Effect of herbal choline and rumen-protected methionine on lamb performance and blood metabolites

Twenty-four lambs (Pelibuey x East Friesian), weighing 22.7 ± 3.2 kg, were fed a basal diet of corn silage, oat hay, alfalfa hay, and concentrate (60% forage and 40% concentrate). Treatments consisted of oral doses of rumen-protected methionine (RPM) (0 and 1.5 g/day) and herbal choline (biocholine) (0 and 4 g/day) in a completely random block design with factorial arrangement of treatments, where lambs were blocked by sex. The experiment was conducted for 60 days, and measurements of live weight and dry matter intake were obtained. No effects of the treatments were observed on performance variables (lamb growth, consumption and feed conversion). Non-esterified fatty acids (NEFA) were increased by biocholine and unaffected by methionine (Met). Biocholine increased glucose and cholesterol, whereas methionine increased triglycerides, albumin and plasma protein. The dietary supplementation with biocholine and RPM did not improve lambs’ growth; however, biocholine and Met showed a lipotropic effect by mobilizing NEFA and stimulating glucose and cholestrol synthesis.Keywords: feed additives, growing sheep, lipid metabolis

Actualización de la base de datos arqueomagnética de Iberia y nuevas curvas de variación paleosecular para los últimos 3000 años

Trabajo presentado en la X Reunión de la Comisión de Paleomagnetismo de la Sociedad Geológica de España, celebrada del 14 al 17 de septiembre de 2017 en el valle del río Grío, Zaragoza (España)En este trabajo se presenta una actualización de la base de datos direccional de Iberia para los últimos 3000 años (Gómez-Paccard et al., 2006) y el primer catálogo de intensidad para este periodo. En direcciones, la base de datos ha aumentado en más de un 80%, incluyendo más de 10 resultados direccionales no publicados hasta la fecha. En intensidades, este estudio representa un aumento de más del 50% en la cantidad de datos de calidad disponibles (si nos referimos al primer milenio a.C., se cuadruplica el número de datos), entendiendo datos de calidad como aquellos que cumplen los siguientes criterios: a) que el número de especímenes empleados para la determinación de la paleointensidad sea igual o superior a 4; b) que el protocolo empleado sea Thellier (Thellier y Thellier, 1959) o derivados; c) que la anisotropía de la imanación termorremanente haya sido investigada y corregida. Toda esta información ha permitido desarrollar nuevas curvas de variación paleosecular de declinación, inclinación e intensidad de Iberia para los tres últimos milenios. Se ha empleado el método bootstrap (Thébault y Gallet, 2010) incluyendo la jerarquía asociada a la información estratigráfica cuando estaba disponible. Las nuevas curvas direccionales no presentan grandes diferencias con las anteriormente publicadas (Fig. 1), aunque se incrementa su precisión. En intensidad las principales diferencias aparecen en el primer milenio a.C. y en el posible doble máximo en torno a 600-800 años d.C, que no es recogido por esta curva. Las nuevas curvas de variación paleosecular suponen una mejora en las posibilidades de la datación arqueomagnética en la península ibéricaPeer reviewe

Stereoscopic disambiguation of vector magnetograms: first applications to SO/PHI-HRT data

Spectropolarimetric reconstructions of the photospheric vector magnetic field are intrinsically limited by the 180$^\circ$-ambiguity in the orientation of the transverse component. So far, the removal of such an ambiguity has required assumptions about the properties of the photospheric field, which makes disambiguation methods model-dependent. The basic idea is that the unambiguous line-of-sight component of the field measured from one vantage point will generally have a non-zero projection on the ambiguous transverse component measured by the second telescope, thereby determining the ``true'' orientation of the transverse field. Such an idea was developed and implemented in the Stereoscopic Disambiguation Method (SDM), which was recently tested using numerical simulations. In this work we present a first application of the SDM to data obtained by the High Resolution Telescope (HRT) onboard Solar Orbiter during the March 2022 campaign, when the angle with Earth was 27 degrees. The method is successfully applied to remove the ambiguity in the transverse component of the vector magnetogram solely using observations (from HRT and from the Helioseismic and Magnetic Imager), for the first time. The SDM is proven to provide observation-only disambiguated vector magnetograms that are spatially homogeneous and consistent. A discussion about the sources of error that may limit the accuracy of the method, and of the strategies to remove them in future applications, is also presented.Comment: 32 pages, 12 figures, accepted in A&A on 09/07/202

Magnetic fields inferred by Solar Orbiter: A comparison between SO/PHI-HRT and SDO/HMI

The High Resolution Telescope (HRT) of the Polarimetric and Helioseismic Imager on board the Solar Orbiter spacecraft (SO/PHI) and the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) both infer the photospheric magnetic field from polarised light images. SO/PHI is the first magnetograph to move out of the Sun--Earth line and will provide unprecedented access to the Sun's poles. This provides excellent opportunities for new research wherein the magnetic field maps from both instruments are used simultaneously. We aim to compare the magnetic field maps from these two instruments and discuss any possible differences between them. We used data from both instruments obtained during Solar Orbiter's inferior conjunction on 7 March 2022. The HRT data were additionally treated for geometric distortion and degraded to the same resolution as HMI. The HMI data were re-projected to correct for the $3^{\circ}$ separation between the two observatories. SO/PHI-HRT and HMI produce remarkably similar line-of-sight magnetograms, with a slope coefficient of $0.97$, an offset below $1$ G, and a Pearson correlation coefficient of $0.97$. However, SO/PHI-HRT infers weaker line-of-sight fields for the strongest fields. As for the vector magnetic field, SO/PHI-HRT was compared to both the $720$-second and $90$-second HMI vector magnetic field: SO/PHI-HRT has a closer alignment with the $90$-second HMI vector. In the weak signal regime ($< 600$ G), SO/PHI-HRT measures stronger and more horizontal fields than HMI, very likely due to the greater noise in the SO/PHI-HRT data. In the strong field regime ($\gtrsim 600$ G), HRT infers lower field strengths but with similar inclinations (a slope of $0.92$) and azimuths (a slope of $1.02$). The slope values are from the comparison with the HMI $90$-second vector.Comment: 10 pages, 5 figures, accepted for publication in A&A; manuscript is a part of Astronomy & Astrophysics special issue: Solar Orbiter First Results (Nominal Mission Phase

Vitrectomy with complete posterior hyaloid removal for ischemic central retinal vein occlusion: Series of cases

BACKGROUND: Central retinal vein occlusion (CRVO) is a common retinal vascular disorder with potentially complications: (1) persistent macular edema and (2) neovascular glaucoma. No safe treatment exists that promotes the return of lost vision. Eyes with CRVO may be predisposed to vitreous degeneration. It has been suggested that if the vitreous remains attached to the macula owing to a firm vitreomacular adhesion, the resultant vitreous traction can cause inflammation with retinal capillary dilation, leakage and subsequent edema6. The roll of vitrectomy in ischemic CRVO surgical procedures has not been evaluated. CASE PRESENTATION: This is a non comparative, prospective, longitudinal, experimental and descriptive series of cases. Ten eyes with ischemic CRVO. Vitrectomy with complete posterior hyaloid removal was performed. VA, rubeosis, intraocular pressure (IOP), and macular edema were evaluated clinically. Multifocal ERG (m-ERG), fluorescein angiography (FAG) and optic coherence tomography (OCT) were performed. Follow-up was at least 6 months. Moderate improvement of visual acuity was observed in 60% eyes and stabilized in 40%. IOP changed from 15.7 ± 3.05 mmHg to 14.9 ± 2.69 mmHg post-operative and macular edema from 976 ± 196 μm to 640 ± 191 μm to six month. The P1 wave amplitude changed from 25.46 ± 12.4 mV to 20.54 ± 11.2 mV. CONCLUSION: A solo PPV with posterior hyaloid removal may help to improve anatomic and functional retina conditions in some cases. These results should be considered when analyzing other surgical maneuvers

Association between Use of Enhanced Recovery after Surgery Protocol and Postoperative Complications in Total Hip and Knee Arthroplasty in the Postoperative Outcomes Within Enhanced Recovery after Surgery Protocol in Elective Total Hip and Knee Arthroplasty Study (POWER2)

Importance: The Enhanced Recovery After Surgery (ERAS) care protocol has been shown to improve outcomes compared with traditional care in certain types of surgery. Objective: To assess the association of use of the ERAS protocols with complications in patients undergoing elective total hip arthroplasty (THA) and total knee arthroplasty (TKA). Design, Setting, and Participants: This multicenter, prospective cohort study included patients recruited from 131 centers in Spain from October 22 through December 22, 2018. All consecutive adults scheduled for elective THA or TKA were eligible for inclusion. Patients were stratified between those treated in a self-designated ERAS center (ERAS group) and those treated in a non-ERAS center (non-ERAS group). Data were analyzed from June 15 through September 15, 2019. Exposures: Total hip or knee arthroplasty and perioperative management. Sixteen individual ERAS items were assessed in all included patients, whether they were treated at a center that was part of an established ERAS protocol or not. Main Outcomes and Measures: The primary outcome was postoperative complications within 30 days after surgery. Secondary outcomes included length of stay and mortality. Results: During the 2-month recruitment period, 6146 patients were included (3580 women [58.2%]; median age, 71 [interquartile range (IQR), 63-76] years). Of these, 680 patients (11.1%) presented with postoperative complications. No differences were found in the number of patients with overall postoperative complications between ERAS and non-ERAS groups (163 [10.2%] vs 517 [11.4%]; odds ratio [OR], 0.89; 95% CI, 0.74-1.07; P =.22). Fewer patients in the ERAS group had moderate to severe complications (73 [4.6%] vs 279 [6.1%]; OR, 0.74; 95% CI, 0.56-0.96; P =.02). The median overall adherence rate with the ERAS protocol was 50.0% (IQR, 43.8%-62.5%), with the rate for ERAS facilities being 68.8% (IQR, 56.2%-81.2%) vs 50.0% (IQR, 37.5%-56.2%) at non-ERAS centers (P <.001). Among the patients with the highest and lowest quartiles of adherence to ERAS components, the patients with the highest adherence had fewer overall postoperative complications (144 [10.6%] vs 270 [13.0%]; OR, 0.80; 95% CI, 0.64-0.99; P <.001) and moderate to severe postoperative complications (59 [4.4%] vs 143 [6.9%]; OR, 0.62; 95% CI, 0.45-0.84; P <.001) and shorter median length of hospital stay (4 [IQR, 3-5] vs 5 [IQR, 4-6] days; OR, 0.97; 95% CI, 0.96-0.99; P <.001). Conclusions and Relevance: An increase in adherence to the ERAS program was associated with a decrease in postoperative complications, although only a few ERAS items were individually associated with improved outcomes

The ratio of horizontal to vertical displacement in solar oscillations estimated from combined SO/PHI and SDO/HMI observations

In order to make accurate inferences about the solar interior using helioseismology, it is essential to understand all the relevant physical effects on the observations. One effect to understand is the (complex-valued) ratio of the horizontal to vertical displacement of the p- and f-modes at the height at which they are observed. Unfortunately, it is impossible to measure this ratio directly from a single vantage point, and it has been difficult to disentangle observationally from other effects. In this paper we attempt to measure the ratio directly using 7.5 hours of simultaneous observations from the Polarimetric and Helioseismic Imager on board Solar Orbiter and the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory. While image geometry problems make it difficult to determine the exact ratio, it appears to agree well with that expected from adiabatic oscillations in a standard solar model. On the other hand it does not agree with a commonly used approximation, indicating that this approximation should not be used in helioseismic analyses. In addition, the ratio appears to be real-valued.Comment: Accepted for publication in Astronomy & Astrophysics. 8 pages, 8 figure

The Pochonia chlamydosporia Serine Protease Gene vcp1 Is Subject to Regulation by Carbon, Nitrogen and pH: Implications for Nematode Biocontrol

The alkaline serine protease VCP1 of the fungus Pochonia chlamydosporia belongs to a family of subtilisin-like enzymes that are involved in infection of nematode and insect hosts. It is involved early in the infection process, removing the outer proteinaceous vitelline membrane of nematode eggs. Little is known about the regulation of this gene, even though an understanding of how nutrients and other factors affect its expression is critical for ensuring its efficacy as a biocontrol agent. This paper provides new information on the regulation of vcp1 expression. Sequence analysis of the upstream regulatory region of this gene in 30 isolates revealed that it was highly conserved and contained sequence motifs characteristic of genes that are subject to carbon, nitrogen and pH-regulation. Expression studies, monitoring enzyme activity and mRNA, confirmed that these factors affect VCP1 production. As expected, glucose reduced VCP1 expression and for a few hours so did ammonium chloride. Surprisingly, however, by 24 h VCP1 levels were increased in the presence of ammonium chloride for most isolates. Ambient pH also regulated VCP1 expression, with most isolates producing more VCP1 under alkaline conditions. There were some differences in the response of one isolate with a distinctive upstream sequence including a variant regulatory-motif profile. Cryo-scanning electron microscopy studies indicated that the presence of nematode eggs stimulates VCP1 production by P. chlamydosporia, but only where the two are in close contact. Overall, the results indicate that readily-metabolisable carbon sources and unfavourable pH in the rhizosphere/egg-mass environment may compromise nematode parasitism by P. chlamydosporia. However, contrary to previous indications using other nematophagous and entomopathogenic fungi, ammonium nitrate (e.g. from fertilizers) may enhance biocontrol potential in some circumstances

Coronal voids and their magnetic nature

Context: Extreme ultraviolet (EUV) observations of the quiet solar atmosphere reveal extended regions of weak emission compared to the ambient quiescent corona. The magnetic nature of these coronal features is not well understood. // Aims: We study the magnetic properties of the weakly emitting extended regions, which we name coronal voids. In particular, we aim to understand whether these voids result from a reduced heat input into the corona or if they are associated with mainly unipolar and possibly open magnetic fields, similar to coronal holes. // Methods: We defined the coronal voids via an intensity threshold of 75% of the mean quiet-Sun (QS) EUV intensity observed by the high-resolution EUV channel (HRIEUV) of the Extreme Ultraviolet Imager on Solar Orbiter. The line-of-sight magnetograms of the same solar region recorded by the High Resolution Telescope of the Polarimetric and Helioseismic Imager allowed us to compare the photospheric magnetic field beneath the coronal voids with that in other parts of the QS. // Results: The coronal voids studied here range in size from a few granules to a few supergranules and on average exhibit a reduced intensity of 67% of the mean value of the entire field of view. The magnetic flux density in the photosphere below the voids is 76% (or more) lower than in the surrounding QS. Specifically, the coronal voids show much weaker or no network structures. The detected flux imbalances fall in the range of imbalances found in QS areas of the same size. // Conclusions: We conclude that coronal voids form because of locally reduced heating of the corona due to reduced magnetic flux density in the photosphere. This makes them a distinct class of (dark) structure, different from coronal holes