Disc loss and renewal in A0535+26

This paper presents observations of the Be/X-ray binary system A0535+26 revealing the first observed loss of its circumstellar disc, demonstrated by the loss of its JHK infrared excess and optical/IR line emission. However optical/IR spectroscopy reveals the formation of a new inner disc with significant density and emission strength at small radii; the disc has proven to be stable over 5 months in this intermediate state.Comment: 4 pages, 4 figures, accepted by MNRAS, uses mn.st

Desempenho produtivo, composição corporal e parâmetros fisiológicos de pacu alimentado com níveis crescentes de fibra.

O objetivo deste trabalho foi avaliar os efeitos de teores de fibra bruta na dieta sobre o desempenho produtivo, composição centesimal da carcaça e parâmetros fsiológicos de juvenis de pacu. O experimento teve duração de 84 dias, e foram utilizados 360 juvenis de pacu, com peso médio de 23,97±0,59 g, distribuídos aleatóriamente em 30 tanques com 180 L de água, em delineamento inteiramente casualizado, com seis tratamentos (5, 7, 9, 11, 13 e 15% de fibra bruta) e cinco repetições. Dietas com altos teores de fibra (11, 13 e 15%) resultaram em piores taxas de ganho de peso, conversão alimentar e crescimento específco, além de menor efciência proteica e consumo de ração. A composição da carcaça dos animais foi alterada pelo aumento do teor de fibra das dietas. Os teores de proteína e cinza tiveram aumento com o incremento nos teores de fibra. O metabolismo foi alterado com o emprego de teores crescentes de fibra, o que resultou em pequena elevação do colesterol plasmático. Teores de fibra bruta de até 9% não tiveram efeitos negativos no metabolismo; entretanto, teores acima de 11% reduziram o crescimento dos peixes

Delayed gastric emptying after classical Whipple or pylorus-preserving pancreatoduodenectomy: a randomized clinical trial (QUANUPAD)

Purpose Pylorus-preserving pancreatoduodenectomy (PPPD) has been the gold standard for pancreatic head lesion resection for several years. Some studies have noted that it involves more delayed gastric emptying (DGE) than classical Whipple (i.e., pancreatoduodenectomy with antrectomy). Our working hypothesis was that the classical Whipple has a lower incidence of DGE. We aimed to compare the incidence of DGE among pancreatoduodenectomy techniques. Methods This pragmatic, randomized, open-label, single-center clinical trial involved patients who underwent classical Whipple (study group) or PPPD (control group). Gastric emptying was clinically evaluated using scintigraphy. DGE was defined according to the International Study Group of Pancreatic Surgery (ISGPS) criteria. The secondary endpoints were postoperative morbidity, length of hospital stay, anthropometric measurements, and nutritional status. Results A total of 84 patients were randomized (42 per group). DGE incidence was 50% (20/40, 95% confidence interval (95% CI): 35-65%) in the study group and 62% (24/39, 95% CI: 46-75%) in the control group (p = 0.260). No differences were observed between both groups regarding postoperative morbidity or length of hospital stay. Anthropometric measurements at 6 months post-surgery: triceps fold measurements were 12 mm and 16 mm (p = 0.021). At 5 weeks post-surgery, triceps fold measurements were 13 mm and 16 mm (p = 0.020) and upper arm circumferences were 26 cm and 28 cm (p = 0.030). No significant differences were observed in nutritional status. Conclusion DGE incidence and severity did not differ between classical Whipple and PPPD. Some anthropometric measurements may indicate a better recovery with PPPD

The Be/X-ray binary LS 992/RX J0812.4-3114: physical parameters and long-term variability

We present the first long-term optical and infrared study of the optical counterpart to the source RX J0812.4-3114, an X-ray pulsar with a Be type companion. During the period covered by the observations the profile of some Balmer lines changed from absorption to emission and back again to absorption. Contemporaneously, the infrared magnitudes varied by more than 0.8 mag. This long-term variability is interpreted as the formation and subsequent dissipation of the Be star's disc. The building up of the disc ended up in an active X-ray state characterised by regular outbursts occurring at 80 day intervals. The overall duration of the formation/dissipation of the disc is found to be < 4.3 years. Optical spectroscopic and infrared photometric observations were used to refine the spectral type of the primary (B0.2IV) and to monitor the circumstellar envelope around the Be star. UBVRI and uvby\beta photometric observations allowed the determination of the astrophysical parameters of the optical companion.Comment: 7 pages, 3 figures, accepted for publication in A&

Diferentes intervalos de coleta na determinação da digestibilidade aparente da proteína e da energia de ingredientes comuns para o apaiari (Astronotus ocellatus).

This study evaluated the apparent protein and energy digestibility of common feed ingredients (soybean meal, fish meal, wheat meal and corn) by juvenile oscars using two different sampling intervals (30 min. and 12h). The 160 juvenile oscar fish tested (22.37 ± 3.06 g BW) were divided into four cylindrical plastic net cages, each one placed in a 1000 L feeding tank. The experiment was completely randomized in a 2 x 4 factorial design (2 feces collection intervals and 4 feed ingredients) with four replications. The statistical tests did not detect an interaction effect of sampling interval and type of ingredient on digestibility coefficients. Sampling interval did not affect protein and energy digestibility. The physical characteristics of juvenile oscar feces likely make them less susceptible to nutrient loss by leaching and can therefore be collected at longer intervals. Protein digestibility of the different ingredients was similar, showing that apparent digestibility of both animal and plant ingredients by juvenile oscars was efficient. Energy digestibility coefficients of fish meal and soybean meal were higher than those of wheat meal and corn. Carbohydrate-rich ingredients (wheat meal and corn) had the worst energy digestibility coefficients and are therefore not used efficiently by juvenile oscars

Photometric observations of the radio bright B[e]/X-ray binary CI Cam

We present multiwavelength (optical, IR, radio) observations of CI Cam, the optical counterpart to the transient X-ray source XTE J0421+560. Pre-outburst quiescent observations reveal the presence of a dusty envelope around the system. Pronounced short term variability is observed at all wavebands from U-K, but no indication of prior flaring of a similar magnitude to the 1998 April outburst is found in these data. Data obtained during the 1998 April X-ray flare reveal pronounced optical-radio flaring. The optical flux was observed to quickly return to quiescent levels, while the radio flare was of much longer duration. The optical component is likely to result from a combination of free-free/free-bound emission, emission line and thermal dust emission, caused by re-radiation of the X-ray flux, while the behaviour of the multiwavelength radio data is consistent with emission from expanding ejecta emitting via the synchrotron mechanism. Post-outburst (1998 August-1999 March) U-M broadband photometric observations reveal that while the optical (UBV) flux remains at pre-outburst quiescent levels, near IR (JHKLM) fluxes exceed the pre-outburst fluxes by ~0.5 magnitudes. Modelling the pre- and post-outburst spectral energy distribution of CI Cam reveals that the structure and/or composition of the dusty component of the circumstellar envelope appears to have changed. Due to a lack of information on the precise chemical composition of the dust within the system several explanations for this behaviour are possible, such as the production of new dust at the inner edge of the envelope, or modification of the composition of the dust due to X-ray irradiation

Infrared studies of the Be star X Per

Photometric and spectroscopic results are presented for the Be star X Per/HD 24534 from near-infrared monitoring in 2010-2011. The star is one of a sample of selected Be/X-ray binaries being monitored by us in the near-IR to study correlations between their X ray and near-IR behaviour. Comparison of the star's present near-IR magnitudes with earlier records shows the star to be currently in a prominently bright state with mean J, H, K magnitudes of 5.49, 5.33 and 5.06 respectively. The JHK spectra are dominated by emission lines of HeI and Paschen and Brackett lines of HI. Lines of OI 1.1287 and 1.3165 micron are also present and their relative strength indicates, since OI 1.1287 is stronger among the two lines, that Lyman beta fluorescence plays an important role in their excitation. Recombination analysis of the HI lines is done which shows that the Paschen and Brackett line strengths deviate considerably from case B predictions. These deviations are attributed to the lines being optically thick and this supposition is verified by calculating the line center optical depths predicted by recombination theory. Similar calculations indicate that the Pfund and Humphrey series lines should also be expected to be optically thick which is found to be consistent with observations reported in other studies. The spectral energy distribution of the star is constructed and shown to have an infrared excess. Based on the magnitude of the IR excess, which is modeled using a free-free contribution from the disc, the electron density in the disc is estimated and shown to be within the range of values expected in Be star discs.Comment: Accepted for publication in MNRAS, 7 pages, 6 figure

Physical parameters of IPHAS-selected classical Be stars. (I. Determination procedure and evaluation of the results.)

Reproduced with permission from Astronomy & Astrophysics, © 2016 ESOWe present a semi-automatic procedure to obtain fundamental physical parameters and distances of classical Be (CBe) stars, based on the Barbier-Chalonge-Divan (BCD) spectrophotometric system. Our aim is to apply this procedure to a large sample of CBe stars detected by the IPHAS photometric survey, to determine their fundamental physical parameters and to explore their suitability as galactic structure tracers. In this paper we describe the methodology used and the validation of the procedure by comparing our results with those obtained from different independent astrophysical techniques for subsamples of stars in common with other studies. We also present a test case study of the galactic structure in the direction of the Perseus Galactic Arm, in order to compare our results with others recently obtained with different techniques and the same sample of stars. We did not find any significant clustering of stars at the expected positions of the Perseus and Outer Galactic Arms, in agreement with previous studies in the same area that we used for verification.Peer reviewedFinal Published versio

XMM-Newton observation of the persistent Be/neutron-star system X Persei at a high-luminosity level

We report on the XMM-Newton observation of the HMXRB X Persei, the prototype of the persistent and low-luminosity Be/neutron star pulsars, which was performed on February 2003. The source was detected at a luminosity level of ~ 1.4x10^35 erg/s, which is the highest level of the latest three decades. The pulsation period has increased up to 839.3 s, thus confirming the overall spin-down of the NS detected in the previous observations. The folded light-curve has a complex structure, with features not observed at lower luminosities, and shows a significant energy dependence. The spectral analysis reveals the presence of a significant excess at low energies over the main power-law spectral component, which can be described by a black-body spectrum of high temperature (kT_BB ~ 1.5 keV) and small emitting region (R_BB ~ 340 m); its properties are consistent with a polar-cap origin. Phase-resolved spectroscopy shows that the emission spectrum varies along the pulse period, but it is not possible to prove whether the thermal component is pulsed or not.Comment: 8 pages, 8 figures, 4 tables. Accepted for publication by Astronomy & Astrophysic