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SXP 15.6  is a recently established Be star X-ray binary system in the Small Magellanic Cloud (SMC). Like many such systems, the variable X-ray emission is driven by the underlying behaviour of the mass donor Be star. It is shown here that the neutron star in this system is exceptionally close to spin equilibrium averaged over several years, with the angular momentum gain from mass transfer being almost exactly balanced by radiative losses. This makes SXP 15.6 exceptional compared to all other known members of its class in the SMC, all of whom exhibit much higher spin period changes. In this paper, we report on X-ray observations of the brightest known outburst from this system. These observations are supported by contemporaneous optical and radio observations, as well as several years of historical data. [ABSTRACT FROM AUTHOR]

This paper analyzes the incidence in our country of the recommendations provided by the OECD in its Guide on the implications of the COVID-19 Pandemic on transfer pricing Guidance on the transfer pricing implications of the COVID-19 pandemic published on December 18, 2020 and which represents the consensus perspective of the more than 137 members of the BEPS Inclusive Framework, among which is Peru, regarding the application of the arm's length principle for problems generated or exacerbated by the pandemic. In particular, the problem of comparability analysis is evaluated in a scenario of lack of comparable transactions and companies in the 2020 and subsequent years affected by the pandemic. Likewise, the issue of losses is addressed from two perspectives, those as a comparable result and the generation of losses in business models with limited risk. It is concluded that several of the measures recommended by the Inclusive Framework can be materialized through the flexibility and openness of the Tax Administration in audits; however, allowing the modification of the transfer pricing analysis reflected in the Local Report based on information of comparable companies obtained later requires the issuance of a legal norm that does not condition the rectifying return to the verification of SUNAT and temporarily avoid the application of infractions and sanctions for the declaration of false data. [ABSTRACT FROM AUTHOR]

We present new spectroscopic observations of the Be/black hole binary MWC 656 obtained during the period 2015–2021. We measure the equivalent width of Hα (EWα), Hβ (EWβ$$ {EW}_{\beta } $$), and the distance between the peaks of Hα (ΔVα$$ \Delta {V}_{\alpha } $$), Hβ (ΔVβ$$ \Delta {V}_{\beta } $$), and FeII (ΔVFeII$$ \Delta {V}_{\mathrm{FeII}} $$) lines. Combining new and old data, we find that: (1) the density of the circumstellar disc of MWC 656 (ΔVα$$ \Delta {V}_{\alpha } $$ versus EWα$$ {EW}_{\alpha } $$ diagram) is similar to the Be stars. For the Be stars, we find the relation ΔVβ=0.999ΔVα+62.4$$ \Delta {V}_{\beta }=0.999\Delta {V}_{\alpha }+62.4 $$ km s−1, and the position of MWC 656 corresponds to the average behavior of the Be stars. This means that the presence of the black hole does not change the overall structure of the circumstellar disc; (2) the periodogram analysis indicates modulation of EWα$$ {EW}_{\alpha } $$ with a period 60.4±0.4$$ 60.4\pm 0.4 $$ days, which is identical to the binary orbital period. The maxima of EWα$$ {EW}_{\alpha } $$ and EWβ$$ {EW}_{\beta } $$ are around periastron (phase zero); (3) around orbital phase zero, ΔVβ$$ \Delta {V}_{\beta } $$ and ΔVFeII$$ \Delta {V}_{FeII} $$ decrease by about 30$$ 30 $$ km s−1. This suggests that we observe an increase of the circumstellar disc size induced by the periastron passage of the black hole and that the entire circumstellar disc pulsates with the orbital period with relative amplitude of 10–20%. The observations also indicate, that the reason for the black hole in MWC 656 to be in deep quiescence is a very low efficiency of accretion (∼2×10−6$$ \sim 2\times {10}^{-6} $$). [ABSTRACT FROM AUTHOR]

Copyright of Verimlilik Dergisi is the property of Verimlilik Dergisi and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Roxana Chis,1 Simon Hew,2 Wilma Hopman,3 Lawrence Hookey,2 Robert Bechara2 1Division of Internal Medicine, Kingston Health Sciences Centre, Queen’s University, Kingston, Ontario, Canada; 2Division of Gastroenterology, Kingston Health Sciences Centre, Queen’s University, Kingston General Hospital, Kingston, Ontario, Canada; 3Research Institute, Kingston Health Sciences Centre, Queen’s University, Kingston, Ontario, CanadaCorrespondence: Robert BecharaDivision of Gastroenterology, Queens University, Kingston Health Sciences Center, 166 Brock Street, Kingston, Ontario K7L1A8, CanadaTel + 613 544 3400Email bechara.robert@gmail.comPurpose: Patients with Barrett’s esophagus (BE) undergo surveillance endoscopies to assess for pre-cancerous changes. We developed a simple endoscopic classification method for predicting non-dysplastic BE (NDBE), low-grade dysplasia (LGD)/indefinite for dysplasia (ID) and high-grade dysplasia (HGD)/early esophageal adenocarcinoma (EAC).Patients and Methods: Twenty-two patients with BE underwent endoscopy using the PENTAX Medical MagniView gastroscope and OPTIVISTA processor. Sixty-six video-still images were analyzed to characterize the microsurface, microvasculature and the presence of a demarcation line. Class A was characterized by regular microvascular and microsurface patterns and absence of a demarcation line, class B by changes in the microvascular and/or microsurface patterns compared to the background mucosa with presence of a demarcation line, and class C by irregular microvascular and/or irregular microsurface patterns with presence of a demarcation line.Results: Of the class A images, 97.9% were NDBE. For class B, 69.2% were LGD/ID and 30.8% NDBE. One hundred percent of the class C samples were HGD/EAC. The sensitivity of our classification system was 93.8%, specificity 92%, positive predictive value 78.9%, negative predictive value 97.9% and an accuracy 92.4%.Conclusion: In this study, we developed a simple classification system for the prediction of NDBE, LGD/ID and HGD/EAC. Its real-time clinical applicability will be validated prospectively.Keywords: Barrett’s esophagus, BE, dysplasia, enhanced endoscopy, esophageal adenocarcinoma

Z Canis Majoris is a fascinating early-type binary with a Herbig Be primary and a FU Orionis-type secondary. Both of the stars exhibit sub-arcsecond jet-like ejecta. In addition, the primary is associated with the extended jet as well as with the large-scale outflow. In this study, we investigate further the nature of the large-scale outflow, which has not been studied since its discovery almost three and a half decades ago. We present proper motion measurements of individual features of the large-scale outflow and determine their kinematical ages. Furthermore, with our newly acquired deep images, we have discovered additional faint arc-shaped features that can be associated with the central binary.

The Li(p,n) and Be(p,n) reactions are widely used as accelerator-based neutron sources for boron neutron capture therapy (BNCT). Because the energy of the neutrons produced by these reactions is high for BNCT, a moderator is required to reduce the energy to the epithermal energy region. The neutron yields and energy spectra derived from the Li(p,n) and Be(p,n) reactions vary with the incident proton energy; a high proton energy results in a high neutron yield. However, a high proton energy can also increase the neutron energy, and in this case, a high neutron energy requires a thick moderator, which decreases the epithermal neutron flux. Notably, these tradeoffs are not completely clear. Furthermore, the upper limit of the epithermal neutron energy used in different BCNT facilities is not the same. Therefore, epithermal neutron flux estimation with applying an appropriate moderator is necessary for comparing epithernal neutron flux depending on the proton energy, target type, and epithermal neutron range definition. In this study, GEANT4 simulations were performed to determine effective moderator materials and thicknesses. After applying a moderator, we examined the epithermal neutron flux by changing the conditions that can influence the epithermal neutron flux, such as the proton energy, target species (Li and Be), and different definitions of the epithermal neutron region. The results showed that the epithermal neutron flux increases with the increasing proton energy until a certain level for both Li and Be targets. For proton energies above 3 MeV for the Li target and above 7 MeV for the Be target, the epithermal neutron flux decreases or its increase rate gradually decreases. And, when the upper energy limit of the epithermal neutron range is changed from 10 keV to 20 keV or 40 keV, the epithermal neutron flux is more than 109 cm−2 s−1 at a proton energy of 3 MeV for Li target and 8 MeV for Be target. • Neutron generation yields and energy spectra from Li(p,n) and Be(p,n) reaction were obtained through GEANT4 simulations. • The combination of MgF 2 and TiF 3 showed a suitable moderator for obtaining epithermal neutrons. • We examined the changes in f epi depending on the proton energy, target type(Li and Be), and epithermal neutron range definition. [ABSTRACT FROM AUTHOR]

The evolutionary status of Be-type stars remains unclear, with both single-star and binary pathways having been proposed. Here, VFTS spectroscopy of 73 Be-type stars, in the spectral-type range, B0–B3, is analysed to estimate projected rotational velocities, radial velocities, and stellar parameters. They are found to be rotating faster than the corresponding VFTS B-type sample but simulations imply that their projected rotational velocities are inconsistent with them all rotating at near critical velocities. The de-convolution of the projected rotational velocities estimates leads to a mean rotational velocity estimate of 320–350 km s−1, approximately 100 km s−1 larger than that for the corresponding B-type sample. There is a dearth of targets with rotational velocities less than 0.4 of the critical velocity, with a broad distribution reaching up to critical rotation. Our best estimate for the mean or median of the rotational velocity is 0.68 of the critical velocity. Rapidly rotating B-type stars are more numerous than their Be-type counterparts, whilst the observed frequency of Be-type stars identified as binary systems is significantly lower than that for normal B-type stars, consistent with their respective radial-velocity dispersions. The semi-amplitudes for the Be-type binaries are also smaller. Similar results are found for a Small Magellanic Cloud Be-type sample centred on NGC 346 with no significant differences being found between the two samples. These results are compared with the predictions of single and binary stellar evolutionary models for Be-type stars. Assuming that a single mechanism dominated the production of classical Be-type stars, our comparison would favour a binary evolutionary history. [ABSTRACT FROM AUTHOR]

The Hα emission of a set of southern γ Cas stars was monitored since 2019, with the aim of detecting transition events and examining how their peculiar X-ray emission would react in such cases. Two stars, namely HD 119682 and V767 Cen, were found to display slowly decreasing disc emissions. These decreases were not perfectly monotonic and several temporary and limited rebuilding events were observed. For HD 119682, the emission component in Hα disappeared in 2020 mid-July. In X-rays, the X-ray flux was twice smaller than that recorded two decades ago but of a similar level as observed a decade ago. The X-ray flux decreased over the campaign by 30 per cent, but the hardness remained similar in data sets of all epochs. In particular, the γ Cas character remained as clear as before even when there was no trace of disc emission in the Hα line. For V767 Cen, the full disappearance of disc emission in Hα never occurred. We followed closely a disc rebuilding event, but no significant change in flux or hardness was detected. These behaviours are compared to those of other γ Cas stars and their consequences on the X-ray generation are discussed. [ABSTRACT FROM AUTHOR]

Luminous blue variables (LBVs) and B[e] supergiants (B[e]SGs) are some of the most massive stars that display extreme and puzzling behavior. Their rarity indicates that they belong to short evolutionary phases or short-lived phenomena in the post-main sequence evolution of massive stars. However, their strong mass loss and episodic mass eruptions may be crucially impacting massive star evolution. LBVs are a group of evolved massive stars that exhibit irregular variability and eruptive mass loss. Various subtypes, including S Doradus variables, giant eruptions, and pre-supernova outbursts, exist. The physical cause of the LBV phenomenon remains heavily debated. B[e]SGs have strong forbidden line emission and infrared excess from dust that are thought to arise in a circumstellar disk or torus. The formation mechanism of their disk-like structures is yet to be settled. The evolutionary phases of LBVs and B[e]SGs and their connection to other evolved massive stars are important unanswered questions in massive star evolution. [ABSTRACT FROM AUTHOR]

NGC 2004 #115 is a recently identified black hole (BH) candidate in the Large Magellanic Cloud (LMC) containing a B star orbiting an unseen companion in a 2.9 d orbit and a Be star tertiary. We show that the unseen companion is not a 25 M⊙ BH, but a |$(2\!-\!3)\, {\rm M}_{\odot }$| luminous star. Analysing the Optical Gravitational Lensing Experiment (OGLE) and MAssive Compact Halo Object (MACHO) light curves of the system, we detect ellipsoidal variability with amplitude 10 times larger than would be expected if the companion were a 25 M⊙ BH, ruling out the low inclination required for a massive companion. The light curve also shows a clear reflection effect that is well modelled with a |$2.5\, {\rm M}_{\odot }$| main-sequence secondary, ruling out a lower mass BH or neutron star companion. We consider and reject models in which the system is a binary containing a stripped star orbiting the Be star: only a triple model with an outer Be star can explain both the observed light curve and radial velocities. Our results imply that the B star, whose slow projected rotation velocity and presumed tidal synchronization were interpreted as evidence for a low inclination (and thus a high companion mass), is far from being tidally synchronized: despite being in a 2.9 d orbit that is fully or nearly circularized (e < 0.04), its surface rotation period appears to be at least 20 d. We offer cautionary notes on the interpretation of dormant BH candidates in binaries. [ABSTRACT FROM AUTHOR]

KIC 8264293 is a fast-rotating B-type pulsator observed by Kepler satellite. Its photometric variability is mainly due to pulsations in high-order g modes. Besides, we detected a weak H α emission. Thus, the second source of variability is the fluctuation in a disc around the star. The pulsational spectrum of KIC 8264293 reveals a frequency grouping and period spacing pattern. Here, we present the thorough seismic analysis of the star based on these features. Taking into account the position of the star in the HR diagram and fitting the 14 frequencies that form the period spacing, we constrain the internal structure of the star. We conclude that the star barely left the zero-age main sequence and the best seismic model has |$M = 3.54\, \mathrm{M}_{\odot }$|⁠ , |$V_\mathrm{rot}=248\, \mathrm{km\, s}^{-1}$|⁠ , and Z  = 0.0112. We found the upper limit on the mixing at the edge of the convective core, with the overshooting parameter up to f ov = 0.03. On the other hand, we were not able to constrain the envelope mixing for the star. To excite the modes in the observed frequency range, we had to modify the opacity data. Our best seismic model with an opacity increase by 100 per cent at the 'nickel' bump log  T  = 5.46 explains the whole instability. KIC 8264293 is the unique, very young star pulsating in high-order g modes with the Be feature. However, it is not obvious whether the source of this circumstellar matter is the ejection of mass from the underlying star or whether the star has retained its protostellar disc. [ABSTRACT FROM AUTHOR]

Contention is the main problem in optical burst switching (OBS) systems that lead to loss more burst by dropping the contended burst. To deal with this problem, we propose a new proactive method which is based on the integration of Real-Time Scheduling Techniques: Earliest-deadline-first (EDF) and round-robin (RR). Based on this consideration, this paper proposes a series of novel coherent interdependence methods to propose a novel OBS edge node Architecture: (i) An adaptive priority system to obtain QoS guarantees, (ii) Admission control and bandwidth distribution to maximize the link throughput. The proposed technique classifies the incoming data packets into two categories: granted service (GS) for high priority and best effort (BE) for low priority. The RR technique is used for scheduling different BE and GS packets when they have the same deadlines while the EDF is used to manage GS packets with different deadlines. In addition, the admission and bandwidth assignment policies vary in function of traffic characteristics. For GS traffic, only the bandwidth used is needed, while the remaining bandwidth is assigned to best effort traffic. With the EDF and RR scheduling algorithms, the proposed edge node design obtains a brand new architecture. The proposed OBS architecture has been tested for dynamic traffic in which both BE and GS traffic arrives according to a Poisson distribution for different scenarios based on traffic distribution and switch resources reservation. In scenario#1, 90% GS traffic and 10% BE traffic and reserve 7% of the switch resources for BE traffic are considered. Therefore, the proposed architecture provides a higher grade of service to the end-users with the guaranteed service level of agreements than the existing architecture that does not implement resource reservation protocols. In addition, the modified OBS-edge node is designed and implemented on FPGA Virtex-11C2V40. The hardware performance analysis shows that the network dimension is a key factor in latency measurement. A $2\times 2$ network dimension can serve approximately 230 Mbps throughput and approximately 400 Mbps in the case when the number of flits (segment of burst) is twice.

We report the discovery of 2 new Be stars, and re-identify one known Be starin the open cluster NGC 6830. Eleven H-alpha emitters were discovered using theH-alpha imaging photometry of the Palomar Transient Factory Survey. Stellarmembership of the candidates was verified with photometric and kinematicinformation using 2MASS data and proper motions. The spectroscopic confirmationwas carried out by using the Shane 3-m telescope at Lick observatory. Based ontheir spectral types, three H-alpha emitters were confirmed as Be stars withH-alpha equivalent widths > -10 Angstrom. Two objects were also observed by thenew spectrograph SED-Machine on the Palomar 60 inch Telescope. The SED-Machineresults show strong H-alpha emission lines, which are consistent with theresults of the Lick observations. The high efficiency of the SED-Machine canprovide rapid observations for Be stars in a comprehensive survey in thefuture.

The binary status of γ Cas stars has been discussed while theoretically examining the origin of their peculiar X-ray emission. However, except in two cases, no systematic radial velocity monitoring of these stars had been undertaken yet to clarify their status. We now fill this gap using TIGRE, CARMENES, and UVES high-resolution spectroscopy. Velocities were determined for 16 stars, revealing shifts and/or changes in line profiles. The orbit of six new binaries could be determined: the long periods (80–120 d) and small velocity amplitudes (5–7 km s−1) suggest low mass companions (0.6–1 M⊙). The properties of the known γ Cas binaries appear similar to those of other Be systems, with no clear-cut separation between them. One of the new systems is a candidate for a rare case of quadruple system involving a Be star. Five additional γ Cas stars display velocity variations compatible with the presence of companions, but no orbital solution could yet be formally established for them hence they only receive the status of 'binary candidate'. [ABSTRACT FROM AUTHOR]

B[e] supergiants have unusual circumstellar environments which may include thin, concentric rings displaying atomic line emission. GG Carinae is a B[e] supergiant binary which exhibits such a geometry in its circumbinary environment. We study atomic emission lines arising from GG Carinae's circumbinary disc in FEROS spectra collected between 1998 and 2015. We find that semiforbidden Fe  ii ] and permitted Ca  ii emission are formed in the same thin circumbinary ring previously reported to have forbidden [O  i ] and [Ca  ii ] emission. We find that there are two circumbinary rings orbiting with projected velocities of 84.6 ± 1.0 and 27.3 ± 0.6  |$\rm km\, s^{-1}$|⁠. Deprojecting these velocities from the line of sight, and using updated binary masses presented by Porter et al. (2021a), we find that the radii of the circumbinary rings are |$2.8^{+0.9}_{-1.1}$| and |$27^{+9}_{-10}$|  au for the inner ring and outer ring, respectively. We find evidence of subtle dynamical change in the inner circumbinary ring over the 17 yr spanned by the data, manifesting in variability in the ratio of the intensity of the blueshifted peak to the redshifted peak of its emission lines and the central velocity becoming more blueshifted. We perform smoothed-particle hydrodynamic simulations of the system which suggest that these observed changes are consistent with pumping of the eccentricity of a radially thin circumbinary ring by the inner binary. We find a systemic velocity of the GG Carinae system of −23.2 ± 0.4  |$\rm km\, s^{-1}$|⁠. [ABSTRACT FROM AUTHOR]

The observed orbits of emission-line stars may be affected by systematics owing to their broad emission lines being formed in complex and extended environments. This is problematic when orbital parameter probability distributions are estimated assuming radial-velocity data are solely comprised of Keplerian motion plus Gaussian white noise, leading to overconfident and inaccurate orbital solutions, with implications for the inferred dynamical masses and hence evolutionary models. We present a framework in which these systems can be meaningfully analysed. We synthesize benchmark data sets, each with a different and challenging noise formulation, for testing the performance of different algorithms. We make these data sets freely available with the aim of making model validation an easy and standardized practice in this field. Next, we develop an application of Gaussian processes to model the radial-velocity systematics of emission-line binaries, named marginalized |$\mathcal {GP}$|⁠. We benchmark this algorithm, along with current standardized algorithms, on the synthetic data sets and find our marginalized |$\mathcal {GP}$| algorithm performs significantly better than the standard algorithms for data contaminated by systematics. Finally, we apply the marginalized |$\mathcal {GP}$| algorithm to four prototypical emission-line binaries: Eta Carinae, GG Carinae, WR 140, and WR 133. We find systematics to be present in several of these case studies; and consequently, the predicted orbital parameter distributions, and dynamical masses, are modified from those previously determined. [ABSTRACT FROM AUTHOR]

We use a three-dimensional smoothed particle hydrodynamics code to simulate growth and dissipation of Be star discs in systems where the binary orbit is misaligned with respect to the spin axis of the primary star. We investigate six different scenarios of varying orbital period and misalignment angle, feeding the disc at a constant rate for 100 orbital periods, and then letting the disc dissipate for 100 orbital periods. During the disc growth phase, we find that the binary companion tilts the disc away from its initial plane at the equator of the primary star before settling to a constant orientation after 40–50 orbital periods. While the mass-injection into the disc is ongoing, the tilting of the disc can cause material to reaccrete on to the primary star prematurely. Once disc dissipation begins, usually the disc precesses about the binary companion's orbital axis with precession periods ranging from 20 to 50 orbital periods. In special cases, we detect phenomena of disc tearing, as well as Kozai–Lidov oscillations of the disc. These oscillations reach a maximum eccentricity of about 0.6, and a minimum inclination of about 20○ with respect to the binary's orbit. We also find the disc material to have highly eccentric orbits beyond the transition radius, where the disc changes from being dominated by viscous forces, to heavily controlled by the companion star, in contrast to its nearly circular motion inwards of the transition radius. Finally, we offer predictions to how these changes will affect Be star observables. [ABSTRACT FROM AUTHOR]

Copyright of Studies in Law & Economics / Studia Prawno-Ekonomiczne is the property of Lodz Scientific Society / Lodzkie Towarzystwo Naukowe and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

PSR B1259-63 is a g-ray binary system, where the compact object is a pulsar. The system has an orbital period of 1236.7 days and shows peculiar g-ray flares (in 100MeV–300 GeV) after its periastron time. We analyzed the Fermi-LAT observation of PSR B1259-63 during its latest periastron passage, as well as its previous three periastrons. The bright GeV flares started about 60 days after the periastron epoch in 2021. This delay is larger than that around the 2017 periastron and much larger than earlier periastrons. The delay of the GeV flux peak time in each periastron passage is apparent in our results. We discussed the possible origin of this delay and made a prediction of the GeV flux peak time in next periastron passage, based on observation of the previous delays. [ABSTRACT FROM AUTHOR]

The bright and understudied classical Be star HD 6226 has exhibited multiple outbursts in the last several years during which the star grew a viscous decretion disc. We analyse 659 optical spectra of the system collected from 2017 to 2020, along with a ultraviolet spectrum from the Hubble Space Telescope and high cadence photometry from both Transiting Exoplanet Survey Satellite (TESS) and the Kilodegree Extremely Little Telescope (KELT) survey. We find that the star has a spectral type of B2.5IIIe, with a rotation rate of 74 per cent of critical. The star is nearly pole-on with an inclination of 13 |${_{.}^{\circ}}$| 4. We confirm the spectroscopic pulsational properties previously reported, and report on three photometric oscillations from KELT photometry. The outbursting behaviour is studied with equivalent width measurements of H α and H β, and the variations in both of these can be quantitatively explained with two frequencies through a Fourier analysis. One of the frequencies for the emission outbursts is equal to the difference between two photometric oscillations, linking these pulsation modes to the mass ejection mechanism for some outbursts. During the TESS observation time period of 2019 October 7 to 2019 November 2, the star was building a disc. With a large data set of H α and H β spectroscopy, we are able to determine the time-scales of dissipation in both of these lines, similar to past work on Be stars that has been done with optical photometry. HD 6226 is an ideal target with which to study the Be disc-evolution given its apparent periodic nature, allowing for targeted observations with other facilities in the future. [ABSTRACT FROM AUTHOR]

Introduction. Early warning scoring systems are important for timely identification of the critically ill, but are they a relevant prognostic tool? Our objective was to test if Modified Early Warning Score (MEWS), lactate, and base excess (BE) have any prognostic value in high dependency unit patients. Methods. This was a prospective observational study that included 364 patients treated at a respiratory high dependency unit. The values of MEWS, lactate, and BE at admission were recorded with patients’ age, sex, and comorbidities. Negative outcome was defined as death or transfer to the intensive care unit. Independent predictors of negative outcome were identified with the use of multivariable logistic regression. Results. Of 369 patients, 203 (55%) were male. Mean age was 62 ± 16. There were 138 (37.4%) patients with negative outcome: 27.37% died, while 10.03% patients required intensive care unit transfer. The median length of hospital stay was 13 days (IQR 7–15). Patients with negative outcome had a significantly higher MEWS (3.68 ± 1.965 vs. 4.57 ± 2.33, p < 0.001), lower BE (-0.139 ± 7.48 vs. -3.751 ± 6.159, p < 0.001), and a higher lactate (2.299 ± 2.350 vs. 3.498 ± 3.578, p < 0.001). MEWS ≥ 4 (OR 1.90, CI 1.082–3.340, p = 0.026) was the only independent predictor of mortality. Area under the curve (AUC) for MEWS with regard to in-hospital mortality prediction was 0.633 (95% CI 0.569–0.697). When age was added to MEWS, the AUC was 0.76 (95% CI 0.707–0.814). Conclusion. Our findings support the prognostic value of MEWS for final outcome of patients admitted to the high dependency unit.

Pre-main-sequence (PMS) stars evolve into main-sequence (MS) phase over a period of time. Interestingly, we found a scarcity of studies in existing literature that examine and attempt to better understand the stars in PMS to MS transition phase. The purpose of this study is to detect such rare stars, which we named as 'transition phase' (TP) candidates – stars evolving from the PMS to the MS phase. We identified 98 TP candidates using photometric analysis of a sample of 2167 classical Be (CBe) and 225 Herbig Ae/Be (HAeBe) stars. This identification is done by analysing the near- and mid-infrared excess and their location in the optical colour–magnitude diagram. The age and mass of 58 of these TP candidates are determined to be between 0.1–5 Myr and 2–10.5 M⊙, respectively. The TP candidates are found to possess rotational velocity and colour excess values in between CBe and HAeBe stars, which is reconfirmed by generating a set of synthetic samples using the machine learning approach. [ABSTRACT FROM AUTHOR]

We continue to search for LBV stars in galaxies outside the Local Group. In this work, we have investigated four luminous stars in NGC 4449. Multiple spectral observations carried out for J122810.94+440540.6, J122811.70+440550.9, and J122809.72+440514.8 revealed the emission features in their spectra that are characteristic of LBVs. Photometry showed noticeable brightness changes of J122809.72+440514.8 (Δ I  = 0.69 ± 0.13 m ) and J122817.83+440630.8 (Δ R  = 2.15 ± 0.13 m ), while the variability of J122810.94+440540.6 and J122811.70+440550.9 does not exceed 0.3 m regardless of the filter. We have obtained estimates of the interstellar reddening, photosphere temperatures, and bolometric luminosities log (L Bol/L⊙) ≈ 5.24–6.42. Using the cmfgen code, we have modelled the spectrum of the cold state of J122809.72+440514.8 (⁠|$T_{\text{eff}}=9300\,$|  K) and have obtained possible value of the mass-loss rate |$\dot{M} = 5.2\times 10^{-3}\, \mathrm{M}_{\odot }\, \mathrm{yr}^{-1}$|⁠. Based on the observational properties, J122809.72+440514.8 and J122817.83+440630.8 were classified as LBVs, while the other two stars were classified as LBV candidates or B[e]-supergiants candidates. [ABSTRACT FROM AUTHOR]

The first high-resolution spectra (resolving powers of R ≥ 60 000) of the emission-line star VES 723, which has an unknown evolutionary status, were taken at the 6-m Big Telescope Alt-Azimuthal and the 3.6-m Canada–France–Hawaii Telescope. The spectrum is dominated with powerful emission lines of neutral hydrogen and helium, and forbidden singly ionized nitrogen. The Hα and He  i lines were found to exhibit broad foundations of the emission profiles at least 250 km s−1 wide. The strongest emission lines exhibit no noticeable variations during the observing period (2011–2017) except for the He  i lines. The spectra contain multicomponent interstellar absorptions of Na  i and K  i (mult. 1) and several strongest diffuse interstellar bands, while photospheric absorptions have not been detected. The average radial velocity of the forbidden [N  ii ] emission line centres was adopted as the systemic velocity (V sys ≈ −52 km s−1), which indicates a large distance of ≈6 kpc. Our luminosity estimates of log  L /L⊙ = 3.7−4.0 for two different Gaia distance measurements, along with an effective temperature of T eff = 25 000 ± 2000 K and a fast decrease of the infrared flux longward of |$\lambda \sim 10\, \mu{\rm m}$|⁠ , allow us to suggest that VES 723 is neither a pre-main-sequence Herbig B[e] star nor a B[e] supergiant but rather a member of the FS CMa group of objects with the B[e] phenomenon. [ABSTRACT FROM AUTHOR]

Evidence-based and culturally relevant parenting programs strengthen adults' capacity to support children's health and development. Optimizing parent participation in programs implemented at scale is a prevailing challenge. Our collaborative team of program developers, implementers, and researchers applied insights from the field of behavioral economics (BE) to support parent participation in ParentCorps—a family-centered program delivered as an enhancement to pre-kindergarten—as it scaled in a large urban school district. We designed a bundle of BE-infused parent outreach materials and successfully showed their feasibility in site-level randomized pilot implementation. The site-level study did not show a statistically significant impact on family attendance. A sub-study with a family-level randomization design showed that varying the delivery time of BE-infused digital outreach significantly increased the likelihood of families attending the parenting program. Lessons on the potential value of a BE-infused approach to support outreach and engagement in parenting programs are discussed in the context of scaling up efforts. [ABSTRACT FROM AUTHOR]

This article proposes a novel account for the overuse of free morphemes and underuse of bound morphemes in English as a second language (L2) based on the framework of Distributed Morphology. It will be argued that an Economy Principle 'Do everything in Narrow Syntax (DENS)' operates in the L2 learner's computational system. Consequently, derivation in Morphology becomes as limited as possible except when applying Vocabulary Items to syntactic objects (Vocabulary Insertion). This results in non-target-like use/acceptance of certain morphemes: Bound morphemes are often omitted in early L2 grammar, and alternative free morphemes may apparently be used instead. Two types of data, namely the overuse of be reported in previous research, and the preference of to- infinitives over -ing gerunds in early L2 grammar, will be presented in support of the proposal, and the plausibility of the operation of DENS will be discussed. [ABSTRACT FROM AUTHOR]

The determination of Li,Be,Sc,V,Cr,Co,Ni,Cu,Zn,Ge,Mo,Cd,Ba,La,Ce, W,Tl,Pb,Th,U in soll samples dissolved wtth phosphoric acid and aqua regaa was studied. The acid system, the best mode and working condition of the ICP-MS was studeed. Rh was used as internal standard to correct the drift of the instrument. By setting several certified standard materials of stream sediments and sols to dissolve together wtth the sampes, the standard curve was estabisshed, which could eliminate the uncertainty error and matrix interference caused by the digestion, fractionation and constant. Eight kinds of soll reference materials were se!ected as experimental samples. The results showed that the accuracy of the method(Algc) was Iss than 0. 1, t he relatives standard devaation SD) was less than 8%, a nd this method was feasible. [ABSTRACT FROM AUTHOR]

Cosmogenic radionuclide 10Be and 26Al targets (BeO and Al2O3) for AMS analysis are produced by a growing number of geochemical laboratories, employing different sample processing methods for the extraction of Be and Al from environmental materials. The reliability of this geochronological tool depends on data reproducibility independent from the preparation steps and the AMS measurements. Our results demonstrate that 10Be and 26Al concentrations of targets processed following different, commonly used protocols and measured at two AMS facilities lead to consistent results. However, insoluble fluoride precipitates, if formed during processing, can cause decreased 26Al results, while 10Be concentrations are unaffected. [ABSTRACT FROM AUTHOR]

Computer modeling of the outflow from Be stars is performed. In our approach, processes of turbulence excitation and turbulent viscosity are added to the conventional model of the radiation driven winds. The objective of our study is to reproduce from the first principles the main features of the outflow from Be stars: a fast polar wind and a slow viscous Keplerian disk at the equator. At sub-critical velocity of rotation up to 0.999 of the critical velocity, our model reproduces the formation of the fast polar wind together with a slow highly turbulent outflow at the equatorial region. This outflow, however, does not reassemble a Keplerian disk. We link this to the absence of the angular moment transfer from the star to the disk. This process provides an increase of the angular momentum of the disk matter with radius. We consider a star with super critical rotation as the simplest way to supply the angular momentum to the disk. In this case, the star surface has a higher azimuthal speed than the matter at the inner edge of the disk. The angular momentum transfer becomes unavoidable. Already at rotation velocity 0.5% above the critical one, a quasi Keplerian disk at the equator is formed with size ∼10 stellar radius. At rotation 1% higher than the critical speed, the disk reaches ∼15 stellar radius. The main conclusion following from our work is that the conventional model of the radiation driven winds is able to reproduce the main features of the outflow from Be stars provided that the process of turbulence excitation and a process of angular momentum supply of the disk from the central source are added in to this model.

We revisit the subject of Be candidate stars towards the Magellanic Clouds, previously studied by the authors using SPM4 proper motions. We obtain Gaia DR2 parallaxes and proper motions for 2357 and 994 LMC and SMC Be candidates, respectively. Parallaxes and proper motions versus colour V − I easily reveal the presence of the redder galactic contaminant foreground, as concluded in our previous work, but this time we do find a few red Be candidates consistent with being true Magellanic objects. A membership assessment to each Magellanic Cloud is done for each Be candidate, based on the distribution of their parallaxes and proper motions. From a compilation of published catalogues of spectroscopically confirmed emission line stars,we find that 41 (LMC) and 56 (SMC) of the Be candidates have shown the H α line in emission. Near-infrared IRSF JHKs magnitudes are obtained for about 70 per cent of the Be candidates with Gaia DR2 astrometric data. Mid-infrared SAGE IRAC 3.6, 4.5, 5.8, and 8.0 |$\mu$| m magnitudes are obtained for about 85 per cent as well. After discarding possible Herbig Ae/Be stars, one LMC and three SMC B emission line confirmed stars show significantly redder optical, near- and mid-infrared colours than what has been typically measured for Classical Be stars – they are called red Be stars. Taking into account that classical Be stars do not show these red colours, further studies about these four stars are needed in order to establish their true nature and explain the observed red excess. [ABSTRACT FROM AUTHOR]

RX J0123.4-7321 is a well-established Be star X-ray binary system in the Small Magellanic Cloud. Like many such systems, the variable X-ray emission is driven by the underlying behaviour of the mass donor Be star. Previous work has shown that the optical and X-ray were characterized by regular outbursts at the proposed binary period of 119 d. However, around 2008 February the optical behaviour changed substantially, with the previously regular optical outbursts ending. Reported here are new optical (OGLE) and X-ray (Swift) observations covering the period after 2008 that suggest an almost total circumstellar disc loss followed by a gradual recovery. This indicates the probable transition of a Be star to a B star, and back again. However, at the time of the most recent OGLE data (2020 March) the characteristic periodic outbursts had yet to return to their early state, indicating that the disc still had some re-building yet to complete. [ABSTRACT FROM AUTHOR]

We consider the problem of identification of the position of some source by observations of K detectors receiving signals from this source. The time of arriving of the signal to the k-th detector depends of the distance between this detector and the source. The signals are observed in the presence of small Gaussian noise. The properties of the MLE and Bayesian estimators are studied in the asymptotic of small noise. [ABSTRACT FROM AUTHOR]

Mass loss plays a key role in the evolution of massive stars and their environment. High mass-loss events are traced by complex circumstellar ejecta and intricate line profiles across the upper Hertzsprung-Russell diagram for massive stars in different evolutionary stages. The basic physics of radiation-driven stellar wind for hot stars is well understood. However, the driving mechanisms and related instabilities for their enhanced mass-loss episodes and the driving mechanisms for the mass loss of cool stars are still debated. In this review, the mass-loss characteristics and the possible mechanisms will be surveyed for an observational set of prominent massive stellar populations that experience outflows, strong stellar winds, and periods of enhanced and eruptive mass loss; massive young stellar objects, OB-type stars, red supergiants, warm hypergiants, luminous blue variables, and Wolf-Rayet stars. [ABSTRACT FROM AUTHOR]

. In this work, we implemented a hydrodynamical solution for fast rotating stars, which leaves high values of mass-loss rates and low terminal velocities of the wind. This 1D density distribution adopts a viscosity mimicking parameter which simulates a quasi-Keplerian motion. Then, it is converted to a volumetric density considering vertical hydrostatic equilibrium using a power-law scale height, as usual in viscous decretion disk models. We calculate the theoretical hydrogen emission lines and the spectral energy distribution utilizing the radiative transfer code HDUST. Our disk-wind structures are in agreement with viscous decretions disk models. [ABSTRACT FROM AUTHOR]

We present a catalogue of point-like H  α -excess sources in the Northern Galactic Plane. Our catalogue is created using a new technique that leverages astrometric and photomeric information from Gaia to select H  α -bright outliers in the INT Photometric H  α Survey of the Northern Galactic Plane (IPHAS), across the colour–absolute magnitude diagram. To mitigate the selection biases due to stellar population mixing and to extinction, the investigated objects are first partitioned with respect to their positions in the Gaia colour–absolute magnitude space, and Galactic coordinates space, respectively. The selection is then performed on both partition types independently. Two significance parameters are assigned to each target, one for each partition type. These represent a quantitative degree of confidence that the given source is a reliable H  α -excess candidate, with reference to the other objects in the corresponding partition. Our catalogue provides two flags for each source, both indicating the significance level of the H  α -excess. By analysing their intensity in the H  α narrow band, 28 496 objects out of 7474 835 are identified as H  α -excess candidates with a significance higher than 3. The completeness fraction of the H  α outliers selection is between 3 and 5 per cent. The suggested 5 σ conservative cut yields a purity fraction of 81.9 per cent. [ABSTRACT FROM AUTHOR]

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GG Carinae (GG Car) is a binary whose primary component is a B[e] supergiant. Using photometric data from the Transiting Exoplanet Survey Satellite (TESS), All Sky Automated Survey (ASAS), Optical Monitoring Camera (OMC), and All Sky Automated Survey for Supernovae (ASAS-SN), and spectroscopic data from the Global Jet Watch to study visible He  i , Fe  ii , and Si  ii emission lines, we investigate the short-period variations that are exhibited in GG Car. We find a hitherto neglected periodicity of 1.583156 ± 0.0002 d that is present in both its photometry and the radial velocities of its emission lines, alongside variability at the well-established ∼31-d orbital period. We find that the amplitudes of the shorter period variations in both photometry and some of the emission lines are modulated by the orbital phase of the binary, such that the short-period variations have largest amplitudes when the binary is at periastron. There are no significant changes in the phases of the short-period variations over the orbital period. We investigate potential causes of the 1.583-d variability, and find that the observed period agrees well with the expected period of the l = 2 f-mode of the primary given its mass and radius. We propose that the primary is periodically pulled out of hydrostatic equilibrium by the quadrupolar tidal forces when the components are near periastron in the binary's eccentric orbit (e = 0.5) and the primary almost fills its Roche lobe. This causes an oscillation at the l = 2 f-mode frequency that is damped as the distance between the components increases. [ABSTRACT FROM AUTHOR]

Each paper must begin with an abstract. The abstract should be typed in the same manner as the body text (see below). Please note that these Instructions are typed just like the manuscripts should be. The abstract must have at least 25-300 words, supplying general information about the achievements, and objectives of the paper, experimental technique, methods applied, significant results and conclusions. Page layout: the text should be printed on the paper A4 format, at least 5 pages, with margins of: Top - 3, Bottom, Left and Right - 2 cm. The abstract, keywords should be presented in English (only for foreign authors), and Ukrainian. The text should be prepared in "doc" or "docx" format. [ABSTRACT FROM AUTHOR]

BackgroundCENDL-3.2 was released in June 2020. Compared with CENDL-3.1, data type and quality has been greatly improved in CENDL-3.2,and most important isotopes including 235U, 238U, 239Pu, 56Fe and others have been re-evaluated and supplemented. Due to its large scattering cross section and small absorption cross section, Be is often used as one of the fuel carrier salt components of molten salt reactor (MSR). The accuracy of reaction cross section data of Be in MSR design cannot be ignored.PurposeThis study aims to examine and analyze the adaptability of the cross section data of Be in CENDL-3.2 to the calculation of MSR problems by the discrete-ordinate method.MethodsBased on CENDL-3.2,the MATXS format multi-group cross section library of 199 neutron groups and 42 photon groups was generated by NJOY, and 35 fast critical benchmarks were selected for its inspection and analysis. Then, results were compared with those of multi-group cross section library based on ENDF/B-7.1 and JENDL-4.0.ResultsThe deviation between the calculated results of the multi-group cross section library based on CENDL-3.2 and the experimental values is less than 0.5% in 26 benchmark cases which is 74.29% of total, outperform those of ENDF/B-7.1 and JENDL-4.0.ConclusionsThe results of this study indicate that the data of Be and the multi-group cross section library based on CENDL-3.2 and its processing method are reliable and can be used in the design of molten salt reactor.

We report the results of optical spectroscopy of the Small Magellanic Cloud supernova remnant (SNR) MCSNR J0127−7332 and the mass donor Be star, 2dFS 3831, in its associated high-mass X-ray binary SXP 1062 carried out with the Southern African Large Telescope. Using high-resolution long-slit spectra, we measured the expansion velocity of the SNR shell of |${\approx} 140 \, {\rm \, km\, s^{-1}}$|⁠ , indicating that MCSNR J0127−7332 is in the radiative phase. We found that the observed line ratios in the SNR spectrum can be understood if the local interstellar medium is ionized by 2dFS 3831 and/or OB stars around the SNR. We propose that MCSNR J0127−7332 is the result of supernova explosion within a bubble produced by the stellar wind of the supernova progenitor and that the bubble was surrounded by a massive shell at the moment of supernova explosion. We estimated the age of MCSNR J0127−7332 to be |${\lesssim} 10\, 000$|  yr. We found that the spectrum of 2dFS 3831 changes with orbital phase. Namely, the equivalent width of the H α emission line decreased by ≈40 per cent in ≈130 d after periastron passage of the neutron star and then almost returned to its original value in the next ≈100 d. Also, the spectrum of 2dFS 3831 obtained closest to the periastron epoch (about 3 weeks after the periastron) shows a noticeable emission line of He  ii λ4686, which disappeared in the next 2 weeks. We interpret these changes as a result of the temporary perturbation and heating of the disc as the neutron star passes through it. [ABSTRACT FROM AUTHOR]

HR 6819 is a bright (V = 5.36), blue star recently proposed to be a triple containing a detached black hole (BH). We show that the system is a binary and does not contain a BH. Using spectral decomposition, we disentangle the observed composite spectra into two components: a rapidly rotating Be star and a slowly rotating B star with low surface gravity (log  g ≈ 2.75). Both stars show periodic radial velocity (RV) variability, but the RV semi-amplitude of the B star's orbit is |$K_{\rm B}= (62.7 \pm 1)\, \rm km\, s^{-1}$|⁠ , while that of the Be star is only |$K_{\rm Be} = (4.5\pm 2)\, \rm km\, s^{-1}$|⁠. This implies that the B star is less massive by at least a factor of 10. The surface abundances of the B star bear imprints of CNO burning. We argue that the B star is a bloated, recently stripped helium star with mass |${\approx}0.5\, \mathrm{ M}_{\odot }$| that is currently contracting to become a hot subdwarf. The orbital motion of the Be star obviates the need for a BH to explain the B star's motion. A stripped-star model reproduces the observed luminosity of the system, while a normal star with the B star's temperature and gravity would be more than 10 times too luminous. HR 6819 and the binary LB-1 probably formed through similar channels. We use MESA (Modules for Experiments in Stellar Astrophysics) models to investigate their evolutionary history, finding that they likely formed from intermediate-mass (⁠|$3\!-\!7\, \mathrm{ M}_{\odot }$|⁠) primaries stripped by slightly lower-mass secondaries and are progenitors to Be + sdOB binaries such as ϕ Persei. The lifetime of their current evolutionary phase is on average 2 × 105 yr, of the order of half a per cent of the total lifetime of the Be phase. This implies that many Be stars have hot subdwarf and white dwarf companions, and that a substantial fraction (⁠|$20\!-\!100{{\ \rm per\ cent}}$|⁠) of field Be stars form through accretion of material from a binary companion. [ABSTRACT FROM AUTHOR]

Numerical modelling of an isothermal wind from a fast rotating star is performed. Excitation of hydrodynamical turbulence and deviation of the shape of the stellar surface from a sphere are taken into account. Rotation and turbulence result in a dramatic increase of the mass flow rate from the star in comparison with a non-rotating one. The outflow occurs predominantly from a region on the stellar surface located at the equator. This flow expands rapidly due to thermal pressure. However, a disc-like flow at the equator is formed. The flow is more complicated near the pole. At large distances from the star a radially expanding wind is formed while close to the star some fraction of the outflow from the equatorial region falls down on to the stellar surface, producing a huge vortex. The dependence of the mass loss rate on the parameters of the star is presented. [ABSTRACT FROM AUTHOR]

In photometry of γ Cas (B0.5 IVe) from the Solar Mass Ejection Imager (SMEI) and the BRIght Target Explorer (BRITE)-Constellation satellites, indications of low-order non-radial pulsation have recently been found, which would establish an important commonality with the class of classical Be stars at large. New photometry with the Transiting Exoplanet Survey Satellite (TESS) has detected three frequency groups near 1.0 (g 1), 2.4 (g 2), and 5.1 (g 3) d−1, respectively. Some individual frequencies are nearly harmonics or combination frequencies but not exactly so. Frequency groups are known from roughly three quarters of all classical Be stars and also from pulsations of β Cep, slowly pulsating B (SPB), and γ Dor stars and, therefore, firmly establish γ Cas as a non-radial pulsator. The total power in each frequency group is variable. An isolated feature exists at 7.57 d−1 and, together with the strongest peaks in the second and third groups ordered by increasing frequency (g 2 and g 3), is the only one detected in all three TESS sectors. The former long-term 0.82 d−1 variability would fall into g 1 and has not returned at a significant level, questioning its attribution to rotational modulation. Low-frequency stochastic variability is a dominant feature of the TESS light curve, possibly caused by internal gravity waves excited at the core–envelope interface. These are known to be efficient at transporting angular momentum outward, and may also drive the oscillations that constitute g 1 and g 2. The hard X-ray flux of γ Cas is the only remaining major property that distinguishes this star from the class of classical Be stars. [ABSTRACT FROM AUTHOR]

We report the first systematic study to identify and characterize a sample of classical Ae stars in the Galaxy. The spectra of these stars were retrieved from the A-star catalogue using the Large sky Area Multi-Object fibre Spectroscopic Telescope (LAMOST) survey. We identified the emission-line stars in this catalogue from which 159 are confirmed as classical Ae stars. This increases the sample of known classical Ae stars by about nine times from the previously identified 21 stars. The evolutionary phase of classical Ae stars in this study is confirmed from the relatively small mid- and far-infrared excess and from their location in the optical colour–magnitude diagram. We estimated the spectral type using MILES spectral templates and identified classical Ae stars beyond A3, for the first time. The prominent emission lines in the spectra within the wavelength range 3700–9000 Å are identified and compared with the features present in classical Be stars. The H α emission strength of the stars in our sample show a steady decrease from late-B type to Ae stars, suggesting that the disc size may be dependent on the spectral type. Interestingly, we noticed emission lines of Fe  ii , O  i , and Paschen series in the spectrum of some classical Ae stars. These lines are supposed to fade out by late B-type and should not be present in Ae stars. Further studies, including spectra with better resolution, is needed to correlate these results with the rotation rates of classical Ae stars. [ABSTRACT FROM AUTHOR]

Using TESS photometry and Rozhen spectra of the Be/γ-ray binaries MWC 148 and MWC 656, we estimate the projected rotational velocity (v sin i), rotational period (Prot), radius (R1), and inclination (i) of the mass donor. For MWC 148, we derive Prot =1.10±0.03 day, R1 =9.2±0.05 Rsun, i = 40◦ ±2◦, and v sin i = 272±5 km s-1. For MWC 656, we obtain Prot =1.12±0.03 day, R1=8.8±0.5 Rsun, i = 52◦ ±3◦, and v sin i = 313±3 km s-1. For MWC 656, we also find that the rotation of the mass donor is coplanar with the orbital plane. [ABSTRACT FROM AUTHOR]