bluuebunny/crossref_metadata_2025_split huggingface dataset:
Entrepreneurial Justice: Syria, the Commission for International Justice and Accountability and the Renewal of International Criminal Justice
Authors: Burgis-Kasthala Michelle 
Published: November 2019

Abstract
This article argues that the crisis of governance generated by the Syrian civil war presents both a challenge and an opportunity to practitioners of international criminal justice. The article also argues that, irrespective of the Syrian case, international criminal law (ICL) institutions are in need of innovation and that increasingly ICL discourses display a blurring between public and private idioms. Evaluating the contribution of the Commission of International Justice and Accountability (CIJA) is one way then of assessing how ICL might evolve. This article characterizes CIJA’s work as exemplifying ‘entrepreneurial justice’, not only in Syria but also in a range of other (post-)conflict settings. We can define entrepreneurial justice as the identification of a gap or weakness in existing public accountability fora and the creation of a new private or privatized organization and/or approach that seeks to address (at least part of) this gap. Although questions remain about CIJA’s own accountability, along with its potential contribution to realizing accountability, this article suggests that its presence within the ICL field is a necessary one and that it has already started to have effects within Syria and beyond.
Subduction of non-Newtonian plates: Thin-sheet dynamics of slab necking and breakoff
Authors: Ribe Neil M , Xu Bingrui 
Published: November 2019

Summary
We use a hybrid boundary-integral/thin-sheet (‘BITS’) model to investigate the subduction of 2-D viscous sheets with composite diffusion creep/dislocation creep rheology, with a focus on the conditions required for slab necking and breakoff. To validate the model, we show that its predictions of the sinking speed of the slab follow a universal scaling law identical to one previously derived for purely Newtonian sheets. We obtain analytical expressions for the fiber stress resultant and bending moment of the sheet during deformation by pure stretching and pure bending, respectively, and show that the non-Newtonian dislocation creep component of the rheology significantly weakens the sheet for both types of deformation. We solve the BITS equations for two distinct situations: “free” subduction, in which the slab pulls an attached negatively buoyant plate without hindrance; and “arrested” subduction that slows or stops when a positively buoyant (continental) portion of the attached plate arrives at the trench. Strong lithospheric thinning is difficult to obtain in free subduction and requires dominantly non-Newtonian rheology, i.e. large (>5) values of the characteristic ratio λ of the Newtonian to the non-Newtonian viscosity. However, during arrested subduction strong thinning leading to breakoff occurs for much lower values of λ, and the point of maximum thinning is at shallower depths. These results are explained by a one-dimensional viscous dripping model (‘DRIP’) of a vertical slab with a composite rheology and an arbitrary kinematically prescribed time-dependent convergence rate U0(t). By injecting into DRIP convergence histories predicted by BITS, we find that DRIP reproduces closely the results of the more complicated BITS model. The DRIP model shows that the convergence rate controls slab breakoff in two distinct ways. On the one hand, the rate of lithospheric thinning is proportional to the accumulated convergence, i.e., the time integral of U0(t). The breakoff depth, on the other hand, is controlled by the convergence rate history, being shallower when U0 rapidly decreases (arrested subduction) after an initial period of oceanic subduction.
Cerebellar contribution to the cognitive alterations in SCA1: evidence from mouse models
Authors: Asher Melissa , Rosa Juao-Guilherme , Rainwater Orion , Duvick Lisa , Bennyworth Michael , Lai Ruo-Yah ,   CRC-SCA, Kuo Sheng-Han , Cvetanovic Marija 
Published: November 2019

Abstract
Spinocerebellar ataxia type 1 (SCA1) is a fatal neurodegenerative disease caused by abnormal expansion of glutamine (Q) encoding CAG repeats in the gene Ataxin-1 (ATXN1). Although motor and balance deficits are the core symptoms of SCA1, cognitive decline is also commonly observed in patients. While mutant ATXN1 is expressed throughout the brain, pathological findings reveal severe atrophy of cerebellar cortex in SCA1 patients. The cerebellum has recently been implicated in diverse cognitive functions, yet to what extent cerebellar neurodegeneration contributes to cognitive alterations in SCA1 remains poorly understood. Much of our understanding of the mechanisms underlying pathogenesis of motor symptoms in SCA1 comes from mouse models. Reasoning that mouse models could similarly offer important insights into the mechanisms of cognitive alterations in SCA1, we tested cognition in several mouse lines using Barnes maze and fear conditioning. We confirmed cognitive deficits in Atxn1154Q/2Q knock-in mice with brain-wide expression of mutant ATXN1 and in ATXN1 null mice. We found that shorter polyQ length and haploinsufficiency of ATXN1 do not cause significant cognitive deficits. Finally, ATXN1[82Q ] transgenic mice—with cerebellum limited expression of mutant ATXN1—demonstrated milder impairment in most aspects of cognition compared to Atxn1154Q/2Q mice, supporting the concept that cognitive deficits in SCA1 arise from a combination of cerebellar and extra-cerebellar dysfunctions.
Unique Characteristics of the Exoskeleton of Bythograeid Crab, Austinograea rodriguezensis in the Indian Ocean Hydrothermal Vent (Onnuri Vent Field)
Authors: Cho Boongho , Kim Dongsung , Bae Hyeonmi , Kim Taewon 
Published: November 2019

Abstract
The Indian Ocean hydrothermal vent is a region where a new oceanic crust is formed by magma at the interface of the deep-sea bed over 2000 m in depth. Here we examined for the first time the exoskeleton structure and mechanical properties of the bythograeid crab Austinograea Rodriguezensis living in hydrothermal vents. Scanning electron microscope and energy dispersive x-ray were used for structural analysis, and a nanoindentation system was used for mechanical analysis. The exoskeleton was divided into four layers: epicuticle, exocuticle, endocuticle, and membrane. The thickness of each layer was different from that of other crustaceans previously reported. Additionally, the number of constituent elements, composition ratio, and hardness of each layer were unique among previously studied crabs. This observation indicates that those characteristics might have evolved for creatures with a hard exoskeleton living in the deep-sea hydrothermal vent.
Effects of feeding melatonin during proestrus and early gestation to gilts and parity 1 sows to minimize effects of seasonal infertility1
Authors: Arend Lidia S , Knox Robert V , Greiner Laura L , Graham Amanda B , Connor Joseph F 
Published: November 2019

AbstractThis study tested whether supplemental melatonin given to mimic the extended nighttime melatonin pattern observed in the higher fertility winter season could minimize infertility during summer and fall in swine. Exogenous melatonin was fed during periods coinciding with follicle selection, corpus luteum formation, pregnancy recognition, and early embryo survival. Experiments were conducted at a commercial farm in 12 sequential replicates. In Exp. 1a, mature gilts (n = 420) that had expressed a second estrus were assigned by weight to receive once daily oral Melatonin (MEL, 3 mg) or Control (CON, placebo) at 1400 h for 3 wk starting before insemination at third estrus. In Exp. 1b, parity 1 sows (n = 470) were randomly assigned by lactation length to receive MEL or CON for 3 wk, starting 2 d before weaning. Follicles, estrus, pregnancy, and farrowing data were analyzed for the main effects of treatment, season (4-wk periods), and their interaction. Environmental measures were also analyzed for reproductive responses. In Exp. 1a, there was no effect (P > 0.10) of MEL on age at third estrus (203 d), follicle size after 7 d of treatment (5.0 mm), estrous cycle length (22.6 d), return to service (9.2%), farrowing rate (FR, 80.0%), or total born pigs (TB, 13.6). However, there was an effect of season (P = 0.03) on number of follicles and on gilts expressing estrus within 23 d of the previous estrus (P < 0.005). In Exp. 1b, there was no effect of MEL (P > 0.10) on follicle measures, wean to estrous interval, FR (84.0%), or TB (13.0). But MEL (73.5%) reduced (P = 0.03) estrous expression within 7 d of weaning compared with CON (82.0%) and season (P = 0.001) decreased FR by ~14.0% during mid summer. Also, gilts and parity 1 sows exposed to low light intensity (<45 lx) during breeding had reduced conception (−8%) and farrowing (−15%) rates, compared with higher light intensity. Similarly, high temperatures (>25 °C) during breeding also reduced gilt conception rates by 7%. Although there was clear evidence of seasonal fertility failures in gilts and sows, MEL treatment did not improve fertility in gilts and reduced estrus in parity 1 sows. It is possible that differences in lighting and thermal environments before breeding could explain the differential response to MEL in sows and gilts.
Gessner’s fossil crab
Authors: Etter Walter , Schmidt Olivier 
Published: November 2019

Abstract
Nearly 450 years ago, the Swiss polymath Conrad Gessner was the first to use illustrations in a systematic manner in a book devoted to the subject of fossils. In his treatise De rerum fossilium . . . liber (1565), around 200 single objects are illustrated, of which almost fifty are fossils in the modern sense. Most of the figures were illustrations of pieces from Gessner’s private collection. Against all odds, some of these have survived to the present day in the Natural History Museum in Basel, Switzerland. These remains form the oldest palaeontological reference collection in the world. Among them is the crab that figured prominently in Gessner’s book and became an icon of the early palaeontological literature.
The Association Between Affect and Sleep in Adolescents With and Without FGIDs
Authors: Monzon Alexandra D , Cushing Christopher C , Friesen Craig A , Schurman Jennifer V 
Published: November 2019

Abstract

Objective
Adolescents with chronic pain associated with functional gastrointestinal disorders (FGIDs) experience negative impacts on their health behaviors (i.e., sleep) and are at risk for a range of problems related to negative affect, which may serve to exacerbate one another in a reciprocal fashion. This study aimed to determine if the strength of the relationship between affect and sleep differs across community adolescents and adolescents with FGIDs. It was hypothesized that shorter sleep durations would be associated with more negative affect and longer sleep durations would be associated with more positive affect, and that group membership would moderate these relationships.

Methods
Twenty-five adolescents with FGIDs were compared with 25 matched peers to examine the differential association between affect and total sleep time (TST). Models were estimated using SAS PROC MIXED for inter- and intraindividual differences.

Results
Models predicting TST revealed a significant three-way interaction among weekday, group status, and negative affect. Simple slopes indicated that when negative affect is one standard deviation below the child’s own average on weekends, participants with FGIDs obtained significantly more sleep than those in the comparison group (β = 47.67, p &lt; .05).

Conclusions
The findings of the present study show that when adolescents with FGIDs have lower negative affect on the weekend, when demands are likely reduced, they are able to obtain more TST. These findings confirm that unique relationships exist between negative affect and sleep duration for youth with FGIDs, and their interaction may hold value in understanding and addressing these targets.
Ellipticity of brightest cluster galaxies as tracer of halo orientation and weak-lensing mass bias
Authors: Herbonnet Ricardo , von der Linden Anja , Allen Steven W , Mantz Adam B , Modumudi Pranati , Morris R Glenn , Kelly Patrick L 
Published: November 2019

ABSTRACT
Weak-lensing measurements of the masses of galaxy clusters are commonly based on the assumption of spherically symmetric density profiles. Yet, the cold dark matter model predicts the shapes of dark matter haloes to be triaxial. Halo triaxiality, and the orientation of the major axis with respect to the line of sight, are expected to be the leading cause of intrinsic scatter in weak-lensing mass measurements. The shape of central cluster galaxies (brightest cluster galaxies; BCGs) is expected to follow the shape of the dark matter halo. Here we investigate the use of BCG ellipticity as predictor of the weak-lensing mass bias in individual clusters compared to the mean. Using weak-lensing masses $M^{\rm WL}_{500}$ from the Weighing the Giants project, and M500 derived from gas masses as low-scatter mass proxy, we find that, on average, the lensing masses of clusters with the roundest/most elliptical 25 per cent of BCGs are biased ∼20 per cent high/low compared to the average, as qualitatively predicted by the cold dark matter model. For cluster cosmology projects utilizing weak-lensing mass estimates, the shape of the BCG can thus contribute useful information on the effect of orientation bias in weak-lensing mass estimates as well as on cluster selection bias.
Cosmic rays or turbulence can suppress cooling flows (where thermal heating or momentum injection fail)
Authors: Su Kung-Yi , Hopkins Philip F , Hayward Christopher C , Faucher-Giguère Claude-André , Kereš Dušan , Ma Xiangcheng , Orr Matthew E , Chan T K , Robles Victor H 
Published: November 2019

ABSTRACT
The quenching ‘maintenance’ and ‘cooling flow’ problems are important from the Milky Way through massive cluster elliptical galaxies. Previous work has shown that some source of energy beyond that from stars and pure magnetohydrodynamic processes is required, perhaps from active galactic nuclei, but even the qualitative form of this energetic input remains uncertain. Different scenarios include thermal ‘heating’, direct wind or momentum injection, cosmic ray heating or pressure support, or turbulent ‘stirring’ of the intracluster medium (ICM). We investigate these in $10^{12}\!-\!10^{14}\, {\rm M}_{\odot }$ haloes using high-resolution non-cosmological simulations with the FIRE-2 (Feedback In Realistic Environments) stellar feedback model, including simplified toy energy injection models, where we arbitrarily vary the strength, injection scale, and physical form of the energy. We explore which scenarios can quench without violating observational constraints on energetics or ICM gas. We show that turbulent stirring in the central $\sim 100\,$ kpc, or cosmic ray injection, can both maintain a stable low-star formation rate halo for &gt;Gyr time-scales with modest energy input, by providing a non-thermal pressure that stably lowers the core density and cooling rates. In both cases, associated thermal-heating processes are negligible. Turbulent stirring preserves cool-core features while mixing condensed core gas into the hotter halo and is by far the most energy efficient model. Pure thermal heating or nuclear isotropic momentum injection require vastly larger energy, are less efficient in lower mass haloes, easily overheat cores, and require fine tuning to avoid driving unphysical temperature gradients or gas expulsion from the halo centre.
A pulsar-based time-scale from the International Pulsar Timing Array
Authors: Hobbs G , Guo L , Caballero R N , Coles W , Lee K J , Manchester R N , Reardon D J , Matsakis D , Tong M L , Arzoumanian Z , Bailes M , Bassa C G , Bhat N D R , Brazier A , Burke-Spolaor S , Champion D J , Chatterjee S , Cognard I , Dai S , Desvignes G , Dolch T , Ferdman R D , Graikou E , Guillemot L , Janssen G H , Keith M J , Kerr M , Kramer M , Lam M T , Liu K , Lyne A , Lazio T J W , Lynch R , McKee J W , McLaughlin M A , Mingarelli C M F , Nice D J , Osłowski S , Pennucci T T , Perera B B P , Perrodin D , Possenti A , Russell C J , Sanidas S , Sesana A , Shaifullah G , Shannon R M , Simon J , Spiewak R , Stairs I H , Stappers B W , Swiggum J K , Taylor S R , Theureau G , Toomey L , van Haasteren R , Wang J B , Wang Y , Zhu X J 
Published: November 2019

ABSTRACT
We have constructed a new time-scale, TT(IPTA16), based on observations of radio pulsars presented in the first data release from the International Pulsar Timing Array (IPTA). We used two analysis techniques with independent estimates of the noise models for the pulsar observations and different algorithms for obtaining the pulsar time-scale. The two analyses agree within the estimated uncertainties and both agree with TT(BIPM17), a post-corrected time-scale produced by the Bureau International des Poids et Mesures (BIPM). We show that both methods could detect significant errors in TT(BIPM17) if they were present. We estimate the stability of the atomic clocks from which TT(BIPM17) is derived using observations of four rubidium fountain clocks at the US Naval Observatory. Comparing the power spectrum of TT(IPTA16) with that of these fountain clocks suggests that pulsar-based time-scales are unlikely to contribute to the stability of the best time-scales over the next decade, but they will remain a valuable independent check on atomic time-scales. We also find that the stability of the pulsar-based time-scale is likely to be limited by our knowledge of solar-system dynamics, and that errors in TT(BIPM17) will not be a limiting factor for the primary goal of the IPTA, which is to search for the signatures of nano-Hertz gravitational waves.
Black hole feedback and the evolution of massive early-type galaxies
Authors: Martín-Navarro Ignacio , Burchett Joseph N , Mezcua Mar 
Published: November 2019

Abstract
Observationally, constraining the baryonic cycle within massive galaxies has proven to be quite difficult. In particular, the role of black hole feedback in regulating star formation, a key process in our theoretical understanding of galaxy formation, remains highly debated. We present here observational evidence showing that, at fixed stellar velocity dispersion, the temperature of the hot gas is higher for those galaxies hosting more massive black holes in their centers. Analyzed in the context of well-established scaling relations, particularly the mass–size plane, the relation between the mass of the black hole and the temperature of the hot gas around massive galaxies provides further observational support to the idea that baryonic processes within massive galaxies are regulated by the combined effects of the galaxy halo virial temperature and black hole feedback, in agreement with the expectations from the EAGLE cosmological numerical simulation.
Discovery of a nearby 1700 km s−1 star ejected from the Milky Way by Sgr A*
Authors: Koposov Sergey E , Boubert Douglas , Li Ting S , Erkal Denis , Da Costa Gary S , Zucker Daniel B , Ji Alexander P , Kuehn Kyler , Lewis Geraint F , Mackey Dougal , Simpson Jeffrey D , Shipp Nora , Wan Zhen , Belokurov Vasily , Bland-Hawthorn Joss , Martell Sarah L , Nordlander Thomas , Pace Andrew B , De Silva Gayandhi M , Wang Mei-Yu ,   (S5 collaboration)
Published: November 2019

ABSTRACT
We present the serendipitous discovery of the fastest main-sequence hyper-velocity star (HVS) by the Southern Stellar Stream Spectroscopic Survey (S5). The star S5-HVS1 is a ∼2.35 M⊙ A-type star located at a distance of ∼9 kpc from the Sun and has a heliocentric radial velocity of 1017 ± 2.7 $\mathrm{\, km\, s^{-1}}$ without any signature of velocity variability. The current 3D velocity of the star in the Galactic frame is 1755 ± 50 $\mathrm{\, km\, s^{-1}}$. When integrated backwards in time, the orbit of the star points unambiguously to the Galactic Centre, implying that S5-HVS1 was kicked away from Sgr A* with a velocity of ∼1800 $\mathrm{\, km\, s^{-1}}$ and travelled for 4.8 Myr to its current location. This is so far the only HVS confidently associated with the Galactic Centre. S5-HVS1 is also the first hyper-velocity star to provide constraints on the geometry and kinematics of the Galaxy, such as the Solar motion Vy,⊙ = 246.1 ± 5.3 $\mathrm{\, km\, s^{-1}}$ or position R0 = 8.12 ± 0.23 kpc. The ejection trajectory and transit time of S5-HVS1 coincide with the orbital plane and age of the annular disc of young stars at the Galactic Centre, and thus may be linked to its formation. With the S5-HVS1 ejection velocity being almost twice the velocity of other hyper-velocity stars previously associated with the Galactic Centre, we question whether they have been generated by the same mechanism or whether the ejection velocity distribution has been constant over time.
Multiwavelength cluster mass estimates and machine learning
Authors: Cohn J D , Battaglia Nicholas 
Published: November 2019

ABSTRACT
One emerging application of machine learning methods is the inference of galaxy cluster masses. In this note, machine learning is used to directly combine five simulated multiwavelength measurements in order to find cluster masses. This is in contrast to finding mass estimates for each observable, normally by using a scaling relation, and then combining these scaling law based mass estimates using a likelihood. We also illustrate how the contributions of each observable to the accuracy of the resulting mass measurement can be compared via model-agnostic Importance Permutation values. Thirdly, as machine learning relies upon the accuracy of the training set in capturing observables, their correlations, and the observational selection function, and as the machine learning training set originates from simulations, two tests of whether a simulation’s correlations are consistent with observations are suggested and explored as well.
Modelling strains and stresses in continuously stratified rotating neutron stars
Authors: Giliberti E , Cambiotti G , Antonelli M , Pizzochero P M 
Published: November 2019

Abstract
We introduce a Newtonian model for the deformations of a compressible, auto-gravitating and continuously stratified neutron star. The present framework can be applied to a number of astrophysical scenarios as it allows to account for a great variety of loading forces. In this first analysis, the model is used to study the impact of a frozen adiabatic index in the estimate of rotation-induced deformations: we assume a polytropic equation of state for the matter at equilibrium but, since chemical reactions may be slow, the perturbations with respect to the unstressed configuration are modeled by using a different adiabatic index. We quantify the impact of a departure of the adiabatic index from its equilibrium value on the stressed stellar configuration and we find that a small perturbation can cause large variations both in displacements and strains. As a first practical application, we estimate the strain developed between two large glitches in the Vela pulsar showing that, starting from an initial unstressed configuration, it is not possible to reach the breaking threshold of the crust, namely to trigger a starquake. In this sense, the hypothesis that starquakes could trigger the unpinning of superfluid vortices is challenged and, for the quake to be a possible trigger, the solid crust must never fully relax after a glitch, making the sequence of starquakes in a neutron star an history-dependent process.