bluuebunny/crossref_metadata_2025_split huggingface dataset:
The RpTOE1-RpFT Module Is Involved in Rejuvenation during Root-Based Vegetative Propagation in Robinia pseudoacacia
Authors: Zhang Zijie , Liu Jie , Cao Sen , Guo Qi , Sun Yuhan , Niu Dongsheng , Long Cui , Fan Yingming , Li Yun 
Published: May 2022

Vegetative propagation is an important method of reproduction and rejuvenation in horticulture and forestry plants with a long lifespan. Although substantial juvenile clones have been obtained through the vegetative propagation of ornamental plants, the molecular factors that regulate rejuvenation during vegetative propagation are largely unknown. Here, root sprouting and root cutting of Robinia pseudoacacia were used as two vegetative propagation methods. From two consecutive years of transcriptome data from rejuvenated seedlings and mature trees, one gene module and one miRNA module were found to be specifically associated with rejuvenation during vegetative propagation through weighted gene co-expression network analysis (WGCNA). In the gene module, a transcription factor-encoding gene showed high expression during vegetative propagation, and it was subsequently named RpTOE1 through homology analysis. Heterologous overexpression of RpTOE1 in wild-type Arabidopsis and toe1 toe2 double mutants prolonged the juvenile phase. The qRT-PCR results predicted RpFT to be a downstream gene that was regulated by RpTOE1. Further investigation of the protein-DNA interactions using yeast one-hybrid, electrophoretic mobility shift, and dual luciferase reporter assays confirmed that RpTOE1 negatively regulated RpFT by binding directly to the TOE binding site (TBS)-like motif on its promoter. On the basis of these results, we showed that the high expression of RpTOE1 during vegetative propagation and its inhibition of RpFT played a key role in the phase reversal of R. pseudoacacia.
Un aperçu de la politique de l’or d’Octavien Auguste : l’émission triumvirale RIC I² Augustus 273
Authors: Suspène Arnaud 
Published: May 2022

Cet article repose sur une nouvelle étude numismatique des aurei RIC I²
Augustus 273. Les données techniques de l’émission (corpus, étude de coins, métrologie, typologie) permettent de renouveler l’interprétation historique de ces monnaies. Cette interprétation conduit à identifier une possible référence à Claudius Marcellus dans la communication politique d’Octavien à la suite de la reconquête de la Sicile.
Intrusion Detection in Smart Homes: A pretest-posttest study of learning modalities for improved Cyber Situational Awareness
Authors: McDermott Christopher D. , Nicho Mathew , Isaacs John P. 
Published: May 2022

<p>Smart homes are becoming increasingly more com- plex and difficult to defend. This paper explores how humans can interact with intelligent virtual agents to improve their awareness and detection of threats in smart homes. Mica Endsley’s situa- tional awareness (SA) model was adopted and used to assess how participants <em>perceive </em>device activity, <em>comprehend </em>this in the context of their environment, and <em>project </em>this knowledge to detect if a threat exists. A pretest-posttest study demonstrated a statistically significant improvement in accuracy and efficiency when detecting threats using the conversational agents. In addi- tion, a qualitative approach was also taken to examine usability in relation to a users preferred learning modality. Participants reported being more confident at detecting threats across the three elements of the SA model when using the conversational agents as part of a multi-modal approach. </p>
RISK ANALYSIS BY MEANS OF A MUSICAL PREFERENCE INFORMATION MAP
Authors: Сердечный Алексей Леонидович , Коденцева Наталья Геннадиевна , Петелин Андрей Алексеевич , Лемешко Анастасия Андреевна , Руженко Валерия Евгеньевна 
Published: May 2022

Роль количественной оценки рисков является ключевой в обоснованном принятии решений в отношении разработки мер защиты. Однако одного лишь интегрального значения, которое характеризует уровень опасности тех или иных видов угроз, недостаточно для полного понимания процессов, связанных с негативными воздействиями на защищаемые объекты. Отображение значений риска с помощью информационной карты позволяет не только оценить, но и «увидеть» уровень опасности с учётом особенностей «ландшафта» защищаемой системы. В настоящей работе демонстрируется реализация данной идеи на примере анализа риска вовлечения пользователей социальных сетей в группы единой тематики. Для расчёта риска используются сведения о музыкальных исполнителях, которых слушают пользователи социальной платформы ВКонтакте, состоящие в группах единой тематики. Для наглядно представления значений риска вовлечения пользователя в группу единой тематики в отношении каждого музыкального исполнителя проводится расчёт частных показателей риска, которые отображаются на информационной карте музыкальных предпочтений. Для её построения использованы данные рекомендательной системы музыкального сервиса Яндекс.Музыка. Также в статье продемонстрирована возможность использования информационных карты музыкальных предпочтений для составления и анализа профилей пользователей социальных платформ.
The role of quantitative risk assessment is key in informed decision-making regarding the development of protective measures. However, the integral value alone, which characterizes the danger level of any type threats, is not enough to fully understand the processes associated with negative impacts on protected objects. Imaging risk values using an information map allows not only to assess, but also to "see" the danger level, taking into account the features of the protected system landscape. This paper demonstrates the implementation of this idea by analyzing the risk of involving social network users in groups of the single theme. To calculate the risk, information is used about musical artists who are listened to by users of the VK social platform who are in groups of the single theme. In order to visually represent the values of the risk of involving the user in a group of the single theme, for each musical artist, the calculation of private risk indicators is carried out, which are displayed on the music map. To build it, data from the recommendation system of the Yandex.Music music service were used. The article also demonstrates the possibility of using a music map for compiling and analyzing users profiles of social platforms.
THE STATE OF PRO-INFLAMMATORY MARKERS IN PATIENTS WITH METABOLIC DISORDERS CAUSED BY OBESITY BEFORE AND AFTER BARIATRIC SURGERY
Authors: Lavryk A. S. , Lavryk O. A. , Lytvynchuk H. M. 
Published: May 2022

Aim. To study the effect of bariatric surgery on pro-inflammatory markers and to study the mechanisms of changes in their concentration in the postoperative period with a decrease in the mass of adipose tissue.
Material and methods. The work is based on the results of surgical treatment of patients with MO (aged 18 to 62 years, with an average BMI of (50.8 +8.5) kg/m2) who underwent bariatric surgery at the National Institute of Surgery and Transplantology of the National Academy of Medical Sciences of Ukraine. In the postoperative period, the following parameters were measured: C-reactive protein, sialic acid and seromucoid at 1, 3, 6 and 12 months after surgery.
Results and discussion. The SRP concentration decreased significantly already during the first 3 months. in all groups: SRP after BSH was — (96±12.6) mg/l, which is 2 times lower than the initial level, after IR — (98±21.6) mg/l, which is 1.2 times lower than the initial level, after BPS — (128±18.6) mg/l, which was 1.3 times lower than the initial level. After 12 months. SRP was (62±10.8) mg/l, which was 3 times lower than the initial level, after IR — (46±8.4) mg/l, 3 times lower than the initial level, after BPH — (36±13.2) mg/l, which was 5 times lower than the initial level.
Sialic acid levels at 6 months. was: after BPSh — (2.4±0.9) Od., after IR — (2.7±0.3) Od after BPSH — (2.6±0.5) Units. After 12 months. the level of sialic acids remained in the upper limit of the norm and were: after BSh — (2.7±0.5) Odes after IR — (2.5±0.7) Odes after BSA — (2.6±0.5) Units.
The seromucoid concentration was the highest before surgery in the CI and BPS groups and amounted to (0.4±0.2) and (0.3±0.2) Compared with (0.2±0.2) in the BPS group. Within 3–6 months. after the operation, the concentration of seromucoid was in the upper limit of the norm.
Conclusions. The reduction in body weight achieved after bariatric surgery leads to the normalization of pro-inflammatory status, which forms the pathogenetic basis for neutralizing the systemic inflammation observed in obesity. These indicators are reliable evidence of a decrease in the intensity or cessation of inflammatory and destructive processes that develop in obese patients.
Primer sezaryen olan hastalarda uterin insizyonun tek kat ya da çift kat onarım tekniklerinin transvajinal ultrasonografi ile karşılaştırılması
Authors: ÇALIŞKAN ŞENAY Zümrüt , ÜSTÜNYURT Emin 
Published: May 2022

ÖZET
Amaç: İlk kez sezaryen operasyonu (primer sezaryen) yapılan olgularda, tek kat ve çift kat sütürasyon tekniği kullanılarak kapatılan uterusun, rezidüel miyometriyal kalınlık ve sezaryen skar defekti açısından karşılaştırılmasını amaçladık.
Gereçler ve Yöntem: Çalışmaya Mart 2016 ile Mayıs 2016 tarihleri arasında, Bursa Yüksek İhtisas Eğitim ve Araştırma Hastanesi’nde, 18-45 yaş arası, gestasyonel yaşı 37 hafta ve üzeri olup primer sezaryen geçirecek 102 hasta dahil edildi. 51 hastada kilitlemeli tek kat ve 51 hastada kilitlemesiz çift kat tekniği ile uterin insizyon sütüre edildi. Çalışma popülasyonunda postoperatif 6. haftada yapılan transvajinal ultrasonografi ile mevcut skar dokusunun derinliği ve genişliği, kalan miyometriyum dokusunun kalınlığı ve uterusun pozisyonu değerlendirildi.
Bulgular: Çift kat tekniği kullanılan grupta sütürasyon süresi tek kat tekniği kullanılan gruba göre istatistiksel açıdan anlamlı olarak uzundu (p
Nature of Supersonic Turbulence and Density Distribution Function in the Multiphase Interstellar Medium
Authors: Kobayashi Masato I. N. , Inoue Tsuyoshi , Tomida Kengo , Iwasaki Kazunari , Nakatsugawa Hiroki 
Published: May 2022

Abstract
Supersonic flows in the interstellar medium (ISM) are believed to be a key driver of the molecular cloud formation and evolution. Among molecular clouds’ properties, the ratio between the solenoidal and compressive modes of turbulence plays important roles in determining the star formation efficiency. We use numerical simulations of supersonic converging flows of the warm neutral medium (WNM) resolving the thermal instability to calculate the early phase of molecular cloud formation, and we investigate the turbulence structure and the density probability distribution function (density PDF) of the multiphase ISM. We find that both the solenoidal and compressive modes have their power spectrum similar to the Kolmogorov spectrum. The solenoidal (compressive) modes account for ≳80% (≲20%) of the total turbulence power. When we consider both the cold neutral medium (CNM) and the thermally unstable neutral medium (UNM) up to T ≲ 400 K, the density PDF follows the lognormal distribution, whose width

σ

s

is well explained by the known relation from the isothermal turbulence as

σ

s

=
ln
(
1

+

b

2



2

)

(where b is the parameter representing the turbulence mode ratio and



is the turbulent Mach number). The density PDF of the CNM component alone (T ≤ 50 K), however, exhibits a narrower

σ

s

by a factor of ∼2. These results suggest that observational estimations of b based on the CNM density PDF requires the internal turbulence within each CNM clump but not the interclump relative velocity, the latter of which is instead powered by the WNM/UNM turbulence.
Spectroscopic Studies of Type Ia Supernovae Using LSTM Neural Networks
Authors: Hu Lei , Chen Xingzhuo , Wang Lifan 
Published: May 2022

Abstract
We present a data-driven method based on long short-term memory (LSTM) neural networks to analyze spectral time series of Type Ia supernovae (SNe Ia). The data set includes 3091 spectra from 361 individual SNe Ia. The method allows for accurate reconstruction of the spectral sequence of an SN Ia based on a single observed spectrum around maximum light. The precision of the spectral reconstruction increases with more spectral time coverages, but the significant benefit of multiple epoch data at around optical maximum is only evident for observations separated by more than a week. The method shows great power in extracting the spectral information of SNe Ia and suggests that the most critical information of an SN Ia can be derived from a single spectrum around the optical maximum. The algorithm we have developed is important for the planning of spectroscopic follow-up observations of future SN surveys with the LSST/Rubin and WFIRST/Roman telescopes.
Mutual Inclination of Ultra-short-period Planets with Time-varying Stellar J
2 Moments
Authors: Chen Chen , Li Gongjie , Petrovich Cristobal 
Published: May 2022

Abstract
Systems with ultra-short-period (USP) planets tend to possess larger mutual inclinations compared to those with planets located farther from their host stars. This could be explained due to precession caused by stellar oblateness at early times when the host star was rapidly spinning. However, stellar oblateness reduces over time due to the decrease in the stellar rotation rate, and this may further shape the planetary mutual inclinations. In this work, we investigate in detail how the final mutual inclination varies under the effect of a decreasing J
2. We find that different initial parameters (e.g., the magnitude of J
2 and planetary inclinations) will contribute to different final mutual inclinations, providing a constraint on the formation mechanisms of USP planets. In general, if the inner planets start in the same plane as the stellar equator (or coplanar while misaligned with the stellar spin axis), the mutual inclination decreases (or increases then decreases) over time due to the decay of the J
2 moment. This is because the inner orbit typically possesses less orbital angular momentum than the outer ones. However, if the outer planet is initially aligned with the stellar spin while the inner one is misaligned, the mutual inclination nearly stays the same. Overall, our results suggest that either USP planets formed early and acquired significant inclinations (e.g., ≳30° with its companion or ≳10° with its host star spin axis for Kepler-653 c) or they formed late (≳Gyr) when their host stars rotated slower.
Postexplosion Positive Jet-feedback Activity in Inner Ejecta of Core Collapse Supernovae
Authors: Akashi Muhammad , Soker Noam 
Published: May 2022

Abstract
We conduct three-dimensional hydrodynamical simulations of weak jets that we launch into a core collapse supernova (CCSN) ejecta half an hour after the explosion and find that the interaction of the fast jets with the CCSN ejecta creates high-pressure zones that induce a backflow that results in mass accretion onto the newly born neutron star. In cases of weak jets, with a total power of ≈1045–1046 erg, the backflow mass accretion might power them up to more energetic jets by an order of magnitude. In total, the jets of the two postexplosion jet-launching episodes have enough energy to influence the morphology of the very inner ejecta, with a mass of ≈0.1 M
⊙. Our results imply that in some, probably a minority of, CCSN remnants the very inner regions might display a bipolar structure that results from postexplosion weak jets. The regions outside this part might display the morphology of jittering jets.
Diagnostics of Non-Maxwellian Electron Distributions in Solar Active Regions from Fe xii Lines Observed by the Hinode Extreme Ultraviolet Imaging Spectrometer and Interface Region Imaging Spectrograph
Authors: Del Zanna G. , Polito V. , Dudík J. , Testa P. , Mason H. E. , Dzifčáková E. 
Published: May 2022

Abstract
We present joint Hinode Extreme Ultraviolet Imaging Spectrometer (EIS) and Interface Region Imaging Spectrograph (IRIS) observations of Fe xii lines in active regions, both on-disk and off-limb. We use an improved calibration for the EIS data, and find that the 192.4 Å/1349 Å observed ratio is consistent with the values predicted by CHIANTI and the coronal approximation in quiescent areas, but not in all active-region observations, where the ratio is often lower than expected by up to a factor of about two. We investigate a number of physical mechanisms that could affect this ratio, such as opacity and absorption from cooler material. We find significant opacity in the EIS Fe xii 193 and 195 Å lines, but not in the 192.4 Å line, in agreement with previous findings. As we cannot rule out possible EUV absorption by H, He, and He ii in the on-disk observations, we focus on an off-limb observation where such absorption is minimal. After considering these, as well as possible nonequilibrium effects, we suggest that the most likely explanation for the observed low Fe xii 192.4 Å/1349 Å ratio is the presence of non-Maxwellian electron distributions in the active regions. This is in agreement with previous findings based on EIS and IRIS observations independently.
Can Carbon Fractionation Provide Evidence for Aerial Biospheres in the Atmospheres of Temperate Sub-Neptunes?
Authors: Glidden Ana , Seager Sara , Huang Jingcheng , Petkowski Janusz J. , Ranjan Sukrit 
Published: May 2022

Abstract
The search for signs of life on other worlds has largely focused on terrestrial planets. Recent work, however, argues that life could exist in the atmospheres of temperate sub-Neptunes. Here we evaluate the usefulness of carbon dioxide isotopologues as evidence of aerial life. Carbon isotopes are of particular interest, as metabolic processes preferentially use the lighter 12C over 13C. In principle, the upcoming James Webb Space Telescope (JWST) will be able to spectrally resolve the 12C and 13C isotopologues of CO2, but not CO and CH4. We simulated observations of CO2 isotopologues in the H2-dominated atmospheres of our nearest (<40 pc), temperate (equilibrium temperature of 250–350 K) sub-Neptunes with M-dwarf host stars. We find 13CO2 and 12CO2 distinguishable if the atmosphere is H2 dominated with a few percentage points of CO2 for the most idealized target with an Earth-like composition of the two most abundant isotopologues, 12CO2 and 13CO2. With a Neptune-like metallicity of 100× solar and a C/O of 0.55, we are unable to distinguish between 13CO2 and 12CO2 in the atmospheres of temperate sub-Neptunes. If atmospheric composition largely follows metallicity scaling, the concentration of CO2 in a H2-dominated atmosphere will be too low to distinguish CO2 isotopologues with JWST. In contrast, at higher metallicities, there will be more CO2, but the smaller atmospheric scale height makes the measurement impossible. Carbon dioxide isotopologues are unlikely to be useful biosignature gases for the JWST era. Instead, isotopologue measurements should be used to evaluate formation mechanisms of planets and exosystems.
Magnetic Discontinuities in the Solar Wind and Magnetosheath: Magnetospheric Multiscale Mission (MMS) Observations
Authors: Liu Y. Y. , Fu H. S. , Cao J. B. , Wang Z. , He R. J. , Guo Z. Z. , Xu Y. , Yu Y. 
Published: May 2022

Abstract
We perform a statistical investigation of the geometric features of interplanetary discontinuities (IDs) in the near-Earth solar wind and magnetosheath, by utilizing 14 months of Magnetospheric Multiscale mission data. 117,669 IDs are collected, including 108,049 events in the solar wind and 6399 events in the magnetosheath, with the remnant in the magnetosphere or near the bow shock/magnetopause. We find the following: (1) the ID occurrence rate is 17.0 events hr−1 in the solar wind and 5.5 events hr−1 in the magnetosheath, (2) the field rotation angles during ID crossings in the magnetosheath exhibit a two-exponential distribution with a breakpoint at 50°, which is not observed for IDs in the solar wind, (3) the magnetosheath IDs with small field rotation angles tend to be clustered, (4) by classifying the IDs into rotational discontinuities (RDs), tangential discontinuities (TDs), either TDs or RDs (EDs), and neither TDs nor RDs (NDs), we estimate RD:TD:ED:ND = 68%:5%:20%:7% in the solar wind, and RD:TD:ED:ND = 15%:44%:18%:23% in the magnetosheath, (5) the occurrence rates of RDs and TDs are, respectively 7.95 and 0.58 events hr−1 in the solar wind, and 0.57 and 1.60 events hr−1 in the magnetosheath, (6) RDs are more likely to propagate antisunward in the plasma rest frame, especially in the magnetosheath, and (7) the average thicknesses of the RDs and TDs are estimated, respectively, as 10.4 and 8.1 proton gyroradii (r

p
) in the solar wind, and 17.4 and 5.0 r

p
in the magnetosheath. This work can improve our understanding of IDs’ interaction with the terrestrial bow shock.
Effects of Magnetic Field Orientations in Dense Cores on Gas Kinematics in Protostellar Envelopes
Authors: Gupta Aashish , Yen Hsi-Wei , Koch Patrick , Bastien Pierre , Bourke Tyler L. , Chung Eun Jung , Hasegawa Tetsuo , Hull Charles L. H. , Inutsuka Shu-ichiro , Kwon Jungmi , Kwon Woojin , Lai Shih-Ping , Lee Chang Won , Lee Chin-Fei , Pattle Kate , Qiu Keping , Tahani Mehrnoosh , Tamura Motohide , Ward-Thompson Derek 
Published: May 2022

Abstract
Theoretically, misalignment between the magnetic field and rotational axis in a dense core is considered to be dynamically important in the star formation process; however, the extent of this influence remains observationally unclear. For a sample of 32 Class 0 and I protostars in the Perseus Molecular Cloud, we analyzed gas motions using C18O data from the SMA MASSES survey and the magnetic field structures using 850 μm polarimetric data from the JCMT BISTRO-1 survey and archive. We do not find any significant correlation between the velocity gradients in the C18O emission in the protostellar envelopes at a 1000 au scale and the misalignment between the outflows and magnetic field orientations in the dense cores at a 4000 au scale, and there is also no correlation between the velocity gradients and the angular dispersions of the magnetic fields. However, a significant dependence on the misalignment angles emerges after we normalize the rotational motion by the infalling motion, where the ratios increase from ≲1 to ≳1 with increasing misalignment angle. This suggests that the misalignment could prompt angular momentum transportation to the envelope scale but is not a dominant factor in determining the envelope rotation, and other parameters, such as mass accretion in protostellar sources, also play an important role. These results remain valid after taking into account projection effects. The comparison between our estimated angular momentum in the protostellar envelopes and the sizes of the known protostellar disks suggests that significant angular momentum is likely lost between radii of ∼1000 and 100 au in protostellar envelopes.
Critically Evaluated Spectral Data for Singly Ionized Carbon (C ii)
Authors: Kramida A. , Haris K. 
Published: May 2022

Abstract
All available experimental data on the spectrum of singly ionized carbon have been critically analyzed. Measurement uncertainties of all published studies have been reassessed. The scope of observational data includes laboratory emission spectra of arcs, sparks, electrodeless discharges, and hollow cathode lamps recorded with grating and Fourier transform spectrometers, laboratory photoabsorption spectra, and emission spectra of planetary nebulae. The total number of observed spectral lines included in this compilation is 597. These lines participate in 972 transitions. From this list of identified transitions, we have derived a set of 414 energy levels, which are optimized using a least-squares fitting procedure. The identifications are supported by parametric calculations with Cowan’s codes. The existing tables of critically evaluated transition probabilities have been extended with our newly calculated data. The ionization energy has been derived from the newly optimized energy levels with improved precision. Data on the isotope shifts and hyperfine structure have also been compiled.