bluuebunny/crossref_metadata_2025_split huggingface dataset:
Incorporating the sustainable development goals in small- to medium-sized enterprises
Authors: Nygaard Sofie , Kokholm Alberte R , Huulgaard Rikke D 
Published: October 2022

Abstract
Multiple international stakeholders emphasise the important role of small- to medium-sized enterprises (SMEs) in achieving the sustainable development goals (SDG). SMEs make up more than 99% of companies in Europe, and holds a potential to promote social and environmental responsibility. However, there is no ‘one size fits all’ when it comes to the incorporation of the SDGs. In this study; we identify five main approaches based on a literature review including (i) rainbow washing, (ii) supporting ‘business as usual’, (iii) adding new initiatives/strategies, (iv) philanthropy and (v) strategic use in core businesses. These approaches are categorised based on their contribution to achieving the SDGs as well as the benefits for the company in question. We performed a case study of six SMEs in Northern Jutland, Denmark, which revealed, that most SMEs work with the SDGs in less proactive and ambitious ways, leaving a gap between the role they have been assigned and their current practices. To investigate this gap further, our case study combined with the literature review has helped identify factors influencing the SMEs choice of approach. These include both negative (uncertainty about the SDGs prospective role, lack of resources and low demand for SDG compliance) and positive (taking responsibility, social license to operate, communication and inspiration) factors. The negative influencing factors are particularly interlinked which is caused by inadequacy in resources, knowledge and qualifications. This indicates that SMEs cannot single-handedly implement the SDGs in a way that enables achievement of the 2030 Agenda, thus external guidance is needed.
ΛCDM halo substructure properties revealed with high-resolution and large-volume cosmological simulations
Authors: Moliné Ángeles , Sánchez-Conde Miguel A , Aguirre-Santaella Alejandra , Ishiyama Tomoaki , Prada Francisco , Cora Sofía A , Croton Darren , Jullo Eric , Metcalf R Benton , Oogi Taira , Ruedas José 
Published: October 2022

ABSTRACT
In this work, we investigate the structural properties, distribution and abundance of ΛCDM dark matter subhaloes using the Phi-4096 and Uchuu suite of N-body cosmological simulations. Thanks to the combination of their large volume, high mass resolution and superb statistics, we are able to quantify – for the first time consistently over more than seven decades in ratio of subhalo-to-host-halo mass – dependencies of subhalo properties on mass, maximum circular velocity, Vmax, host halo mass, and distance to host halo centre. We also dissect the evolution of these dependencies over cosmic time. We provide accurate fits for the subhalo mass and velocity functions, both exhibiting decreasing power-law slopes and with no significant dependence on redshift. We also find subhalo abundance to depend weakly on host halo mass. Subhalo structural properties are codified via a concentration parameter, cV, that does not depend on any pre-defined density profile and relies only on Vmax. We derive the cV−Vmax relation and find an important dependence on distance of the subhalo to the host halo centre. Interestingly, we also find subhaloes of the same mass to be significantly more concentrated when they reside inside more massive hosts. Finally, we investigate the redshift evolution of cV, and provide accurate fits. Our results offer an unprecedented detailed characterization of the subhalo population, consistent over a wide range of subhalo and host halo masses, as well as cosmic times. Thus, we expect our work to be particularly useful for any future research involving dark matter halo substructure.
H i intensity mapping with MeerKAT: power spectrum detection in cross-correlation with WiggleZ galaxies
Authors: Cunnington Steven , Li Yichao , Santos Mario G , Wang Jingying , Carucci Isabella P , Irfan Melis O , Pourtsidou Alkistis , Spinelli Marta , Wolz Laura , Soares Paula S , Blake Chris , Bull Philip , Engelbrecht Brandon , Fonseca José , Grainge Keith , Ma Yin-Zhe 
Published: October 2022

ABSTRACT
We present a detection of correlated clustering between MeerKAT radio intensity maps and galaxies from the WiggleZ Dark Energy Survey. We find a 7.7σ detection of the cross-correlation power spectrum, the amplitude of which is proportional to the product of the ${\rm H}\, {\small I}$ density fraction ($\Omega _{{\rm H}\, {\small I}}$), ${\rm H}\, {\small I}$ bias ($b_{{\rm H}\, {\small I}}$), and the cross-correlation coefficient (r). We therefore obtain the constraint $\Omega _{{\rm H}\, {\small I}}b_{{\rm H}\, {\small I}}r\, {=}\, [0.86\, {\pm }\, 0.10\, ({\rm stat})\, {\pm }\, 0.12\, ({\rm sys})]\, {\times }\, 10^{-3}$, at an effective scale of $k_{\rm eff}\ {\sim }\ 0.13\, h\, \text{Mpc}^{-1}$. The intensity maps were obtained from a pilot survey with the MeerKAT telescope, a 64-dish pathfinder array to the SKA Observatory (SKAO). The data were collected from 10.5 h of observations using MeerKAT’s L-band receivers over six nights covering the 11 h field of WiggleZ, in the frequency range 1015–973 MHz (0.400 $\, {\lt }\, z\, {\lt }\,$ 0.459 in redshift). This detection is the first practical demonstration of the multidish autocorrelation intensity mapping technique for cosmology. This marks an important milestone in the roadmap for the cosmology science case with the full SKAO.
Angular momentum loss rates in Be stars determined by the viscous decretion disc model
Authors: Ghoreyshi M R , Jones C E , Granada A 
Published: October 2022

ABSTRACT
Circumstellar discs around Be stars are formed by the material ejected by the central star. This process removes excess angular momentum from the star as viscosity facilitates the mass and angular momentum transfer within the disc and its growth. The angular momentum loss rates (AMLR) of Be stars is a subject of debate in the literature. Through the modelling of the disc formation and dissipation phases observed from Be stars, their average AMLR can be determined and this is the goal of this work. We use the viscous decretion disc (VDD) model to provide a range of the average AMLR for Be stars and compare these rates with predicted values from the literature. We explore the reasons for discrepancies between the predicted values of average AMLR, using the VDD and Geneva stellar evolution models that were previously reported in literature and find that the largest differences occur when Be stars are rotating below their critical speeds. We show that the time over which the mass reservoir builds up is inversely proportional to the average AMLR. Also, we determine a revised value of the average AMLR for the Galactic Be star ω CMa of $4.7\times 10^{36}\, \mathrm{g\, cm^2\, s^{-2}}$, which is in better agreement with the values expected for a typical B2-type star. Finally, the effect of disc truncation due to the presence of a companion star is investigated and we find that this has a minimal effect on the average AMLR.
Analysis of the ionized interstellar medium and orbital dynamics of PSR J1909-3744 using scintillation arcs
Authors: Askew J , Reardon D J , Shannon R M 
Published: October 2022

ABSTRACT
Long-term studies of binary millisecond pulsars (MSPs) provide precise tests of strong-field gravity, and can be used to measure neutron-star masses. PSR J1909-3744, a binary MSP has been the subject of several pulsar timing analyses. The edge-on orbit enables measurement of its mass using the Shapiro delay; however, there is degeneracy in the sense of the inclination angle, i, and multiple solutions for the longitude of ascending node, Ω. Radio pulsars scintillate due to inhomogeneities in the ionized interstellar medium (IISM). This can result in scintillation arcs in the power spectrum of the dynamic spectrum that can use these to study the interstellar medium and constrain binary pulsar orbits. Here, we study the scintillation of PSR J1909-3744 using observations from the 64-m Parkes Radio Telescope (Murriyang) over ≈13 yr, using techniques to study scintillation in a lower signal-to-noise regime. By monitoring annual and orbital variations of the arc-curvature measurements, we are able to characterize the velocity of the IISM. We find that the statistics of the IISM remained stationary over this time and a slightly anisotropic model (axial ratio ≳1.2) is preferred. We measure the relative distance to a single dominant thin scattering screen at s = 0.49 ± 0.04, or Ds = 590 ± 50 pc, with an angle of anisotropy ζ = 85 ± 6° (East of North) and velocity in the direction of anisotropy VIISM,ζ = 14 ± 10 km s−1. By combining a physical model of the IISM and current pulsar timing results, we also constrain Ω = 225 ± 3° and i = 86.46 ± 0.05°.
The structure and 3D kinematics of vela OB2
Authors: Armstrong Joseph J , Wright Nicholas J , Jeffries R D , Jackson R J , Cantat-Gaudin Tristan 
Published: October 2022

ABSTRACT
The kinematics of stars in OB associations can provide insights into their formation, dynamical evolution, and eventual fate. The low-mass stellar content of OB associations are sufficiently numerous as to provide a detailed sampling of their kinematic properties, however spectroscopy is required to confirm the youth of individual stars and to get 3D kinematics. In this paper, we present and analyse results from a large spectroscopic survey of Vela OB2 conducted using 2dF/HERMES on the AAT. This spectroscopy is used to confirm the youth of candidate young stars and determine radial velocities, which are combined with proper motions and parallaxes from Gaia to measure 3D positions and velocities. We identify multiple separate kinematic groups in the region, for which we measure velocity dispersions and infer their virial states. We measure expansion rates for all these groups and find strong evidence for anisotropic expansion in the Vela OB2 association of at least 11σ significance in all three dimensions, as well as some evidence for expansion in the γ Vel and P Puppis clusters. We trace back the motions of these groups into the past and find that the open cluster NGC 2547 is an interloper in the Vela OB2 region and actually formed &gt;100 pc away from the association. We conclude that Vela OB2 must have formed with considerable spatial and kinematic substructure over a time-scale of ∼10 Myr, with clear temporal substructure within the association, but no clear evidence for an age gradient.
The plasma suppression effect can be ignored in realistic FRB models invoking bunched coherent radio emission
Authors: Qu Yuanhong , Zhang Bing , Kumar Pawan 
Published: October 2022

ABSTRACT
One widely discussed mechanism to produce highly coherent radio emission of fast radio bursts (FRBs) is coherent emission by bunches, either via curvature radiation or inverse Compton scattering (ICS). It has been suggested that the plasma oscillation effect can significantly suppress coherent emission power by bunches. We examine this criticism in this paper. The suppression factor formalism was derived within the context of radio pulsars in which radio waves are in the low-amplitude, linear regime and cannot directly be applied to the large-amplitude, non-linear regime relevant for FRBs. Even if one applies this linear treatment, plasma suppression is not important for two physical reasons. First, for an efficient radiation mechanism, such as ICS, the required plasma density is not high so that a high-density plasma may not exist. Secondly, both bunched coherent mechanisms demand that a large global parallel electric field (E∥) must exist in the emission region in order to continuously inject energy to the bunches to power an FRB. In order to produce typical FRB duration via coherent curvature or ICS radiation, a parallel electric field must be present to balance the acceleration and radiation back reaction. The plasma suppression factor should be modified with the existence of E∥. We show that the correction factor for curvature radiation, fcur, increases with E∥ and becomes 1 when E∥ reaches the radiation-reaction-limited regime. We conclude that the plasma suppression effect can be ignored for realistic FRB emission models invoking bunched coherent radio emission.
A Bayesian Monte Carlo assessment of orbital stability in the late stages of planetary system formation
Authors: Salas Jassyr , Bautista Frank , Chaparro Germán 
Published: October 2022

ABSTRACT
The final orbital configuration of a planetary system is shaped by both its early star–disc environment and late-stage gravitational interactions. Assessing the relative importance of each of these factors is not straightforward due to the observed diversity of planetary systems compounded by observational biases. Our goal is to understand how a planetary system may change when planetesimal accretion and planet migrations stop and secular gravitational effects take over. Our approach starts with a novel classification of planetary systems based on their orbital architecture, validated using Approximate Bayesian Computation methods. We apply this scheme to observed planetary systems and also to ∼400 synthetic systems hosting ∼5000 planets, synthesized from a Monte Carlo planet population model. Our classification scheme robustly yields four system classes according to their planet masses and semimajor axes, for both observed and synthetic systems. We then estimate the orbital distribution density of each of the synthetic systems before and after dynamically evolving for 0.1–1 Myr using a gravitational + collisional N-body code. Using the Kullback–Leibler divergence to statistically measure orbital configuration changes, we find that ≲10 per cent of synthetic planetary systems experience such changes. We also find that this fraction belongs to a class of systems for which their centre of mass is very close to their host star. Although changes in the orbital configuration of planetary systems may not be very common, they are more likely to happen in systems with close-in, massive planets, with F- and G-type host-stars and stellar metallicities [Fe/H] &gt;0.2.
Dust formation in the outflows of catastrophically evaporating planets
Authors: Booth Richard A , Owen James E , Schulik Matthäus 
Published: October 2022

ABSTRACTUltrashort period planets offer a window into the poorly understood interior composition of exoplanets through material evaporated from their rocky interiors. Among these objects are a class of disintegrating planets, observed when their dusty tails transit in front of their host stars. These dusty tails are thought to originate from dust condensation in thermally driven winds emanating from the sublimating surfaces of these planets. Existing models of these winds have been unable to explain their highly variable nature and have not explicitly modelled how dust forms in the wind. Here, we present new radiation-hydrodynamic simulations of the winds from these planets, including a minimal model for the formation and destruction of dust, assuming that nucleation can readily take place. We find that dust forms readily in the winds, a consequence of large dust grains obtaining lower temperatures than the planet’s surface. As hyphothesized previously, we find that the coupling of the planet’s surface temperature to the outflow properties via the dust’s opacity can drive time-variable flows when dust condensation is sufficiently fast. In agreement with previous work, our models suggest that these dusty tails are a signature of catastrophically evaporating planets that are close to the end of their lives. Finally, we discuss the implications of our results for the dust’s composition. More detailed hydrodynamic models that self-consistently compute the nucleation and composition of the dust and gas are warranted in order to use these models to study the planet’s interior composition.
Radio observations of the tidal disruption event AT2020opy: a luminous non-relativistic outflow encountering a dense circumnuclear medium
Authors: Goodwin A J , Miller-Jones J C A , van Velzen S , Bietenholz M , Greenland J , Cenko B , Gezari S , Horesh A , Sivakoff G R , Yan L , Yu W , Zhang X 
Published: October 2022

ABSTRACT
Tidal disruption events (TDEs) occur when a star passes too close to a supermassive black hole and is destroyed by tidal gravitational forces. Radio observations of TDEs trace synchrotron emission from outflowing material that may be ejected from the inner regions of the accretion flow around the supermassive black hole or by the tidal debris stream. Radio detections of TDEs are rare, but provide crucial information about the launching of jets and outflows from supermassive black holes and the circumnuclear environment in galaxies. Here, we present the radio detection of the TDE AT2020opy, including three epochs of radio observations taken with the Karl G. Jansky Very Large Array, MeerKAT, and upgraded Giant Metrewave Radio telescope. AT2020opy is the most distant thermal TDE with radio emission reported to date, and from modelling the evolving synchrotron spectra we deduce that the host galaxy has a more dense circumnuclear medium than other thermal TDEs detected in the radio band. Based on an equipartition analysis of the synchrotron spectral properties of the event, we conclude that the radio-emitting outflow was likely launched approximately at the time of, or just after, the initial optical flare. We find no evidence for relativistic motion of the outflow. The high luminosity of this event supports that a dense circumnuclear medium of the host galaxy produces brighter radio emission that rises to a peak more quickly than in galaxies with lower central densities.
A Sun-like star orbiting a black hole
Authors: El-Badry Kareem , Rix Hans-Walter , Quataert Eliot , Howard Andrew W , Isaacson Howard , Fuller Jim , Hawkins Keith , Breivik Katelyn , Wong Kaze W K , Rodriguez Antonio C , Conroy Charlie , Shahaf Sahar , Mazeh Tsevi , Arenou Frédéric , Burdge Kevin B , Bashi Dolev , Faigler Simchon , Weisz Daniel R , Seeburger Rhys , Almada Monter Silvia , Wojno Jennifer 
Published: October 2022

ABSTRACT
We report discovery of a bright, nearby ($G = 13.8;\, \, d = 480\, \rm pc$) Sun-like star orbiting a dark object. We identified the system as a black hole candidate via its astrometric orbital solution from the Gaia mission. Radial velocities validated and refined the Gaia solution, and spectroscopy ruled out significant light contributions from another star. Joint modelling of radial velocities and astrometry constrains the companion mass of $M_2 = 9.62\pm 0.18\, \mathrm{M}_{\odot }$. The spectroscopic orbit alone sets a minimum companion mass of $M_2\gt 5\, \mathrm{M}_{\odot }$; if the companion were a $5\, \mathrm{M}_{\odot }$ star, it would be 500 times more luminous than the entire system. These constraints are insensitive to the mass of the luminous star, which appears as a slowly rotating G dwarf ($T_{\rm eff}=5850\, \rm K$, log g = 4.5, $M=0.93\, \mathrm{M}_{\odot }$), with near-solar metallicity ($\rm [Fe/H] = -0.2$) and an unremarkable abundance pattern. We find no plausible astrophysical scenario that can explain the orbit and does not involve a black hole. The orbital period, Porb = 185.6 d, is longer than that of any known stellar-mass black hole binary. The system’s modest eccentricity (e = 0.45), high metallicity, and thin-disc Galactic orbit suggest that it was born in the Milky Way disc with at most a weak natal kick. How the system formed is uncertain. Common envelope evolution can only produce the system’s wide orbit under extreme and likely unphysical assumptions. Formation models involving triples or dynamical assembly in an open cluster may be more promising. This is the nearest known black hole by a factor of 3, and its discovery suggests the existence of a sizable population of dormant black holes in binaries. Future Gaia releases will likely facilitate the discovery of dozens more.
Three-dimensional propagation of kink wave trains in solar coronal slabs
Authors: Li Bo , Guo Mingzhe , Yu Hui , Chen Shao-Xia , Shi Mijie 
Published: October 2022

ABSTRACT
Impulsively excited wave trains are of considerable interest in solar coronal seismology. To our knowledge, however, it remains to examine the three-dimensional (3D) dispersive propagation of impulsive kink waves in straight, field-aligned, symmetric, low-beta, slab equilibria that are structured only in one transverse direction. We offer a study here, starting with an analysis of linear oblique kink modes from an eigenvalue problem perspective. Two features are numerically found for continuous and step structuring alike, one being that the group and phase velocities may lie on opposite sides of the equilibrium magnetic field ($\boldsymbol {B}_0$), and the other being that the group trajectories extend only to a limited angle from $\boldsymbol {B}_0$. We justify these features by making analytical progress for the step structuring. More importantly, we demonstrate by a 3D time-dependent simulation that these features show up in the intricate interference patterns of kink wave trains that arise from a localized initial perturbation. In a plane perpendicular to the direction of inhomogeneity, the large-time slab-guided patterns are confined to a narrow sector about $\boldsymbol {B}_0$, with some wavefronts propagating toward $\boldsymbol {B}_0$. We conclude that the phase and group diagrams lay the necessary framework for understanding the complicated time-dependent behaviour of impulsive waves.
A case of giant cell arteritis complicated by polymyalgia rheumatica with scalp necrosis and refractory jaw claudication
Authors: Kosaka Shumpei , Nawata Masao , Yamazumi Kenji , Nawata Aya , Nakamura Katsumi , Saito Kazuyoshi , Tanaka Yoshiya 
Published: October 2022

ABSTRACT
Scalp necrosis is a rare complication of giant cell arteritis (GCA); however, it is a predictor of severe disease. In this case study, a patient presented with GCA complicated by polymyalgia rheumatica with scalp necrosis. An 86-year-old woman was admitted to the hospital for pulsating headache, scalp pain, jaw claudication, and generalised pain. Bilateral temporal arteries were found to be distended and pulseless, and scalp necrosis was observed in the parietal region. Simultaneous high-resolution contrast-enhanced magnetic resonance imaging (MRI) sequences of the head, shoulder, and hip showed staining around the bilateral shallow temporal arteries, shoulder, and hip joints, which was confirmed as GCA with polymyalgia rheumatica using other examination findings. After treatment with early induction remission therapy, scalp necrosis healed, but jaw claudication persisted. Six months after the start of treatment, scalp necrosis was cured to full hair growth. Despite remission induction therapy combined with tocilizumab, the patient had persistent jaw claudication for several months. At that time, a high-resolution contrast-enhanced MRI re-examination was useful in assessing disease activity. GCA with scalp necrosis may cause prolonged jaw claudication reflecting the progression of ischaemic lesions, whereas the disease activity can be accurately assessed by combining MRI studies.