are the opportunities that can metamorphose from challenges inherent in the power and potential of the ‘published word’?The perspectives expressed in this paper stem from learning experiences of the authors at the Indian Academy of Sciences, publishers of ten science journals including the Journal of Astrophysics and Astronomy, and at the Raman Research Institute Library (in which Astronomy is one of the core subjects for research)
Carbonaceous Material in Extra-terrestrial Matter
Authors: Martins Zita 
Published: October 2016

AbstractComets, asteroids, meteorites, micrometeorites, interplanetary dust particles (IDPs), and ultra-carbonaceous Antarctic micrometeorites (UCAMMs) may contain carbonaceous material, which was exogenously delivered to the early Earth. Carbonaceous chondrites have an enormous variety of extra-terrestrial compounds, including all the key compounds important in terrestrial biochemistry. Comets contain several carbon-rich species and, in addition, the hypervelocity impact-shock of a comet can produce several α-amino acids. The analysis of the carbonaceous content of extra-terrestrial matter provides a window into the resources delivered to the early Earth, which may have been used by the first living organisms.
The molecular universe: from observations to laboratory and back
Authors: van Dishoeck Ewine F. 
Published: October 2016

AbstractThis brief overview stresses the importance of molecular processes in modern astrophysics and provides examples where the availability of new laboratory or theoretical data proved crucial in the analysis. This includes basic data such as spectroscopy and collisional rate coefficients, but also an improved understanding of reactions and photoprocesses in the gaseous and solid state. In spite of many lingering uncertainties, the future of molecular astrophysics is bright with new facilities such as ALMA, JWST and ELTs on the horizon. Together, they will allow increased understanding of the journey of gas and solids from clouds to stars and planets, and back to the interstellar medium.
Divisions Panel Discussion: Astronomy for Development
Authors: Govender Kevin , Hemenway Mary Kay , Wolter Anna , Haghighipour Nader , Yan Yihua , van Dishoeck E.F. , Silva David , Guinan Edward 
Published: October 2016

AbstractThe main purpose of this panel discussion was to encourage conversation around potential collaborations between the IAU Office of Astronomy for Development (OAD) and IAU Divisions. The discussion was facilitated by the OAD and the conversation revolved mainly around two questions: (i) What should the OAD be doing to enhance the work of the Divisions? (ii) What could the Divisions (both members and respective scientific discipline in general) contribute towards the implementation of the IAU strategic plan?
Session 21.2 – Measurement of Light at Night
Authors: Wainscoat Richard J. 
Published: October 2016

AbstractThe introduction of the mercury vapor lamp for general lighting in the 1930s probably marked the beginning of significant light pollution. Lighting levels have increased slowly, year-to-year, with sky brightness levels increasing only slowly on timescales of a year; no measurement protocols or instruments existed to quantify this increase. However, on timescales of 10--20 years, or on generational timescales, the increases in night sky levels, particularly in urban areas, have been dramatic. Younger people speak with their parents or grandparents who remark how beautiful the sky used to be, and how many stars they could see when they when they were younger. Older people can themselves remember how many stars were visible in the sky when they were younger. Whole generations of children now grow up without ever seeing the Milky Way.Society has not had tools to easily measure sky brightness, and monitoring from space has only recently become available. A subtle increase of 10% sky brightness per year, for example, is not noticeable to the human eye on the time scale of a year, and has been tolerated by society. But such an increase compounds to an increase of a factor 2.6 in 10 years, 6.7 in 20 years, and a factor 45 in 40 years, corresponding to a dramatic increase in sky brightness, an almost complete loss in ability to see faint objects in the night sky, and rendering the sky unusable for most forms of astronomy. The most striking examples are the urban observatories found in many major cities that can no longer be used.Session 2 was primarily focused on measurement of light at night, with an emphasis on measurement of light pollution. It comprised of 6 papers that are summarized below. Over the last decade, our ability to measure light pollution has grown tremendously, and the instrumentation needed to produce reliable quantitative measurements has become much more affordable, and now includes consumer grade digital cameras and even smart phones. During this same time period, light pollution has continued to grow. The widespread changes from mostly high-pressure sodium lighting to LED lighting that are now occurring make continued monitoring and measurement of light pollution particularly important into the future.Complete presentations may be viewed at: http://www.noao.edu/education/IAUGA2015FM21
Extended halos and intracluster light using Planetary Nebulae as tracers in nearby clusters
Authors: Arnaboldi Magda 
Published: October 2016

AbstractSince the first detection of intracluster planetary nebulae in 1996, imaging and spectroscopic surveys identified such stars to trace the radial extent and the kinematics of diffuse light in clusters. This topic of research is tightly linked with the studies of galaxy formation and evolution in dense environment, as the spatial distribution and kinematics of planetary nebulae in the outermost regions of galaxies and in the cluster cores is relevant for setting constraints on cosmological simulations. In this sense, extragalactic planetary nebulae play a very important role in the near-field cosmology, in order to measure the integrated mass as function of radius and the orbital distribution of stars in structures placed in the densest regions of the nearby universe.
Time dependent chemistry in Planck clouds?
Authors: Berczik Peter , Bertsyk Peter , Fehér Orsolya , Harju Jorma , Onishi Toshykazu , Tóth László Viktor 
Published: October 2016

AbstractWe present a set of time dependent chemical evolution models (based on the UMIST† astrochemistry 2012 code, McElroy et al. (2013) for a range of initial physical cloud parameters: 10 K < T < 20 K; 103 cm−3 < n(H2) < 5 ⋅ 104 cm−3; 1 < AV < 10 and with estimated values of scaled interstellar ultraviolet radiation field. We compare our chemical model results with the relative abundances of: CO, CH, OH, HCO+, HCN, HNC, NH3, N2H+ and H2CO molecules. We find significant time dependent variations of the chemical ratios of: X(NH3/H2); X(HCO+/H2) and X(HCO+/NH3). The input physical conditions were taken from Fehér O. et al. (2015) at 16 positions along the TMC-1 dark cloud. The NH3 and HCO+ relative densities based on the observations of Fehér O. et al. (2015) help to find the “chemical age” of the given position in the evolution curves.
A correlation between SN II metal line strength and host H ii region oxygen abundance
Authors: Anderson Joseph P. , Gutiérrez Claudia P. , Dessart Luc 
Published: October 2016

AbstractDessart et al., demonstrated that type II supernova (SN II) model spectra present increasing metal line strength with increasing progenitor metallicity. To confront these models with observations, we obtained a large sample of SN II host H ii region emission line spectroscopy. We show that inferred SN II host H ii region metallicities have a statistically significant correlation with the strength of SN II metal lines, specifically Fe ii 5018Å.
Massive Black Holes in Merging Galaxies
Authors: Volonteri Marta , Bogdanović Tamara , Dotti Massimo , Colpi Monica 
Published: October 2016

AbstractThe dynamics of massive black holes (BHs) in galaxy mergers is a rich field of research that has seen much progress in recent years. In this contribution we briefly review the processes describing the journey of BHs during mergers, from the cosmic context all the way to when BHs coalesce. If two galaxies each hosting a central BH merge, the BHs would be dragged towards the center of the newly formed galaxy. If/when the holes get sufficiently close, they coalesce via the emission of gravitational waves. How often two BHs are involved in galaxy mergers depends crucially on how many galaxies host BHs and on the galaxy merger history. It is therefore necessary to start with full cosmological models including BH physics and a careful dynamical treatment. After galaxies have merged, however, the BHs still have a long journey until they touch and coalesce. Their dynamical evolution is radically different in gas-rich and gas-poor galaxies, leading to a sort of “dichotomy” between high-redshift and low-redshift galaxies, and late-type and early-type, typically more massive galaxies.
Modeling the Observability of Recoiling Black Holes as Offset Quasars
Authors: Blecha Laura , Torrey Paul , Vogelsberger Mark , Genel Shy , Springel Volker , Sijacki Debora , Snyder Gregory , Bird Simeon , Nelson Dylan , Xu Dandan , Hernquist Lars 
Published: October 2016

AbstractThe merger of two supermassive black holes (SMBHs) imparts a gravitational-wave (GW) recoil kick to the remnant SMBH, which can even eject the SMBH from its host galaxy. An actively-accreting, recoiling SMBH may be observable as an offset quasar. Prior to the advent of a space-based GW observatory, detections of these offset quasars may offer the best chance for identifying recent SMBH mergers. Indeed, observational searches for recoiling quasars have already identified several promising candidates. However, systematic searches for recoils are currently hampered by large uncertainties regarding how often offset quasars should be observable and where they are most likely to be found. Motivated by this, we have developed a model for recoiling quasars in a cosmological framework, utilizing information about the progenitor galaxies from the Illustris cosmological hydrodynamic simulations. For the first time, we model the effects of BH spin alignment and recoil dynamics based on the gas-richness of host galaxies. We predict that if BH spins are not highly aligned, seeing-limited observations could resolve offset AGN, making them promising targets for all-sky surveys. The rarity of large broad-line offsets among SDSS quasars is likely due in part to selection effects but suggests that spin alignment plays a role in suppressing recoils. Nonetheless, in our most physically motivated model where alignment occurs only in gas-rich mergers, hundreds of offset AGN should be found in all-sky surveys. Our findings strongly motivate a dedicated search for recoiling AGN.
Formation, destruction and chemical influences of water ice: A review of recent laboratory results
Authors: Öberg Karin I. 
Published: October 2016

AbstractWater ice is the dominant constituent of icy grain mantles in the interstellar medium, and as such one of the most abundant species during all stages of star and planet formation. Its formation through atom addition reactions on grain surfaces, its destruction through different desorption channels, and its influence on the chemistry and desorption efficiencies of other species in icy grain mantles have all been the objects of intense study. This contribution reviews our current understanding of these processes, and the laboratory experiments that have been instrumental in establishing the existing paradigm.
Water in small bodies of the Solar System
Authors: Bockelee-Morvan Dominique 
Published: October 2016

AbstractWater in form of ice or vapour is observed in comets, transneptunian objects and icy satellites formed in the outer regions of the Solar System, as well as in objects orbiting in the inner Solar System, such as dwarf planet Ceres. I will present an overview of the water content and properties in these objects and the implications in terms of solar system formation and evolution.
Internal sources of water on Earth
Authors: Elkins-Tanton Linda T. 
Published: October 2016

AbstractRocky planets are built through a series of highly energetic accretionary impacts. The accreting bodies are thought to carry small amounts of water to the growing planet, but it is debated whether the planet can retain this water through the accretionary process, or if water needs to be added largely after the planet is complete and cooled. Most of the relatively few measurements of deuterium to hydrogen in cometary water do not match Earths water, though the single example of 103P/Hartley 2 is a good match (Mumma & Charnley 2011, Hartogh et al. 2011). Alexander et al. (2012) point out, however, that organic materials in comets have far higher D/H than does their water, so in bulk no comet matches Earths D/H ratio, not even comet Hartley. Meteorites provide evidence that the material that built planets had small but sufficient amounts of water, and analysis of its isotopic composition demonstrates that water from rocky material, and not comets, provided water to the Earth (Alexander et al. 2012). This current evidence that Earths water came from rocky asteroidal material does not solve the question of whether this material was the accreting material that built the planet, or if it was added later. Mission data from the Moon and Mercury demonstrates that those bodies are not completely devoid of volatiles (McCubbin et al. 2010, Saal et al. 2008, Peplowski et al. 2011). The Moon, in particularly, has small amounts of internal water that survived its energetic origins (Hauri et al. 2011). Thus, the giant accretionary impacts that build planets do not completely dry them, and the water from their initial building blocks can be retained. If volatiles are delivered and partly retained during accretion, then the initial habitability of a young planet may be set by degassing of a magma ocean. Models predict that cooling can result in liquid water oceans within ten or tens of millions of years (Abe and Matsui 1986, Elkins-Tanton 2011). Thus, rocky planets in solar systems similarly composed to our own have a good chance of forming with water oceans, and of being habitable, at least for some period of time.
Calculating Pre-SN Mass-Loss Histories from Post-Explosion Observations and the Special Case of SN 2006gy
Authors: Fox Ori D. 
Published: October 2016

AbstractA growing number of SNe now show evidence for significant interaction between the forward shock and a pre-existing circumstellar medium (CSM) formed by the pre-SN mass-loss. The SN community likes to argue that it can indirectly constrain the progenitor systems for these SNe by measuring the wind speeds, densities, compositions, and asymmetries of the CSM. The measurements, however, rely on a number of assumptions and can result in degeneracies that straddle the divide between RSGs and more massive stars. Furthermore, the implications of the measured properties may sometimes be simplified to fit a SN expert's relatively basic understanding of stellar wind parameters. Given the opportunity to have experts in massive stars, cool stars, and supernovae together in the same room, I thought it would be a good opportunity to review the different methods employed by the SN community to measure mass-loss rates. I will then provide an update from a recent Spitzer survey on the measured CSM properties from different subclasses of SNe with known shock interaction (including SLSNe, SNe II, IIn, Ibc, and even Ia-CSM). Finally, I will present new HST data on the SLSN Type IIn SN 2006gy and discuss the implications on the progenitor system and pre-SN mass-loss.
Combined stellar evolution and spectroscopic modeling of massive stars
Authors: Groh Jose H. 
Published: October 2016

AbstractThe morphological appearance of massive stars during their evolution and at the pre-SN stage is very uncertain, both from theoretical and observational perspectives. We recently developed coupled stellar evolution and atmospheric modeling of stars done with the Geneva and CMFGEN codes, for initial masses between 9 and 120 M⊙. We are able to predict the observables such as the high-resolution spectrum and broadband photometry. Here I discuss how the spectrum of a massive star changes across its evolution and before death. Our models allow, for the first time, direct comparison between predictions from stellar evolution models and observations of SN progenitors.
Revealing the true face of the behemoths
Authors: Ohnaka Keiichi 
Published: October 2016

AbstractTo improve our understanding of the mass loss in red supergiants (RSGs), it is of paramount importance to observe the wind acceleration region close to the star with high spatial resolution. I review the recent progress in milliarcsecond-resolution imaging of the surface and atmosphere of RSGs with optical and infrared long-baseline interferometers. The high resolution images of RSGs have revealed the true face of these behemoths, which have turned out to be very complex.