bluuebunny/crossref_metadata_2025_split huggingface dataset:
Overview of the contributions from all lanthanide elements to kilonova opacity in the temperature range from 25 000 to 40 000 K
Authors: Carvajal Gallego H. , Deprince J. , Maison L. , Palmeri P. , Quinet P. 
Published: March 2024

Context. It is now well established that the neutron star (NS) merger is at the origin of the production of trans-iron heavy elements in the universe. These elements are therefore present in large quantities in the ejected matter, whose electromagnetic radiation, called kilonova, is characterized by a significant opacity due to the high density of spectral lines belonging to many heavy ions. Among these, the lanthanide ions play an essential role since, with their open 4f subshell, they have a considerable number of transitions that can absorb emitted light. The knowledge of the atomic structure and the radiative parameters of these ions as well as the determination of the corresponding opacities is therefore of paramount importance for the spectral analysis of kilonovae.
Aims. The main goal of the present work is to determine the relative contributions of the different lanthanide elements to the opacity of the emission spectrum of a kilonova in its early phase, that is, a few hours after the NS merger, where the conditions are such that the temperature is between 25 000 and 40 000 K. At these temperatures, the lanthanide ions whose charge states are between V and VII are predominant.
Methods. We used the pseudo-relativistic Hartree–Fock (HFR) method extensively to calculate the relevant atomic data (energy levels, wavelengths, and oscillator strengths) in La-Lu V-VII ions. The corresponding monochromatic opacities were estimated from the expansion formalism.
Results. We calculated the spectroscopic parameters for a total of more than 800 million radiative transitions in all the ions considered. These data were used to estimate the expansion opacities and Planck mean opacities for all the lanthanide elements at early-phase kilonova conditions between 25 000 and 40 000 K, making it possible to deduce the respective contributions of each element as a function of temperature. Atomic calculations were also carried out with the fully relativistic Multiconfiguration Dirac-Hartree-Fock (MCDHF) method in the specific case of the Yb V ion, as the available experimental data had not yet been compared with the theoretical calculations in our previous studies on lanthanide ions.
Energetic particle activity in AD Leo: Detection of a solar-like type-IV burst
Authors: Mohan Atul , Mondal Surajit , Wedemeyer Sven , Gopalswamy Natchimuthuk 
Published: March 2024

Context. AD Leo is a young and active M dwarf with high flaring rates across the X-ray-to-radio bands. Flares accelerate particles in the outer coronal layers and often impact exo-space weather. Wide-band radio dynamic spectra let us explore the evolution of particle acceleration activity across the corona. Identifying the emission features and modelling the mechanisms can provide insights into the possible physical scenarios driving the particle acceleration processes.Aims. We performed an 8 h monitoring of AD Leo across the 550-850 MHz band using upgraded-Giant Metrewave Radio Telescope (uGMRT). The possible flare and post-flare emission mechanisms are explored based on the evolution of flux density and polarisation.Methods. The python-based module, Visibility Averaged Dynamic spectrum (VISAD), was developed to obtain the visibility-averaged wide-band dynamic spectra. Direct imaging was also performed with different frequency-time averaging. Based on existing observational results on AD Leo and on solar active region models, radial profiles of electron density and magnetic fields were derived. Applying these models, we explored the possible emission mechanisms and magnetic field profile of the flaring active region.Results. The star displayed a high brightness temperature (TB≈ 1010−1011K) throughout the observation. The emission was also nearly 100% left circularly polarised during bursts. The post-flare phase was characterised by a highly polarised (60–80%) solar-like type IV burst confined above 700 MHz.Conclusions. The flare emission favours a Z-mode or a higher harmonic X-mode electron cyclotron maser emission mechanism. The >700 MHz post-flare activity is consistent with a type-IV radio burst from flare-accelerated particles trapped in magnetic loops, which could be a coronal mass ejection (CME) signature. This is the first solar-like type-IV burst reported on a young active M dwarf belonging to a different age-related activity population (‘C’ branch) compared to the Sun (‘I’ branch). We also find that a multipole expansion model of the active region magnetic field better accounts for the observed radio emission than a solar-like active region profile.
Supermassive black hole spin evolution in cosmological simulations with OPENGADGET3
Authors: Sala Luca , Valentini Milena , Biffi Veronica , Dolag Klaus 
Published: March 2024

Context. The mass and spin of massive black holes (BHs) at the centre of galaxies evolve due to gas accretion and mergers with other BHs. Besides affecting the evolution of relativistic jets, for example, the BH spin determines the efficiency with which the BH radiates energy.
Aims. Using cosmological, hydrodynamical simulations, we investigate the evolution of the BH spin across cosmic time and its role in controlling the joint growth of supermassive BHs and their host galaxies.
Methods. We implemented a sub-resolution prescription that models the BH spin, accounting for both BH coalescence and misaligned accretion through a geometrically thin, optically thick disc. We investigated how BH spin evolves in two idealised setups, in zoomed-in simulations and in a cosmological volume. The latter simulation allowed us to retrieve statistically robust results for the evolution and distribution of BH spins as a function of BH properties.
Results. We find that BHs with MBH ≲ 2 × 107 M⊙ grow through gas accretion, occurring mostly in a coherent fashion that favours spin-up. Above MBH ≳ 2 × 107 M⊙, the gas angular momentum directions of subsequent accretion episodes are often uncorrelated with each other. The probability of counter-rotating accretion and hence spin-down increases with BH mass. In the latter mass regime, BH coalescence plays an important role. The spin magnitude displays a wide variety of histories, depending on the dynamical state of the gas feeding the BH and the relative contribution of mergers and gas accretion. As a result of their combined effect, we observe a broad range of values of the spin magnitude at the high-mass end. Reorientation of the BH spin direction occurs on short timescales (≲ 10 Myr) only during highly accreting phases (ƒEdd ≳ 0.1). Our predictions for the distributions of BH spin and spin-dependent radiative efficiency as a function of BH mass are in very good agreement with observations.
Massive clumps in W43-main: Structure formation in an extensively shocked molecular cloud
Authors: Lin Y. , Wyrowski F. , Liu H. B. , Gong Y. , Sipilä O. , Izquierdo A. , Csengeri T. , Ginsburg A. , Li G. X. , Spezzano S. , Pineda J. E. , Leurini S. , Caselli P. , Menten K. M. 
Published: March 2024

Aims. W43-main is a massive molecular complex undergoing starburst activities, located at the interaction of the Scutum arm and the Galactic bar. We aim to investigate the gas dynamics, in particular, the prevailing shock signatures from cloud to clump scales. We also look to assess the impact of shocks on the formation of dense gas and early-stage cores in OB cluster formation processes.
Methods. We carried out NOEMA and IRAM-30 m observations at 3 mm towards five molecular gas clumps in W43 main located within large-scale interacting gas components. We used CH3CCH and H2CS lines to trace the extended gas temperature and CH3OH lines to probe the volume density of the dense gas components (≳105 cm−3). We adopted multiple tracers that are sensitive to different gas density regimes to reflect the global gas motions. The density enhancements constrained by CH3OH and a population of NH2D cores are correlated (in the spatial and velocity domains) with SiO emission, which is a prominent indicator of shock processing in molecular clouds.
Results. The emission of SiO (2–1) is extensive across the region (~4 pc) and it is contained within a low-velocity regime, hinting at a large-scale origin for the shocks. Position-velocity maps of multiple tracers show systematic spatio-kinematic offsets supporting the cloud-cloud collision-merging scenario. We identified an additional extended velocity component in the CCH emission, which coincides with one of the velocity components of the larger scale 13CO (2−1) emission, likely representing an outer, less-dense gas layer in the cloud merging process. We find that the ‘V-shaped’, asymmetric SiO wings are tightly correlated with localised gas density enhancements, which is direct evidence of dense gas formation and accumulation in shocks. The dense gas that is formed in this way may facilitate the accretion of the embedded, massive pre-stellar and protostellar cores. We resolved two categories of NH2D cores: those exhibiting only subsonic to transonic velocity dispersions and those with an additional supersonic velocity dispersion. The centroid velocities of the latter cores are correlated with the shock front seen via SiO. The kinematics of the ~0.1 pc NH2D cores are heavily imprinted by shock activities and may represent a population of early-stage cores forming around the shock interface.
HD 7977 and its possible influence on Solar System bodies
Authors: Dybczyński Piotr A. , Królikowska Małgorzata , Bartczak Przemysław , Podlewska-Gaca Edyta , Kamiński Krzysztof , Tokarek Jakub , Langner Krzysztof , de Bruijne Jos 
Published: March 2024

Context. In the latest Gaia third data release, one can find extremely small proper motion components for the star HD 7977. This, together with the radial velocity measurement lead to the conclusion that this star passed very close to the Sun in the recent past.
Aims. Such a very close approach of a one solar mass star must have resulted in noticeable changes in the motion of all Solar System bodies, especially those on less tight orbits, namely long-period comets (LPCs) and transneptunian objects (TNOs). We estimate and discuss these effects.
Methods. Our current knowledge on the solar neighbourhood found in the latest Gaia catalogues allowed us to perform numerical integrations and prepare a list of potential stellar perturbers of LPCs. We used this list, made available in the StePPeD database. To study the past motion of LPCs under the simultaneous action of the Galactic potential and passing stars, we used precise original cometary orbits taken from the current CODE catalogue.
Results. We examined the reliability of the extremely small proper motion of HD 7977 and conclude that this star can be an unresolved binary; however, according to the astrometry covering more than a century, the current Gaia data cannot be ruled out. We present the parameters of a very close passage of this star near the Sun. We also show examples of the strong influence of this passage on the past motion of some LPCs. We also discuss the possible influence of this perturber on other Solar System bodies.
Conclusions. It is possible that 2.47 Myr ago the one solar mass star HD 7977 passed as close as 1000 au from the Sun. Such an event constitutes a kind of dynamical horizon for all studies of the past Solar System bodies’ dynamics.
Up around the bend: A multiwavelength view of the quasar 3C 345
Authors: Röder Jan , Ros Eduardo , Schinzel Frank K. , Lobanov Andrei P. 
Published: March 2024

Context. The flat-spectrum radio quasar 3C 345 has been showing γ-ray activity since the mid-2000s, along with activity across the electromagnetic spectrum. A γ-ray burst in 2009 was successfully linked to relativistic outflow in 43 GHz very long baseline interferometry (VLBI) observations and has since also been analyzed using single-dish measurements. A multiwavelength follow-up VLBI observation of the 2009 flare in conjunction with 43 GHz catalog data from the VLBA-BU-BLAZAR and BEAM-ME programs are analyzed in this study in the context of the long-term evolution of the source.
Aims. We aim to probe the innermost few milliarcseconds of the ultracompact 3C 345 jet. To do so, we analyzed the long-term kinematics of the inner jet and discuss the magnetic field morphology at different scales, as well as the origin of the γ-ray emission.
Methods. New observations at 23, 43, and 86 GHz were carried out at ten epochs between 2017 and 2019. We calibrated the 30 datasets using the rPicard pipeline, imaged them in Difmap, and carried out polarization calibration using the GPCAL pipeline. We complemented our VLBI data by 43 GHz observations carried out in the framework of the BEAM-ME and VLBA-BU-BLAZAR monitoring programs.
Results. We find multiple distinct component paths in the inner jet, which together have a helical geometry. The helix appears to be anchored at a stationary feature some 0.16 mas from the 43 GHz VLBI core and has an evolution timescale of about 8 yr. The characteristic bends in the jet morphology are caused by variations in the component ejection angle. We confirm the result of previous studies: the γ-ray emission is caused by relativistic outflow and violent interactions within the jet.
Bildgebung bei Großgefäßvaskulitiden
Authors: Bauer Claus-Jürgen , Petzinna Simon Michael , Schäfer Valentin Sebastian 
Published: March 2024

ZusammenfassungGroßgefäßvaskulitiden sind rheumatologische Autoimmunerkrankungen, die mit entzündlichen Gefäßwandveränderungen in der arteriellen Strombahn einhergehen und zu vielfältigen Organschäden führen können. Die beiden Hauptformen sind die Riesenzellarteriitis und die Takayasu-Arteriitis.Als Bildgebungsmodalitäten stehen die Gefäßsonografie mit ihren Stärken in der unmittelbaren Point-of-care-Anwendung (insbesondere in der Riesenzellarteriitisdiagnostik), die Magnetresonanztomografie und Computertomografie mit einer besonders guten Darstellung der Aorta und ihrer Abgänge sowie die 18F-Fluordesoxyglukose-Positronenemissionstomografie (18F-FDG-PET) zur Detektion von Entzündungsherden und der Großgefäßvaskulitisdiagnostik zur Verfügung. Zukünftige Entwicklungen in der bildgebenden Diagnostik von Großgefäßvaskulitiden könnten von Verfahren profitieren, die eine zielgerichtete Darstellung der Gefäßentzündung ermöglichen, wie beispielsweise das Gallium-68 DOTAVAP-P1 PET, welches derzeit am Universitätsklinikum Bonn erforscht wird.
Therapiekontrolle bei Immuntherapien mittels PET/CT
Authors: Wasserloos Anne , Beer Ambros J. , Thaiss Wolfgang 
Published: March 2024

ZusammenfassungIn der Therapiekontrolle bei Immuntherapien werden neben klinischen Einschätzungen auch bildgebende Verfahren eingesetzt. Hier gibt es einige Herausforderungen, die bei der Beurteilung beachtet werden müssen. Insbesondere der Pseudoprogress, Hyperprogress, ein heterogenes Therapieansprechen sowie unerwünschte Arzneimittelwirkungen können die Beurteilung des Therapieansprechens erschweren. Im Vergleich zur Computertomografie (CT) oder Magnetresonanztomografie (MRT) können Positronenemissionstomografie (PET)/Computertomografie (CT)-Untersuchungen zusätzliche Informationen liefern und bei der besseren Einordnung von Veränderungen helfen. Sowohl für die Beurteilung mittels CT und MRT als auch mittels PET/CT wurden bereits mehrere Klassifikationssysteme entwickelt, wobei sich für die Therapiebeurteilung mittels PET/CT noch keine Klassifikation als Standard im klinischen Alltag etabliert hat.
Immuntherapie mit Checkpointinhibitoren und schilddrüsentypische Komplikationen
Authors: Kreppel Barbara 
Published: March 2024

ZusammenfassungDie Therapie mit Immuncheckpointinhibitoren findet in den letzten Jahren zunehmend Anwendung bei der Therapie einer Vielzahl onkologischer Erkrankungen. Schilddrüsenfunktionsstörungen stellen eine der häufigsten unerwünschten Nebenwirkungen unter diesen Therapien dar. Initial kommt es häufig zu einer transienten, zerfallsbedingten Hyperthyreose, die dann in eine Hypothyreose übergeht. Der genaue pathophysiologische Mechanismus ist jedoch noch nicht hinreichend geklärt. Die Verläufe können asymptomatisch sein; nicht selten kommt es jedoch zu hyper- und hypothyreosetypischen Symptomen, die unter Umständen erst spät einer Schilddrüsenfunktionsstörung zugeordnet werden, da diese letztlich unspezifisch und auch im Rahmen der onkologischen Grunderkrankung denkbar sind. Daher ist bei Verdacht auf das Vorliegen eine fachspezifische Vorstellung beim Nuklearmediziner wichtig zur gezielten Diagnostik mittels Anamnese, Labor, Sonografie und ggf. auch Szintigrafie um weitere Differenzialdiagnosen auszuschließen. Bei Auftreten einer Hyperthyreose steht die symptomatische Therapie im Vordergrund; der Einsatz von Thyreostatika ist nur eingeschränkt zu empfehlen. Eine Hypothyreose sollte mit einer an den TSH-Wert und die Klinik angepassten Schilddrüsenhormonsubstitution therapiert werden. Bis ein stabiler Zustand erreicht ist, sollten dem Krankheitsverlauf angepasste fachspezifische Vorstellungen erfolgen. Im Regelfall kann die Immuntherapie ohne Unterbrechung fortgeführt werden.
Subkutane Applikation von Protonenpumpeninhibitoren – was ist bekannt?
Authors: Berner Jennifer , Rémi Constanze 
Published: March 2024

ZusammenfassungIn der Palliativversorgung ist die subkutane Applikationsroute als Alternative zur intravenösen Anwendung weit verbreitet. Bei einigen Arzneistoffen liegen nur wenige Daten zur Sicherheit dieses Applikationswegs vor. Hierzu zählen die Protonenpumpeninhibitoren (PPI) Omeprazol, Esomeprazol und Pantoprazol. Auf Basis einer Literaturrecherche (Medline Datenbank) wurde die verfügbare Evidenz zur subkutanen Applikation von PPI evaluiert. Sieben Publikationen wurden in die Auswertung eingeschlossen. Die subkutane Applikation der drei PPI ist in der Literatur in Fallberichten und Beobachtungsstudien mit geringer Fallzahl beschrieben, überwiegend als subkutane Kurzinfusion mit meist guter Verträglichkeit.
Exploring the link between financial literacy and business interruption insurance: evidence from Italian micro-enterprises
Authors: Ricci Ornella , Santilli Gianluca 
Published: March 2024

AbstractThis article examines the relationship between financial literacy and business interruption (BI) insurance among Italian entrepreneurs. Following an increase in unexpected shocks, such as COVID-19 and geopolitical conflicts, a high level of BI risk is expected to persist, especially among small firms, which play a key role in the Italian economy. Using a Bank of Italy 2021 survey of 1998 non-financial firms with fewer than 10 employees, we show a significant positive association between the level of the entrepreneur’s financial literacy and the purchase of BI insurance. Our results highlight the key role of financial literacy in shaping risk management strategies and are robust to different model specifications, also addressing endogeneity concerns.
Parylene-bonded micro-fluidic channels for cryogenic experiments at superfluid He-4 temperatures
Authors: Midlik Š. , Gablech I. , Goleňa M. , Brodský J. , Schmoranzer D. 
Published: March 2024

We present the manufacturing process of a (24.5 × 100) μm2-sized on-chip flow channel intended for flow experiments with normal and superfluid phases of 4He and showcase such a proof-of-concept experiment. This work proves the suitability of chip-to-chip bonding using a thin layer of Parylene-C for cryogenic temperatures as a simpler alternative to other techniques, such as anodic bonding. A monocrystalline silicon chip embeds the etched meander-shaped micro-fluidic channel and a deposited platinum heater and is bonded to a Pyrex glass top. We test the leak tightness of the proposed bonding method for superfluid 4He, reaching temperatures of ≈1.6 K and evaluate its possible effects on flow experiments. We demonstrate that powering an on-chip platinum heater affects the superfluid flow rate by local overheating of a section of the micro-fluidic channel.
A near-infrared laser dispersion spectrometer with phase modulation for open-path methane sensing
Authors: Wall Thomas E. , Macleod Neil A. , Weidmann Damien 
Published: March 2024

A laser-based open-path dispersion spectrometer for measuring atmospheric methane has been developed with the goal of achieving a very simple architecture, yet enabling molecular dispersion measurements immune to optical power variation. Well-mature, near-infrared photonics components were retained to demonstrate a compact, cost-effective, and low-power consumption dispersion spectrometer. In particular, measurements immune to received optical power variations are demonstrated despite the use of only phase modulation and are supported by the development of the corresponding physical model. The instrument has been validated under laboratory conditions, finding a precision of 2.6 ppb 100 m for a 2 s measurement, and demonstrated through atmospheric measurements performed continuously over six days with an 86 m path length.
Compact remanence-free permanent magnet-based variable magnetic field source
Authors: Ivanov S. , Chen H. , Szurek M. , Urazhdin S. 
Published: March 2024

We demonstrate a simple and compact variable magnetic field source based on the permanent cube magnet array approximating a Halbach cylinder. The large air gap area accommodates standard cryostat tails while providing a high uniformity and magnetic field stability of up to 0.5 T over regions of up to about a centimeter. It eliminates magnetic remanence effects and produces reproducible fields without the need for feedback. Thanks to the low cost and exceptional energy efficiency, it provides an accessible solution for modest magnetic field requirements in a wide range of research applications.