bluuebunny/crossref_metadata_2025 huggingface dataset:
Unveiling hidden companions in post-common-envelope binaries: A robust strategy and uncertainty exploration
Authors: Giuppone Cristian A. , Gramajo Luciana V. , Gianuzzi Emmanuel , Ramos Matías N. , Cuello Nicolás , Hinse Tobias C.
Published: January 2024

Context. Some post-common-envelope binaries (PCEBs) are binary stars with short periods that exhibit significant period variations over long observational time spans. These eclipse timing variations (ETVs) are most likely to be accounted for by the presence of an unseen massive companion, potentially of planetary or substellar nature, and the light-travel time (LTT) effect. The existence of such companions challenges our current understanding of planetary formation and stellar evolution.

Aims. In this study, our main objective is to describe the diversity of compatible nontransit companions around PCEBs and explore the robustness of the solutions by employing tools for uncertainty estimation. We select the controversial data of the QS Vir binary star, which previous studies have suggested hosts a planet.

Methods. We employ a minimizing strategy, using genetic algorithms to explore the global parameter space followed by refinement of the solution using the simplex method. We evaluate errors through the classical Markov chain Monte Carlo (MCMC) approach and discuss the error range for parameters, considering the 1σ values obtained from the minimization.

Results. Our results highlight the strong dependence of ETV models for close binaries on the dataset used, which leads to relatively loose constraints on the parameters of the unseen companion. We find that the shape of the O – C curve is influenced by the dataset employed. We propose an alternative method to evaluate errors on the orbital fits based on a grid search surrounding the best-fit values, obtaining a wider range of plausible solutions that are compatible with goodness-of-fit statistics. We also analyze how the parameter solutions are affected by the choice of the dataset, and find that this system continuously changes the compatible solutions as new data are obtained from eclipses.

Conclusions. The best-fit parameters for QS Vir correspond to a low-mass stellar companion (57.71 Mjup ranging from ~40 to ~64 Mjup) on an eccentric orbit (e = 0.91−0.17+0.07) with a variety of potential periods (P = 16.69−0.42+0.47 yr.). Most solutions within 1σ exhibit regular orbits, despite their high eccentricity. Additional observations are required to accurately determine the period and other parameters of the unseen companion. In this context, we propose that a fourth body should not be modeled to fit the data, unless new observations considerably modify the computed orbital parameters. This methodology can be applied to other evolved binary stars suspected of hosting companions.
A model for the hydrogenation and charge states of fullerene C60
Authors: Abbink Daphne , Foing Bernard , Ehrenfreund Pascale
Published: January 2024

Context. The diffuse interstellar bands (DIBs) are a set of ∼600 absorption features at optical and near-infrared wavelengths that are found in the interstellar medium in the Milky Way and other galaxies. They remain mostly unidentified and represent the greatest unsolved mystery in astronomical spectroscopy of the past 100 years. Many studies indicate that the carrier molecules are likely carbonaceous molecules, such as polycyclic aromatic hydrocarbons (PAHs) or fullerenes, a theory that is supported by the identifications of five DIBs in the near-infrared attributed to C60+.

Aims. This work aims to narrow down which compounds related to C60 could be promising DIB carrier candidates. We did so by conducting a theoretical study of its hydrogenation and charge balance.

Methods. We defined a system of relevant reactions, and for each reaction we computed or derived from the literature a reaction rate coefficient. Assuming a steady state, we then computed a distribution of relative abundances in each hydrogenation and charge state.

Results. From the model outcomes, we expect the most abundant hydrogenated buckminsterfullerene compound in the diffuse interstellar medium to be C60H+.
Eruptive events with exceptionally bright emission in H I Ly-α observed by the Metis coronagraph
Authors: Russano G. , Andretta V. , De Leo Y. , Teriaca L. , Uslenghi M. , Giordano S. , Telloni D. , Heinzel P. , Jejčič S. , Abbo L. , Bemporad A. , Burtovoi A. , Capuano G. E. , Frassati F. , Guglielmino S. L. , Jerse G. , Landini F. , Liberatore A. , Nicolini G. , Pancrazzi M. , Romano P. , Sasso C. , Susino R. , Zangrilli L. , Da Deppo V. , Fineschi S. , Grimani C. , Moses J. D. , Naletto G. , Romoli M. , Spadaro D. , Stangalini M.
Published: January 2024

Context. Ultraviolet (UV) emission from coronal mass ejections can provide information on the evolution of plasma dynamics, temperature, and elemental composition, as demonstrated by the UV Coronagraph Spectrometer (UVCS) on board the SOlar and Heliospheric Observatory (SOHO). Metis, the coronagraph on board Solar Orbiter, provides for the first time coronagraphic imaging in the UV H I Ly-α line and, simultaneously, in polarized visible light, thus providing a host of information on the properties of coronal mass ejections and solar eruptions such as their overall dynamics, time evolution, mass content, and outflow propagation velocity in the expanding corona.

Aims. For this work, we analyzed six coronal mass ejections observed by Metis between April and October 2021, which are characterized by a very strong H I Ly-α emission. We studied in particular the morphology, kinematics, and the temporal and radial evolution of the emission of such events, focusing on the brightest UV features.

Methods. The kinematics of the eruptive events under consideration were studied by determining the height-time profiles of the brightest parts on the Metis plane of the sky. Furthermore, the 3D positions in the heliosphere of the coronal mass ejections were determined by employing co-temporal images, when available, from two other coronagraphs: LASCO/C2 on board SOHO, and COR2 on board STEREO-A. In three cases, the most likely source region on the solar surface could be identified. Finally, the radiometrically calibrated Metis images of the bright UV features were analyzed to provide estimates of their volume and density. From the kinematics and radiometric analysis, we obtained indications of the temperatures of the bright UV cores of these events. These results were then compared with previous studies with the UVCS spectrocoronagraph.

Results. The analysis of these strong UV-emitting features associated with coronal mass ejections demonstrates the capabilities of the current constellation of space coronagraphs, Metis, LASCO/C2, and COR2, in providing a complete characterization of the structure and dynamics of eruptive events in their propagation phase from their inception up to several solar radii. Furthermore, we show how the unique capabilities of the Metis instrument to observe these events in both the H I Ly-α line and polarized VL radiation allow plasma diagnostics on the thermal state of these events.
High-speed stars
Authors: Bonifacio P. , Caffau E. , Monaco L. , Sbordone L. , Spite M. , Mucciarelli A. , François P. , Lombardo L. , Matas Pinto A. d. M.
Published: January 2024

Context. The data from the Gaia satellite led us to revise our conception of the Galaxy structure and history. Hitherto unknown components have been discovered and a deep re-thinking of what the Galactic halo is in progress.

Aims. We selected from the Gaia catalogue stars with extreme transverse velocities with respect to the Sun (|VT|> 500 km s−1) and observed them with FORS2 at the ESO VLT, to classify them using both their chemical and dynamical properties. Two apparently young stars, identified in Paper I, were observed with UVES.

Methods. We derived abundances for Na, Mg, Ca, Ti, Mn, and Fe, analysing the spectra with MyGIsFOS, while for Ba we used line profile fitting. We computed actions from parallaxes and kinematical data.

Results. The stars span the metallicity range −3.5 ≤ [Fe/H] ≤ −0.5 with ⟨[Fe/H]⟩ = −1.6. Star GHS143 has a total speed of about 1440 km s−1, which is almost three times faster than the local escape velocity of 522 km s−1, strongly implying this star is unbound to the Galaxy. Remarkably, this star is not escaping from the Galaxy, but it is falling into it. Ten stars are apparently young with masses in excess of 1.3 M⊙. Their interpretation as evolved blue stragglers is doubtful. The existence of a young metal-poor population is possible. The two stars observed with UVES show no lithium, suggesting they are blue stragglers. We detected a metal-poor population, confined to the bulge, that we call SpiteF, and argue that it is the result of a recent accretion event. We detect 102 candidates of the Aurora population that should have formed prior to the formation of the disc.

Conclusions. Our sample is non-homogeneous and mainly retrograde. The stars are metal poor, and 23% have [Fe/H] ≤ −2.0. Our selection is efficient at finding very metal-poor stars, but it selects peculiar populations.
GA-NIFS: Early-stage feedback in a heavily obscured active galactic nucleus at z  =  4.76
Authors: Parlanti Eleonora , Carniani Stefano , Übler Hannah , Venturi Giacomo , Circosta Chiara , D’Eugenio Francesco , Arribas Santiago , Bunker Andrew J. , Charlot Stéphane , Lützgendorf Nora , Maiolino Roberto , Perna Michele , Del Pino Bruno Rodríguez , Willott Chris J. , Böker Torsten , Cameron Alex J. , Chevallard Jacopo , Cresci Giovanni , Jones Gareth C. , Kumari Nimisha , Lamperti Isabella , Scholtz Jan
Published: January 2024

Dust-obscured galaxies are thought to represent an early evolutionary phase of massive galaxies in which the active galactic nucleus (AGN) is still deeply buried in significant amounts of dusty material and its emission is strongly suppressed. The unprecedented sensitivity of the James Webb Space Telescope (JWST) enabled us for the first time to detect the rest-frame optical emission of heavily obscured AGNs and unveil the properties of the hidden accreting super-massive black holes (BHs). In this work, we present the JWST/NIRSpec integral field spectroscopy (IFS) data of ALESS073.1, a massive (log(M⋆/M⊙) = 10.98) dusty, star-forming galaxy at z = 4.755 hosting an AGN at its center. The detection of a very broad (> 9000 km s−1) Hα emission associated with the broad line region (BLR) confirms the presence of a BH (log(MBH/M⊙) > 8.7) accreting at less than 18% of its Eddington limit. The identification of the BLR classifies the target as a type 1 AGN despite the observed high column density of NH ∼ 1024 cm−2. The rest-frame optical emission lines also reveal a fast (∼1700 km s−1) ionized gas outflow marginally resolved in the galaxy center. The high sensitivity of NIRSpec allowed us to perform the kinematic analysis of the narrow Hα component, which indicates that the warm ionized gas velocity field is consistent with disk rotation. Interestingly, we find that in the innermost nuclear regions (< 1.5 kpc), the intrinsic velocity dispersion of the disk reaches ∼150 km s−1, which is ∼2 − 3 times higher than the velocity dispersion inferred from the [C II] 158 μm line tracing mostly cold gas. Since at large radii the velocity dispersion of the warm and cold gas are comparable, we conclude that the outflows are injecting turbulence in the warm ionized gas in the central region, but they are not sufficiently powerful to disrupt the dense gas and quench star formation. These findings support the scenario that dust-obscured galaxies represent the evolutionary stage preceding the unobscured quasar when all gas and dust are removed from the host.
Revisiting the warm sub-Saturn TOI-1710b
Authors: Orell-Miquel J. , Carleo I. , Murgas F. , Nowak G. , Pallé E. , Luque R. , Masseron T. , Sanz-Forcada J. , Dragomir D. , Dalba P. A. , Tronsgaard R. , Wittrock J. , Kim K. , Stibbards C. , Collins K. I. , Plavchan P. , Howell S. B. , Furlan E. , Buchhave L. A. , Gnilka C. L. , Gupta A. F. , Henning Th. , Lester K. V. , Rodriguez J. E. , Scott N. J. , Osborn H. P. , Villanueva S. , Seager S. , Winn J. N. , Jenkins J. M. , Vanderspek R. , Latham D. W. , Rowden P. , Watanabe D. , Torres G. , Burke C. J. , Daylan T. , Barclay T. , Twicken J. D. , Ricker G. R.
Published: January 2024

The Transiting Exoplanet Survey Satellite (TESS) provides a continuous suite of new planet candidates that need confirmation and precise mass determination from ground-based observatories. This is the case for the G-type star TOI-1710, which is known to host a transiting sub-Saturn planet (Mp = 28.3 ± 4.7 M⊕) in a long-period orbit (P = 24.28 days). Here we combine archival SOPHIE and new and archival HARPS-N radial velocity data with newly available TESS data to refine the planetary parameters of the system and derive a new mass measurement for the transiting planet, taking into account the impact of the stellar activity on the mass measurement. We report for TOI-1710b a radius of Rp = 5.15 ± 0.12 R⊕, a mass of Mp = 18.4 ± 4.5 M⊕, and a mean bulk density of ρp = 0.73 ± 0.18 g cm−3, which are consistent at 1.2σ, 1.5σ, and 0.7σ, respectively, with previous measurements. Although there is not a significant difference in the final mass measurement, we needed to add a Gaussian process component to successfully fit the radial velocity dataset. This work illustrates that adding more measurements does not necessarily imply a better mass determination in terms of precision, even though they contribute to increasing our full understanding of the system. Furthermore, TOI-1710b joins an intriguing class of planets with radii in the range 4–8 R⊕ that have no counterparts in the Solar System. A large gaseous envelope and a bright host star make TOI-1710b a very suitable candidate for follow-up atmospheric characterization.
The size-luminosity relation of local active galactic nuclei from interferometric observations of the broad-line region
Authors:   GRAVITY Collaboration, Amorim A. , Bourdarot G. , Brandner W. , Cao Y. , Clénet Y. , Davies R. , de Zeeuw P. T. , Dexter J. , Drescher A. , Eckart A. , Eisenhauer F. , Fabricius M. , Feuchtgruber H. , Förster Schreiber N. M. , Garcia P. J. V. , Genzel R. , Gillessen S. , Gratadour D. , Hönig S. , Kishimoto M. , Lacour S. , Lutz D. , Millour F. , Netzer H. , Ott T. , Paumard T. , Perraut K. , Perrin G. , Peterson B. M. , Petrucci P. O. , Pfuhl O. , Prieto M. A. , Rabien S. , Rouan D. , Santos D. J. D. , Shangguan J. , Shimizu T. , Sternberg A. , Straubmeier C. , Sturm E. , Tacconi L. J. , Tristram K. R. W. , Widmann F. , Woillez J.
Published: January 2024

By using the GRAVITY instrument with the near-infrared (NIR) Very Large Telescope Interferometer (VLTI), the structure of the broad (emission-)line region (BLR) in active galactic nuclei (AGNs) can be spatially resolved, allowing the central black hole (BH) mass to be determined. This work reports new NIR VLTI/GRAVITY interferometric spectra for four type 1 AGNs (Mrk 509, PDS 456, Mrk 1239, and IC 4329A) with resolved broad-line emission. Dynamical modelling of interferometric data constrains the BLR radius and central BH mass measurements for our targets and reveals outflow-dominated BLRs for Mrk 509 and PDS 456. We present an updated radius-luminosity (R-L) relation independent of that derived with reverberation mapping (RM) measurements using all the GRAVITY-observed AGNs. We find our R-L relation to be largely consistent with that derived from RM measurements except at high luminosity, where BLR radii seem to be smaller than predicted. This is consistent with RM-based claims that high Eddington ratio AGNs show consistently smaller BLR sizes. The BH masses of our targets are also consistent with the standard MBH-σ* relation. Model-independent photocentre fitting shows spatial offsets between the hot dust continuum and the BLR photocentres (ranging from ∼17 μas to 140 μas) that are generally perpendicular to the alignment of the red- and blueshifted BLR photocentres. These offsets are found to be related to the AGN luminosity and could be caused by asymmetric K-band emission of the hot dust, shifting the dust photocentre. We discuss various possible scenarios that can explain this phenomenon.
Accurate ab initio spectroscopic studies of promising interstellar ethanolamine iminic precursors
Authors: Alberton D. , Inostroza-Pino N. , Fortenberry Ryan C. , Lattanzi V. , Endres C. , Zamponi J. Fuentealba , Caselli P.
Published: January 2024

Context. The detection of NH2CH2CH2OH (ethanolamine) in molecular cloud G+0.693-0.027 adds an additional player to the pre-biotic molecules discovered so far in the interstellar medium (ISM). As this molecule might be formed through condensed-phase hydrogenation steps, detecting one or more of the molecules involved might help to elucidate the chemical pathway leading to its production.

Aims. The chemical path involves the formation of four chemical species. In this work, we study the energies of the isomers involved, indicate the best candidates for detection purposes, and provide the distortion constants of the most energetically favoured isomers undetected so far.

Methods. We used highly accurate CCSD(T)-F12/cc-pCVTZ-F12 computations to predict the lowest energy isomers as well as their spectroscopic constants, taking corrections for core electron correlation and scalar relativity into account.

Results. We studied 14 isomers. We find that the lowest energy isomer proposed in previous studies is not the actual minimum. We provide a set of rotational and distortion constants of the two new most stable isomers together with their fundamental vibrational frequencies in order to guide the search for these important astrochemical precursors of prebiotic molecules in the ISM.
Effect of nuclear reactions rates and core boundary mixing on the seismology of red clump stars
Authors: Noll Anthony , Basu Sarbani , Hekker Saskia
Published: January 2024

Context. Modeling of the stars in the red clump (RC), that is, core helium-burning stars that have gone through a He flash, is challenging because of the uncertainties associated with the physical processes in their core and during the helium flash. By probing the internal stellar structure, asteroseismology allows us to constrain the core properties of RC stars and eventually, to improve our understanding of this evolutionary phase.

Aims. We aim to quantify the impact on the seismic properties of the RC stars of the two main core modeling uncertainties: core boundary mixing, and helium-burning nuclear reaction rates.

Methods. Using the MESA stellar evolution code, we computed models with different core boundary mixing as well as different 3α and 12C(α, γ)16O nuclear reaction rates. We investigated the impact of these parameters on the period spacing ΔΠ, which is a probe of the region around the core.

Results. We find that different core boundary mixing schemes yield significantly different period spacings, with differences of 30 s between the maximum ΔΠ value computed with semiconvection and maximal overshoot. We show that an increased rate of 12C(α, γ)16O lengthens the core helium-burning phase, which extends the range of ΔΠ covered by the models during their evolution. This results in a difference of 10 s between the models computed with a nominal rate and a rate multiplied by 2, which exceeds the observational uncertainties. The effect of changing the 3α reaction rate is comparatively small.

Conclusions. The core boundary mixing is the main source of uncertainty in the seismic modeling of RC stars. Moreover, the effect of the 12C(α, γ)16O is non-negligible, even though it is difficult to distinguish from the effect of the mixing. This degeneracy could be seen more frequently in the future in the new seismic data from the PLATO mission and through theoretical constraints from numerical simulations.
Tracing the evolution of short-period binaries with super-synchronous fast rotators
Authors: Britavskiy N. , Renzo M. , Nazé Y. , Rauw G. , Vynatheya P.
Published: January 2024

Context. The initial distribution of rotational velocities of stars is still poorly known, and how the stellar spin evolves from birth to the various end points of stellar evolution is an actively debated topic. Binary interactions are often invoked to explain the existence of extremely fast-rotating stars (vsin i ≳ 200 km s−1). The primary mechanisms through which binaries can spin up stars are tidal interactions, mass transfer, and possibly mergers. However, fast rotation could also be primordial, that is, a result of the star formation process. To evaluate these scenarios, we investigated in detail the evolution of three known fast-rotating stars in short-period spectroscopic and eclipsing binaries, namely HD 25631, HD 191495, and HD 46485, with primaries of masses of 7, 15, and 24 M⊙, respectively, with companions of ∼1 M⊙ and orbital periods of less than 7 days. These systems belong to a recently identified class of binaries with extreme mass ratios, whose evolutionary origin is still poorly understood.

Aims. We evaluated in detail three scenarios that could explain the fast rotation observed in these binaries: it could be primordial, a product of mass transfer, or the result of a merger within an originally triple system. We also discuss the future evolution of these systems to shed light on the impact of fast rotation on binary products.

Methods. We computed grids of single and binary MESA models varying tidal forces and initial binary architectures to investigate the evolution and reproduce observational properties of these systems. When considering the triple scenario, we determined the region of parameter space compatible with the observed binaries and used a publicly available machine-learning model to determine the dynamical stability of the triple system.

Results. We find that, because of the extreme mass-ratio between binary components, tides have a limited impact, regardless of the prescription used, and that the observed short orbital periods are at odds with post-mass-transfer scenarios. We also find that the overwhelming majority of triple systems compatible with the observed binaries are dynamically unstable and would be disrupted within years of formation, forcing a hypothetical merger to happen so close to a zero-age main-sequence that it could be considered part of the star formation process.

Conclusions. The most likely scenario to form such young, rapidly rotating, and short-period binaries is primordial rotation, implying that the observed binaries are pre-interaction ones. Our simulations further indicate that such systems will subsequently go through a common envelope and likely merge. These binaries show that the initial spin distribution of massive stars can have a wide range of rotational velocities.
Six new eccentric eclipsing systems with a third body
Authors: Zasche P. , Henzl Z. , Wolf M.
Published: January 2024

We present the discovery of six new triple stellar system candidates composed of an inner eccentric-orbit eclipsing binary with an apsidal motion. These stars were studied using new, precise TESS light curves and a long-term collection of older photometric ground-based data. These data were used for the monitoring of ETVs (eclipse timing variations) and to detect the slow apsidal movements along with additional periodic signals. The systems analysed were ASASSN-V J012214.37+643943.3 (orbital period 2.01156 d, eccentricity 0.15, third body with 3.3 yr period); ASASSN-V J052227.78+345257.6 (2.42673 d, 0.35, 3.2 yr); ASASSN-V J203158.98+410731.4 (2.53109 d, 0.20, 2.7 yr); ASASSN-V J230945.10+605349.3 (2.08957 d, 0.18, 2.3 yr); ASASSN-V J231028.27+590841.8 (2.41767 d, 0.43, 4.9 yr); and NSV 14698 (3.30047 d, 0.147, 0.5 yr). In the system ASASSN-V J230945.10+605349.3, we detected a second eclipsing pair (per 2.99252 d) and found adequate ETV for the pair B, proving its 2+2 bound quadruple nature. All of these detected systems deserve special attention from long-term studies for their three-body dynamics since their outer orbital periods are not too long and because some dynamical effects should be detectable during the next decades. The system NSV 14698 especially seems to be the most interesting from the dynamical point of view due to it having the shortest outer period of the systems we studied, its fast apsidal motion, and its possible orbital changes during the whole 20th century.
Investigating coronal loop morphology and dynamics from two vantage points
Authors: Mandal Sudip , Peter Hardi , Klimchuk James A. , Solanki Sami K. , Pradeep Chitta Lakshmi , Aznar Cuadrado Regina , Schühle Udo , Teriaca Luca , Berghmans David , Verbeeck Cis , Auchère Frederic , Stegen Koen
Published: January 2024

Coronal loops are the fundamental building blocks of the solar corona. Therefore, comprehending their properties is essential in unraveling the dynamics of the upper solar atmosphere. In this study, we conduct a comparative analysis of the morphology and dynamics of a coronal loop observed from two different spacecraft: the High Resolution Imager (HRIEUV) of the Extreme Ultraviolet Imager on board the Solar Orbiter, and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory. These spacecraft were separated by 43° during this observation. The main findings of this study are that (1) the observed loop exhibits similar widths in both the HRIEUV and AIA data, suggesting that the cross-sectional shape of the loop is circular; (2) the loop maintains a uniform width along its entire length, supporting the notion that coronal loops do not exhibit expansion; and (3) notably, the loop undergoes unconventional dynamics, including thread separation and abrupt downward movement. Intriguingly, these dynamic features also appear similar in data from both spacecraft. Although based on observation of a single loop, these results raise questions about the validity of the coronal-veil hypothesis and underscore the intricate and diverse nature of the complexity within coronal loops.
Testing pulsation diagnostics in the rapidly oscillating magnetic Ap star γ Equ using near-infrared CRIRES+ observations
Authors: Järvinen S. P. , Hubrig S. , Wolff B. , Kurtz D. W. , Mathys G. , Chojnowski S. D. , Schöller M. , Ilyin I.
Published: January 2024

Context. Pulsations of rapidly oscillating Ap stars and their interaction with the stellar magnetic field have not been studied in the near-infrared (near-IR) region despite the benefits these observations offer compared to visual wavelengths. The main advantage of the near-IR is the quadratic dependence of the Zeeman effect on the wavelength, as opposed to the linear dependence of the Doppler effect.

Aims. To test pulsation diagnostics of roAp stars in the near-IR, we aim to investigate the pulsation behaviour of one of the brightest magnetic roAp stars, γ Equ, which possesses a strong surface magnetic field of the order of several kilogauss and exhibits magnetically split spectral lines in its spectra.

Methods. Two magnetically split spectral lines belonging to different elements, the triplet Fe I at 1563.63 nm and the pseudo-doublet Ce III at 1629.2 nm, were recorded with CRIRES+ over about one hour in the H band with the aim of understanding the character of the line profile variability and the pulsation behaviour of the magnetic field modulus.

Results. The profile shapes of both studied magnetically split spectral lines vary in a rather complex manner probably due to a significant decrease in the strength of the longitudinal field component and an increase in the strength of the transverse field components over the last decade. A mean magnetic field modulus of 3.9 kG was determined for the Zeeman triplet Fe I at 1563.63 nm, whereas for the pseudo-doublet Ce III at 1629.2 nm we observe a much lower value of only about 2.9 kG. For comparison, a mean field modulus of 3.4kG was determined using the Zeeman doublet Fe II at 6249.25 in optical PEPSI spectra recorded just about two weeks before the CRIRES+ observations. Different effects that may lead to the differences in the field modulus values are discussed. Our measurements of the mean magnetic field modulus using the line profiles recorded in different pulsational phase bins suggest a field modulus variability of 32 G for the Zeeman triplet Fe I at 1563.63 nm and 102 G for the pseudo-doublet Ce III at 1629.2 nm.
Hyperfine excitation of NH and ND by molecular hydrogen
Authors: Pirlot Jankowiak Paul , Lique François , Goicoechea Javier R.
Published: January 2024

The NH and ND radicals are of key importance in the comprehension of nitrogen chemistry and the enhancement of deuterated molecules in the interstellar medium. Observations by space telescopes yield spectra that can resolve the fine and hyperfine structure of these radicals, a consequence of the electronic and magnetic interactions of nitrogen, hydrogen, and deuterium nuclei. Accurate rate coefficients, induced by collisions with H2, are required to interpret spectra of these radicals. We report the first rate coefficients for fine and hyperfine transitions of NH and ND in collision with both ortho- and para-H2. Based on a recent four-dimensional potential energy surface, fine-structure resolved cross sections and rate coefficients are computed with the time-independent close-coupling method over a temperature range of 5–300 K. Our calculations include the first 25 energy levels of NH and ND. Hyperfine resolved cross sections and rate coefficients are determined using the infinite-order sudden (IOS) approximation between 5 and 200 K for NH and 100 K for ND. We consider the first 71 and 105 energy levels of NH and ND, respectively. General propensity rules are discussed. We found a significant isotopic substitution effect in the rate coefficients. In addition, the rate coefficients for collisions with H2 are larger than those with He by a factor of up to 5, leading to lower critical densities for collisional excitation with H2 than He. The impact of the new set of collisional data has been investigated in simple radiative transfer models of the NH emission seen toward the Orion Bar and the ejecta of the η Carinae binary star. We observed significant differences by a factor of 5 between the presently determined column densities for NH compared to those from the literature using He as a collider.
Color restoration of images through high order zeroing neural networks
Authors: Mourtas Spyridon D.
Published: January 2024

One of the fundamental tasks in pattern recognition is color image restoration. Every color image has three channels in the RGB color space, in contrast to grayscale images. The restoration of color images is typically far more challenging than that of grayscale images because of the internal relationships among the three channels. Given that the color image restoration can be represented as a dynamic problem with quaternion matrices, a new high order zeroing neural network (HZNN) model is developed to tackle this issue. Specifically, the time-varying quaternion matrix linear equations can be solved using the HZNN design, which is a member of the family of zeroing neural network (ZNN) models that correlate to hyperpower iterative techniques. In a realistic color image restoration application, the HZNN design outperforms the ZNN design, although both approaches work amazingly well.
Quantum optimization methods in energy systems
Authors: Muhamediyeva Dilnoz
Published: January 2024

This paper discusses the application of quantum algorithms to the optimization of energy systems, focusing on solving the routing problem in the context of energy. A quantum approach that utilizes the principles of superposition and inversion with respect to the mean to efficiently find optimal energy routing is proposed. Research is carried out to develop a special quantum oracle to represent the structure of energy networks and energy flows between nodes. The application of inversion with respect to the mean provides efficient convergence to optimal solutions in the space of possible routes. We implement the quantum algorithm in the form of a quantum circuit, visualize the results and provide an analysis of the optimal energy routes. The work represents an important step in the development of quantum optimization methods for solving complex problems in the field of energy and may have prospects in practical applications in the future.
Development of the model of external control of quality indicators of electronic courses
Authors: Shifrin Boris , Eliseev Igor , Sokolova Viktoriia , Voinash Sergey , Zagidullin Ramil , Akhmetshin Stanislav , Meshkov Sergey
Published: January 2024

This article presents an analytical survey of internationally accepted samples for the assessment of online courses. By reviewing existing practices from around the world, the article identifies common approaches and methodologies used to evaluate the quality of electronic courses. This approach utilizes a combination of simple numeric values and fuzzy linguistic variables, which are then aggregated using fuzzy logic. This combination of numeric values and linguistic variables allows for a more comprehensive assessment of electronic courses. It takes into account both quantifiable factors, such as completion rates or assessment scores, as well as subjective factors, such as user satisfaction or engagement levels by utilizing fuzzy logic, the proposed approach is able to handle the inherent uncertainty and subjectivity in some of these indicators. The proposed approach aims to provide a more robust and accurate evaluation of the quality of electronic courses. It builds upon internationally accepted samples and incorporates a combination of objective and subjective indicators, using fuzzy logic to handle the varying degrees of uncertainty. This approach can contribute to the development of a standardized and comprehensive system for assessing the quality of electronic courses.
Topological optimization of the design of a permanent magnet synchronous motor using a genetic algorithm
Authors: Petrov Timur
Published: January 2024

The operating efficiency of a synchronous motor strongly depends on the design of its component parts, including the arrangement of materials (topology) of the rotor. An important element of the rotor, and at the same time the most expensive, are permanent magnets made of NdFeB material. Topological optimization allows you to reduce the volume of permanent magnets, which will reduce the price of the motor, or switch to cheaper materials, for example, ferrite, while maintaining performance characteristics. A genetic algorithm is used as a search method. And an important feature is that topological optimization is complex; not only electromagnetic parameters are checked, but also the thermal and strength characteristics of a synchronous motor. This test allows us to obtain designs that can be manufactured in practice. The article discusses the developed method of complex topological optimization using a genetic algorithm, optimization results and methods for testing the resulting structures. Optimization allows you to reduce the volume of NdFeB magnets by 2232%, which reduces the cost of the motor by 14–21%, or switch to ferrite magnets, which reduces the cost by 24–33%, while the torque value changes within 2%, which indicates about conservation of torque.
System approach to building a mathematical model of a complex organizational-technical system in transport
Authors: Zhukov Aleksandr , Kalinin Timur , Kartsan Igor , Lisickiy Vladimir , Stasiuk Vladislav
Published: January 2024

The current situation in the synthesis of complex organizational and technical systems in transport is characterized by a significant lag in the level of development of special mathematical and software, which significantly reduces the pace of development and efficiency of complex organizational and technical systems. This, in turn, does not allow to fully use the potential opportunities of scientific and technical progress to improve complex organizational and technical systems in transport. The fact of system and circuit synthesis of complex systems, a number of important fundamental tasks of system synthesis of multi-level hierarchical systems, to which complex organizational and technical systems belong. In the literature the objective prerequisites determining the necessity, expediency and possibility of their solution have not been sufficiently considered yet.
Thefittest: evolutionary machine learning in Python
Authors: Sherstnev Pavel
Published: January 2024

Thefittest is a new Python library specializing in evolutionary optimization methods and machine learning methods that use evolutionary optimization methods. Thefittest provides both classical evolutionary algorithms and efficient modifications of these algorithms that do not have implementations in the open access. Among the advantages of the library are the performance of the implemented methods, accessibility and ease of use. The paper discusses the motivation for developing and leading the project, describes the structure of the library with examples of use, and provides a comparison with other projects with a similar development goal. Thefittest is an open-source project published on GitHub and PyPi, developed using modern methods of code analysis and testing. At the moment of writing the paper, the latest version of the library is 0.2.3.
Development and analysis of a self-configuring differential evolution algorithm
Authors: Novikov Zakhar , Vakhnin Aleksei
Published: January 2024

In this study to solve optimization problem, three differential evolution algorithms are tested on various functions, highlighting its parameter sensitivity. To overcome this, a self-configuring algorithm is introduced, which core idea is to periodically reevaluate configurations, favoring those with superior performance. Self-configuring algorithms in most cases outperform or match conventional methods, enhancing the likelihood of achieving superior results.
Developing a machine learning model for fake news detection
Authors: Filippov Rodion , Sazonova Anna , Leonov Yuri
Published: January 2024

The article is devoted to the problem of detecting fake news. This issue is relevant nowadays. Fake news paves the way for deceiving people and promoting ideologies. People who provide incorrect information benefit by earning money from the number of interactions with their publications. One of the typical tasks that arise in the process of identifying news is determining whether news belongs to one of two classes, namely the fake news or the real news. With the help of modern methods of machine learning and primary data processing, this problem is effectively solved.
Detection of malicious requests aimed at disrupting the availability of cyber-physical systems
Authors: Iskhakova Anastasia
Published: January 2024

The work is devoted to solving the problem of algorithmization of the security management processes of cyber-physical systems by detecting malicious requests aimed at disrupting the availability of management interfaces. Particular attention is paid to attacks aimed at denial of service of cyber-physical systems by sending HTTP-flood to web management interfaces. This paper proposes algorithmic provision for comprehensive adaptive analysis of incoming requests. The proposed algorithm for the detection of malicious requests analyses the activity of the investigated components of the cyber-physical system's web service at various network levels. The work applies a visual analysis and data processing method based on the representation as a single normalized set. The raw data of the analysed queries is grouped in a special way to detect a particular anomaly as a suspected threat. Examples of data changes and security responses are given. The experimental results confirm that the proposed algorithmic software achieves first- and second-order error reduction compared to the commonly used regression models in modern application-layer firewalls. The results obtained can be applied to the further development of the theory of information security, in particular the information security of cyber-physical systems and systems of processing of especially protected confidential information.
Methodology for assessing the predicted didactic effects from the use of educational and training tools
Authors: Zhukov Aleksandr , Kalinin Timur , Kartsan Igor , Makarov Maksim , Karabitsina Ekaterina
Published: January 2024

The assessment of didactic effect is the most important in evaluating the effectiveness of training simulators. Modern methods of training specialists have shown that the most applicable at present is the step-by-step formation of skills and abilities. The methodology of obtaining the value of a complex indicator that takes into account the degree of influence of didactic possibilities realized in training simulators on the reduction of training time based on the methods of expert evaluation, the method of selecting the main component, convolution of single indicators into private ones and selection of the type of its function of a private indicator
Artificial intelligence's ability to process images
Authors: Magomedov Islam A. , Khafizova Amina Sh. , Ketova Fardiana R.
Published: January 2024

Penetration of technology into different fields and their dominion over them after a while is undoubtable. New technologies lure our souls and the dependency on them is inextricable once having tasted the fruit. We as a human easily addict to the convenient and comforting songs. As well as when they do our work for us in a more preferable and presentable way. This work was done to illustrate the artificial intelligence use in image processing. Its capabilities and issues are the key factors of the concerns of the work. Therefore, the work outlines the basic ideas behind artificial intelligence and its use in different areas and making accent on the capabilities of the technology when using tools powered by artificial intelligence to understand the meaning of the provided picture. Possible solutions are also described.
Application of the evolutionary approach to structural and parametric identification of dynamic objects
Authors: Karaseva Tatiana
Published: January 2024

The paper examines the evolutionary approach to structural and parametric identification of dynamic systems in the form of differential equations. The approach is based on a genetic programming algorithm to determine a structure of the equation and differential evolution method for parameters selection. The author proposed approach based on such evolutionary algorithms as genetic programming and differential evolution. The search for the structure is carried out by genetic programming. The selection of numerical parameters and initial conditions is implemented by a method of differential evolution. The problem of finding a model that describes changes in the efficiency of a hydraulic system is solved with the help of this approach. The proposed approach is compared with a recurrent neural network and a nonparametric kernel regression estimation.
The comparison of different PDP-type self-adaptive schemes for the cooperation of GA, DE, and PSO algorithms
Authors: Sopov Anton , Karaseva Tatiana
Published: January 2024

Many global optimization problems are presented as a black-box model, in which there is no information on the objective function properties. Traditional optimization algorithms usually can't effectively solve that kind of problems. Different heuristics and metaheuristics are usually applied in that case. Evolutionary algorithms are one of the most popular and effective approaches to black-box optimization problems. However, it's hard to choose one specific method that will solve the given problem better than other algorithms. For dealing with this issue, self-adaptive schemes are usually implemented. In this paper we have investigated the performance of different PDP-type adaptive schemes using such popular evolutionary-based algorithms as Genetic Algorithm, Differential Evolution, and Particle Swarm Optimization. The experimental results on a set of benchmark problems have shown that investigated schemes can improve the performance compared with the performance of a stand-alone evolutionary algorithm. At the same time the choice of a scheme and its parameters affect the results.
Nichtsuizidales selbstverletzendes Verhalten in der KJP
Authors: Bohle Frederik
Published: January 2024

Bei nichtsuizidalem selbstverletzendem Verhalten kann es zu schwerwiegenden Verletzungen mit erheblicher Gefährdung kommen. Die Sicherheit und das Sicherheitsgefühl sowie die körperliche Unversehrtheit der Betroffenen sind stark bedroht 1. Für die Pflege ist es daher sehr bedeutsam, fachkundig damit umzugehen.
Stimmenhören: Fluch oder Segen?
Authors: Ommer Daniel , Stellberg-Sönchen Laura , Wabnitz Pascal
Published: January 2024

Die traditionelle Behandlungsweise des Phänomens „Stimmenhören“ wird seit Ende der 1990er-Jahre in zahlreichen Publikationen infrage gestellt. Wurde bis dahin das „Stimmenhören“ als rein psychopathologisches Symptom im Rahmen akustischer Halluzinationen eingeordnet, so fokussieren neuere Publikationen mehr auf die intrapersonelle Perspektive und Bedeutung des Stimmenhörens. Im Zentrum steht die Frage, wie Menschen, die selbst Stimmen hören, diese – gegebenenfalls sinnstiftend – einordnen und biografisch verorten. Wir stellen das Ergebnis einer naturalistischen Forschungsarbeit vor, in der vier Menschen, die in einer psychiatrischen Institutsambulanz behandelt wurden, berichten, wie sich das Stimmenhören auf ihr Leben auswirkt.
Das Gesundheitsdatennutzungsgesetz – Potenziale für
die elektronische Patientenakte?
Authors: Falkai Peter
Published: January 2024

Aus Gründen der besseren Lesbarkeit wird auf die gleichzeitige Verwendung der
Sprachformen männlich, weiblich und divers (m/w/d)
verzichtet. Sämtliche Personenbezeichnungen gelten gleichermaßen
für alle Geschlechter.
Hirnmetastasen
Authors: Schulz Christian , Proescholdt Martin , Schmidt Nils Ole , Steger Felix , Heudobler Daniel
Published: January 2024

Zerebrale Metastasen bei Patienten mit Lungenkarzinom im Stadium der Metastasierung finden sich bereits bei mehr als 30% Patienten zum Zeitpunkt der Erstdiagnose und manifestieren sich im Verlauf der Erkrankung bei 2 von 3 Patienten. Die zerebrale Krankheitsmanifestation wurde lange Zeit als prognostisch ungünstig eingestuft. Betroffene Patienten wurden regelhaft von Therapiestudien unter Berücksichtigung der ungünstigen Prognose ausgeschlossen. Im Kontext zielgerichteter molekularer Therapiestrategien und etablierter immunonkologischer Systemtherapien stellt die Blut-Hirn-Schranke mittlerweile keine unüberwindbare Barriere mehr dar. Die Therapie von Hirnmetastasen erfordert aber stets die Betreuung in einem interdisziplinären Team und muss als Zentrumsaufgabe angesehen werden. Unter Berücksichtigung von Anzahl, Größe und Lokalisation der Hirnmetastasen, Neurologie und Allgemeinzustand, Komorbiditäten, potenzieller Lebenserwartung und Wunsch des Patienten, aber auch Tumorbiologie inklusive molekularer Veränderungen, extrakranieller Tumorlast und Verfügbarkeit einer ZNS-wirksamen Therapie erfolgt die differenzierte Therapieentscheidung. Hierbei werden mittlerweile häufig Systemtherapien sowie lokale neurochirurgische und strahlentherapeutische Therapiekonzepte kombiniert im Sinne optimierter und prognoseverbessernder Therapiestrategien.