bluuebunny/crossref_metadata_2025_split huggingface dataset:
Article 22
Authors: Boerefijn Ineke , Fraser Julie 
Published: November 2022

Abstract
This chapter highlights Article 22 of the Convention on the Elimination of All Forms of Discrimination against Women (CEDAW). The CEDAW Committee’s practice under Article 22 has developed significantly over the years. While the text refers exclusively to specialized agencies, the Committee’s current practice is to invite other UN entities to submit reports, as well as other non-UN entities. In the early years, the Committee did not ask the specialized agencies to submit country-specific information to be used in the consideration of States parties’ reports as some members believed this was beyond the Committee’s mandate. Gradually, it allowed a larger role for these agencies in the reporting procedure, and it welcomes country-specific information as well as input at the pre-session working group. This latter input is extremely useful to inform the written questions the Committee asks States parties to answer before the constructive dialogue. Moreover, it considers the specialized agencies to be valuable partners in assisting States parties in implementing the Convention at the domestic level. In recent years, there has been increased cooperation on the ground between UN entities, encouraged also by the now permanent presence of UN Women within the human rights framework in Geneva.
Article 27
Authors: Kroworsch Susann 
Published: November 2022

Abstract
This chapter details Article 27 of the Convention on the Elimination of All Forms of Discrimination against Women (CEDAW). In accordance with Article 27(1), the Convention entered into force on 3 September 1981, the thirtieth day after the deposit of the twentieth instrument of accession by St Vincent and the Grenadines. Paragraph 1 repeats that the UN Secretary-General (UN SG) acts as a depositary; the depositary provides the information that establishes when the treaty enters into force. Article 27(1) stipulates that thirty days must elapse between the date on which the required number of instruments is deposited and the date of entry into force. This period is required to ensure that preconditions are met and gives the depositary time to notify contracting States of the pending entry into force. The drafters’ compromise of twenty instruments of ratification or accession as condition for the Convention’s entry into force became a model for subsequent UN human rights treaties.
Article 28
Authors: Connors Jane 
Published: November 2022

Abstract
This chapter focuses on Article 28 of the Convention on the Elimination of All Forms of Discrimination against Women (CEDAW). Article 28 explicitly envisages that States ratifying or acceding to the Convention may do so with reservations, indicating that these shall be received by the Secretary-General and circulated to all States. Article 28(3) indicates that reservations may be withdrawn at any time through notification to the Secretary-General, with the withdrawal taking effect on the date on which that notification is received. Meanwhile, Article 28(2) mirrors Article 19(c) of the 1969 Vienna Convention of the Law of Treaties (VCLT), prohibiting reservations that are incompatible with the Convention’s object and purpose. There are no provisions in the Convention described as non-derogable, nor is there any provision which identifies articles which may not be subject to reservation. However, the CEDAW Committee has identified Article as a core provision with which reservations cannot be reconciled. In the state reporting procedure and its concluding observations, the Committee urges States parties to work towards withdrawing its reservations, especially when States parties have not entered reservations to comparable provisions in other human rights treaties.
The Scope of Application of the Three Additional Protocols
Authors: Bellal Annyssa , Casey-Maslen Stuart 
Published: November 2022

Abstract
This chapter discusses the scope and limitations of the application of the two Additional Protocols of 1977 and the Third Additional Protocol of 2005. It explains that some provisions must be implemented amidst peacetime, while other provisions are limited to armed conflict situations. Additional Protocol I focused on international armed conflict, while a particular form of non-international armed conflict had been addressed by the conditions of Additional Protocol II. Meanwhile, the Third Additional Protocol became effective in all situations falling within the scope of the aforementioned Protocols. The chapter also looks into the geographical and temporal scope of application within the sovereign territory.
Precautions in Attack and Defence
Authors: Bellal Annyssa , Casey-Maslen Stuart 
Published: November 2022

Abstract
This chapter tackles the requirement imposed upon attackers and defenders when taking feasible precautions to protect civilians. It also acknowledges how the requirement coincided with the principles of distinction and proportionality in the attack. The notion of precautionary measures aims to minimise civilian harm by ensuring that few if any civilians are present amidst an attack strike and limiting the ambient effects of an attack to a military objective. According to the International Committee of the Red Cross (ICRC), the provisions were the subject of protracted and difficult negotiations in the diplomatic conference that adopted the Protocol. Moreover, the UN Secretary-General called on all parties to the conflict to refrain from using explosive weapons with wide-area effects in populated areas, as discussions still continue concerning the use of explosive weapons in populated areas (EWIPA).
Prohibited Weapons
Authors: Bellal Annyssa , Casey-Maslen Stuart 
Published: November 2022

Abstract
This chapter looks into the treatment of weapons under the two Additional Protocols of 1977. It defines a weapon in accordance with international law. The right of parties to use weapons is not unlimited due to applicable treaties and customary rules restricting armed conflict parties. Additionally, the use of lawful weapons must comply with the rules of distinction and proportionality in attacks, while inherently indiscriminate weapons like biological and nuclear weapons and other things that cause unnecessary suffering should never be used. The 1977 Additional Protocol I stipulated the prohibition of weapons causing widespread, severe, and long-term damage to the environment. The chapter then clarifies how cyber operations are not inherently indiscriminate. It also highlights the importance of verifying the legality of weapons.
Reprisals
Authors: Bellal Annyssa , Casey-Maslen Stuart 
Published: November 2022

Abstract
This chapter looks into reprisals, which had been the primary means of enforcing respect for the laws of war despite being inherently barbaric and unjust for the victims. It starts with the international humanitarian law (IHL) outlawing reprisals, but a comprehensive prohibition has not been incorporated in treaty law or custom law. However, the International Committee of the Red Cross (ICRC) insisted that reprisals remain lawfully subjected to stringent conditions. The chapter then explicates the interpretation and application of the rules governing reprisals within the Geneva Conventions, 1977 Additional Protocols, rules of customary law, international criminal law, and the Rome Statute of the International Criminal Court. It covers the concept of a belligerent reprisal and its conditions for lawful exercise under general international law.
Tremellomycetes isolated from organs of Columba livia
Authors: Bermann Carolina dos Santos , Braga Caroline Quintana , Silveira Júlia de Souza , Milech Angelita , dos Santos Carolina Caetano , Ianiski Lara Baccarin , Maciel Aline Fontanella , Brod Augusto Duarte , Weiblen Carla , Botton Sônia de Avila , Pereira Daniela Isabel Brayer 
Published: November 2022

Abstract
Brain, lungs, and intestines of Columba livia captured in Brazil were analyzed for research on Tremellomycetes. Mycological culture presented the growth of colonies suggestive of Cryptococcus spp. in 11.60% (13/112) of the samples. Microscopy revealed capsulated yeast cells. Molecular analysis evidenced Papiliotrema flavescens, Naganishia diffluens, Filobasidium magnum, and Naganishia randhawae. Thermotolerance of Tremellomycetes isolates from brain and lung (n = 10) evidenced cell growth and viability at 37 °C. At 42 °C/24 h, these isolates showed viability, except for one P. flavescens isolate. Here, we report the first isolation of Tremellomycetes species from the brain and lungs of a healthy C. livia.
Making hot Jupiters in stellar clusters: The importance of binary exchange
Authors: Li Daohai , Mustill Alexander J , Davies Melvyn B , Gong Yan-Xiang 
Published: November 2022

ABSTRACT
It has been suggested that the occurrence rate of hot Jupiters (HJs) in open clusters might reach several per cent, significantly higher than that of the field (∼a per cent). In a stellar cluster, when a planetary system scatters with a stellar binary, it may acquire a companion star, which may excite large-amplitude von Zeipel–Lidov–Kozai oscillations in the planet’s orbital eccentricity, triggering high-eccentricity migration, and the formation of an HJ. We quantify the efficiency of this mechanism by modelling the evolution of a gas giant around a solar mass star under the influence of successive scatterings with binary and single stars. We show that the chance that a planet ∈ (1, 10) au becomes an HJ in a Gyr in a cluster of stellar density n* = 50 pc−3, and binary fraction fbin = 0.5 is about 2 per cent and an additional 4 per cent are forced by the companion star into collision with or tidal disruption by the central host. An empirical fit shows that the total percentage of those outcomes asymptotically reaches an upper limit determined solely by fbin (e.g. 10 per cent at fbin = 0.3 and 18 per cent at fbin = 1) on a time-scale inversely proportional to n* (∼Gyr for n* ∼ 100 pc−3). The ratio of collisions to tidal disruptions is roughly a few, and depends on the tidal model. Therefore, if the giant planet occurrence rate is 10 per cent, our mechanism implies an HJ occurrence rate of a few times 0.1 per cent in a Gyr and can thus explain a substantial fraction of the observed rate.
Radial profiles of surface density in debris discs
Authors: Rafikov Roman R 
Published: November 2022

ABSTRACT
Resolved observations of debris discs can be used to derive radial profiles of azimuthally averaged surface density (ASD), which carries important information about the disc structure even in the presence of non-axisymmetric features and has improved signal-to-noise characteristics relative to the two-dimensional surface brightness measurements. We develop a (semi-)analytical formalism allowing one to relate ASD to the underlying semimajor axis and eccentricity distributions of the debris particles in a straightforward manner. This approach does not involve the distribution of particle apsidal angles, thus simplifying calculations. It is a much faster, more flexible and effective way of calculating ASD than the Monte Carlo sampling of orbital parameters of debris particles. We present explicit analytical results based on this technique for a number of particle eccentricity distributions, including two cases of particular practical importance: a prescribed radial profile of eccentricity, and the Rayleigh distribution of eccentricities. We then show how our framework can be applied to observations of debris discs and rings for retrieving either the semimajor axis distribution or (in some cases) the eccentricity distribution of debris, thus providing direct information about the architecture and dynamical processes operating in debris discs. Our approach also provides a fast and efficient way of forward modelling observations. Applications of this technique to other astrophysical systems, e.g. the nuclear stellar disc in M31 or tenuous planetary rings, are also discussed.
Bright X-ray pulsars: how outflows influence beaming, pulsations and pulse phase lags
Authors: Mushtukov Alexander A , Portegies Zwart Simon 
Published: November 2022

ABSTRACT
Extreme accretion in X-ray pulsars (XRPs) results in radiation-driven outflows launched from the inner parts of the accretion disc. The outflows affect the apparent luminosity of the XRPs and their pulsations through the geometrical beaming. We model processes of geometrical beaming and pulse formation using Monte Carlo simulations. We confirm our earlier statement that strong amplification of luminosity due to the collimation of X-ray photons is inconsistent with a large pulsed fraction. Accounting for relativistic aberration due to possibly high outflow velocity (∼0.2c) does not affect this conclusion. We demonstrate that the beaming causes phase lags of pulsations. Within the opening angle of the accretion cavity formed by the outflows, phase lags tend to be sensitive to observers viewing angles. Variations in outflow geometry and corresponding changes of the phase lags might influence the detectability of pulsation in bright X-ray pulsars and ULXs. We speculate that the strong geometrical beaming is associated with large radiation pressure on the walls of accretion cavity due to multiple photons reflections. We expect that the mass-loss rate limits geometrical beaming: strong beaming becomes possible only under sufficiently large fractional mass-loss rate from the disc.
GOGREEN: A critical assessment of environmental trends in cosmological hydrodynamical simulations at z ≈ 1
Authors: Kukstas Egidijus , Balogh Michael L , McCarthy Ian G , Bahé Yannick M , De Lucia Gabriella , Jablonka Pascale , Vulcani Benedetta , Baxter Devontae C , Biviano Andrea , Cerulo Pierluigi , Chan Jeffrey C , Cooper M C , Demarco Ricardo , Finoguenov Alexis , Font Andreea S , Lidman Chris , Marchioni Justin , McGee Sean , Muzzin Adam , Nantais Julie , Old Lyndsay , Pintos-Castro Irene , Poggianti Bianca , Reeves Andrew M M , Rudnick Gregory , Sarron Florian , van der Burg Remco , Webb Kristi , Wilson Gillian , Yee Howard K C , Zaritsky Dennis 
Published: November 2022

ABSTRACT
Recent observations have shown that the environmental quenching of galaxies at z ∼ 1 is qualitatively different to that in the local Universe. However, the physical origin of these differences has not yet been elucidated. In addition, while low-redshift comparisons between observed environmental trends and the predictions of cosmological hydrodynamical simulations are now routine, there have been relatively few comparisons at higher redshifts to date. Here we confront three state-of-the-art suites of simulations (BAHAMAS+MACSIS, EAGLE+Hydrangea, IllustrisTNG) with state-of-the-art observations of the field and cluster environments from the COSMOS/UltraVISTA and GOGREEN surveys, respectively, at z ∼ 1 to assess the realism of the simulations and gain insight into the evolution of environmental quenching. We show that while the simulations generally reproduce the stellar content and the stellar mass functions of quiescent and star-forming galaxies in the field, all the simulations struggle to capture the observed quenching of satellites in the cluster environment, in that they are overly efficient at quenching low-mass satellites. Furthermore, two of the suites do not sufficiently quench the highest mass galaxies in clusters, perhaps a result of insufficient feedback from AGN. The origin of the discrepancy at low stellar masses ($M_* \lesssim 10^{10}$ M⊙), which is present in all the simulations in spite of large differences in resolution, feedback implementations, and hydrodynamical solvers, is unclear. The next generation of simulations, which will push to significantly higher resolution and also include explicit modelling of the cold interstellar medium, may help us to shed light on the low-mass tension.
Galaxy And Mass Assembly (GAMA): the dependence of star formation on surface brightness in low-redshift galaxies
Authors: Phillipps S , Bellstedt S , Bremer M N , De Propris R , James P A , Casura S , Liske J , Holwerda B W 
Published: November 2022

ABSTRACT
The star-formation rate in galaxies is well known to correlate with stellar mass (the ‘star-forming main sequence’). Here, we extend this further to explore any additional dependence on galaxy surface brightness, a proxy for stellar mass surface density. We use a large sample of low-redshift (z ≤ 0.08) galaxies from the Galaxy And Mass Assembly survey which have both spectral energy distribution (SED) derived star-formation rates and photometric bulge-disc decompositions, the latter providing measures of disc surface brightness and disc masses. Using two samples, one of galaxies fitted by a single component with Sérsic index below 2 and one of the discs from two-component fits, we find that once the overall mass dependence of star-formation rate is accounted for, there is no evidence in either sample for a further dependence on stellar surface density.
Differences in chemical evolution between isolated and embedded prestellar cores
Authors: Priestley F D , Whitworth A P , Fogerty E 
Published: November 2022

ABSTRACT
Models of prestellar cores often assume that the cores are isolated from their environment – material outside the core boundary plays no role in the subsequent evolution. This is unlikely to be the case in reality, where cores are located within hierarchically substructured molecular clouds. We investigate the dynamical and chemical evolution of prestellar cores, modelled as Bonnor–Ebert spheres, and show that the density of the ambient medium has a large impact on the resulting chemical properties of the cores. Models embedded in high-density, low-temperature surroundings have greatly enhanced abundances of several molecules, such as CO and CS, compared to models with more diffuse surroundings, corresponding to relatively isolated cores. The predicted intensities and profile shapes of molecular lines are also affected. The density of the ambient medium has a stronger effect on the chemical evolution than whether the cores are initially in or out of equilibrium. This suggests that the impact of environment cannot be neglected when modelling chemistry in prestellar cores; the results of these models are highly sensitive to the assumptions made about the core surroundings.
The FRB 20121102A November rain in 2018 observed with the Arecibo Telescope
Authors: Jahns J N , Spitler L G , Nimmo K , Hewitt D M , Snelders M P , Seymour A , Hessels J W T , Gourdji K , Michilli D , Hilmarsson G H 
Published: November 2022

ABSTRACT
We present 849 new bursts from FRB 20121102A detected with the 305-m Arecibo Telescope. Observations were conducted as part of our regular campaign to monitor activity and evolution of burst properties. The 10 reported observations were carried out between 1150 and $1730\, {\rm MHz}$ and fall in the active period around 2018 November. All bursts were dedispersed at the same dispersion measure and are consistent with a single value of $(562.4 \pm 0.1)\, {\rm pc\, cm^{-3}}$. The rate varies between 0 bursts and 218 ± 16 bursts per hour, the highest rate observed to date. The times between consecutive bursts show a bimodal distribution. We find that a Poisson process with varying rate best describes arrival times with separations ${\gt}{0.1\, {\rm s}}$. Clustering on time-scales of $22\, {\rm ms}$ reflects a characteristic time-scale of the source and possibly the emission mechanism. We analyse the spectro-temporal structure of the bursts by fitting 2D Gaussians with a temporal drift to each sub-burst in the dynamic spectra. We find a linear relationship between the sub-burst’s drift and its duration. At the same time, the drifts are consistent with coming from the sad-trombone effect. This has not been predicted by current models. The energy distribution shows an excess of high-energy bursts and is insufficiently modelled by a single power law even within single observations. We find long-term changes in the energy distribution, the average spectrum, and the sad-trombone drift, compared to earlier and later published observations. Despite the large burst rate, we find no strict short-term periodicity.
Mesh-free hydrodynamics in pkdgrav3 for galaxy formation simulations
Authors: Alonso Asensio Isaac , Dalla Vecchia Claudio , Potter Douglas , Stadel Joachim 
Published: November 2022

ABSTRACT
We extend the state-of-the-art N-body code pkdgrav3 with the inclusion of mesh-free gas hydrodynamics for cosmological simulations. Two new hydrodynamic solvers have been implemented, the mesh-less finite volume and mesh-less finite mass methods. The solvers manifestly conserve mass, momentum, and energy, and have been validated with a wide range of standard test simulations, including cosmological simulations. We also describe improvements to pkdgrav3 that have been implemented for performing hydrodynamic simulations. These changes have been made with efficiency and modularity in mind, and provide a solid base for the implementation of the required modules for galaxy formation and evolution physics and future porting to GPUs. The code is released in a public repository, together with the documentation, and all the test simulations presented in this work.
Massive quiescent galaxies at z ∼ 3: A comparison of selection, stellar population, and structural properties with simulation predictions
Authors: Lustig Peter , Strazzullo Veronica , Remus Rhea-Silvia , D’Eugenio Chiara , Daddi Emanuele , Burkert Andreas , De Lucia Gabriella , Delvecchio Ivan , Dolag Klaus , Fontanot Fabio , Gobat Raphael , Mohr Joseph J , Onodera Masato , Pannella Maurilio , Pillepich Annalisa 
Published: November 2022

ABSTRACT
We study stellar population and structural properties of massive log (M⋆/M⊙) &gt; 11 galaxies at z ≈ 2.7 in the Magneticum and IllustrisTNG hydrodynamical simulations and GAEA semi-analytic model. We find stellar mass functions broadly consistent with observations, with no scarcity of massive, quiescent galaxies at z ≈ 2.7, but with a higher quiescent galaxy fraction at high masses in IllustrisTNG. Average ages of simulated quiescent galaxies are between ≈0.8 and ${1.0\, \textrm {Gyr}}$, older by a factor ≈2 than observed in spectroscopically confirmed quiescent galaxies at similar redshift. Besides being potentially indicative of limitations of simulations in reproducing observed star formation histories, this discrepancy may also reflect limitations in the estimation of observed ages. We investigate the purity of simulated UVJ rest-frame colour-selected massive quiescent samples with photometric uncertainties typical of deep surveys (e.g. COSMOS). We find evidence for significant contamination (up to ${60\, \rm {per\, cent}}$) by dusty star-forming galaxies in the UVJ region that is typically populated by older quiescent sources. Furthermore, the completeness of UVJ-selected quiescent samples at this redshift may be reduced by $\approx {30\, \rm {per\, cent}}$ due to a high fraction of young quiescent galaxies not entering the UVJ quiescent region. Massive, quiescent galaxies in simulations have on average lower angular momenta and higher projected axis ratios and concentrations than star-forming counterparts. Average sizes of simulated quiescent galaxies are broadly consistent with observations within the uncertainties. The average size ratio of quiescent and star-forming galaxies in the probed mass range is formally consistent with observations, although this result is partly affected by poor statistics.