Through the magnifying glass: ALMA acute viewing of the intricate nebular architecture of OH231.8+4.2

We present continuum and molecular line emission ALMA observations of OH 231.8+4.2, a well studied bipolar nebula around an asymptotic giant branch (AGB) star. The high angular resolution (~0.2-0.3 arcsec) and sensitivity of our ALMA maps provide the most detailed and accurate description of the overall nebular structure and kinematics of this object to date. We have identified a number of outflow components previously unknown. Species studied in this work include 12CO, 13CO, CS, SO, SO2, OCS, SiO, SiS, H3O+, Na37Cl, and CH3OH. The molecules Na37Cl and CH3OH are first detections in OH 231.8+4.2, with CH3OH being also a first detection in an AGB star. Our ALMA maps bring to light the totally unexpected position of the mass-losing AGB star (QX Pup) relative to the large-scale outflow. QX Pup is enshrouded within a compact (<60 AU) parcel of dust and gas (clump S) in expansion (V~5-7 km/s) that is displaced by 0.6arcsec to the south of the dense equatorial region (or waist) where the bipolar lobes join. Our SiO maps disclose a compact bipolar outflow that emerges from QX Pup's vicinity. This outflow is oriented similarly to the large-scale nebula but the expansion velocities are about ten times lower (~35 km/s). We deduce short kinematical ages for the SiO outflow, ranging from ~50-80 yr, in regions within ~150 AU, to ~400-500 yr at the lobe tips (~3500 AU). Adjacent to the SiO outflow, we identify a small-scale hourglass-shaped structure (mini-hourglass) that is probably made of compressed ambient material formed as the SiO outflow penetrates the dense, central regions of the nebula. The lobes and the equatorial waist of the mini-hourglass are both radially expanding with a constant velocity gradient. The mini-waist is characterized by extremely low velocities, down to ~1 km/s at ~150 AU, which tentatively suggest the presence of a stable structure. (abridged

The disrupted molecular envelope of Frosty Leo

We present maps of CO emission in the protoplanetary nebula Frosty Leo. Observations of the rotational transitions ^(12)CO J=2-1 and 1-0 have been obtained with the IRAM interferometer and the OVRO array. The molecular envelope of Frosty Leo is found to be complex and compact; most of the gas extends ≾6" and shows a structure that is very different to the extended optical nebula. It is composed of a central ring-like structure, whose symmetry axis is inclined ~-40° with respect to the sky plane and expands at speeds of up to ~30 km s^(-1), and high-velocity jets distributed along the symmetry axis of the ring, which reach expansion velocities as high as ~75 km s^(-1). The symmetry axis of the molecular jets in the plane of the sky coincides with the direction of some jet-like features seen in the optical, which are not aligned at all with the main symmetry axis of the optical nebula. The brightness distribution of the ring presents a clumpy structure. We have modeled the spatio-kinematical distribution of, and the excitation conditions in, the molecular envelope. For both transitions, the ^(12)CO emission is found to be very optically thick in the center of the nebula. From our best-fit model, we find that the nebular particle density varies between ~10^5 cm^(-3) and ~10^3 cm^(-3), and that the rotational temperature is very low, ~10 K. The kinematical lifetime of the molecular jets is ~1700 yr, long in comparison with the lifetime of the post-AGB winds of most PPNe. It is very remarkable that the bulk of the gas accelerated during the post-AGB phase of Frosty Leo is located within the central ring, reaching expansion velocities of up to ~30 km s^(-1). The central ring-like distribution of Frosty Leo is probably not the undisrupted remnant of the previous AGB envelope (as found for most PPNe), but its dynamics likely result from multiple post-AGB interactions

Inherently Safer Design and Optimization of Intensified Separation Processes for Furfural Production

Currently furfural production has been the subject of increased interest because it is a biobased chemical able to compete with fossil-based chemicals. Furfural is characterized by flammability, explosion, and toxicity properties. Improper handling and process design can lead to catastrophic accidents. Hence it is of most importance to use inherent safety concepts during the design stage. This work is the first to present several new downstream separation processes for furfural purification, which are designed using an optimization approach that simultaneously considers safety criteria in addition to the total annual cost and the eco-indicator 99. The proposed schemes include thermally coupled configuration, thermodynamic equivalent configuration, dividing-wall column, and a heat integrated configuration. These are compared with the traditional separation process of furfural known as the Quaker Oats Process. The results show that because of a large amount of water present in the feed, similar values are obtained for total annual cost and eco-indicator 99 in all cases. Moreover, the topology of the processes has an important role in the safety criteria. The thermodynamic equivalent configuration resulted as the safest alternative with a 40% reduction of the inherent risk with respect to the Quaker Oats Process, and thus it is the safest option to purify furfural

Colaboración internacional y buenas prácticas en la gestión de enfermedades crónicas complejas a través de herramientas web 2.0: Observatorio de prácticas innovadoras en el manejo de enfermedades crónicas complejas OPIMEC

Ponencias de la Segunda Conferencia internacional sobre brecha digital e inclusión social, celebrada del 28 al 30 de octubre de 2009 en la Universidad Carlos III de MadridLas enfermedades crónicas (EC) constituyen un reto de salud mundial en el siglo XXI. La OMS las define como enfermedades de larga duración por lo general de progresión lenta y prevé que en 2020 serán responsables del 73% de las muertes y del 60% de la carga global de enfermedad (World Health Organization, 2002). Es primordial que la comunidad internacional de salud pública y de gestión sanitaria conozca y comparta información sobre los avances en las prácticas tecnológicas y organizativas más innovadoras en gestión de EC, con énfasis en las EC Complejas (ECC) asociadas a una mayor pérdida de autonomía y grado de dependencia y discapacidad. Con este propósito, a mediados de 2006, la Dirección General de Innovación Sanitaria, Sistemas y Tecnología de la Consejería de Salud de la Junta de Andalucía crea el «Observatorio de Prácticas Innovadoras para el Manejo de Enfermedades Crónicas Complejas» (OPIMEC) que impulsa la participación y generación de conocimiento en información sanitaria para profesionales y una Plataforma de Red en el ámbito de la gestión de ECC para el fomento de alianzas y colaboraciones desde Andalucía basadas en dar y recibir conocimiento abierto entre personas, equipos y organizaciones (Jadad AR, 1999, p. 761-764; Jadad AR, 2000, p.362-365). La Web del Observatorio de Prácticas Innovadoras en el Manejo de Enfermedades Crónicas Complejas (OPIMEC), http://www.opimec.org, va centrada en la creación de una plataforma basada en la Web 2.0. que permite el acceso y la edición colaborativa de contenidos para profesionales. El objetivo fundamental de esta plataforma es compartir y colaborar en la generación y difusión de conocimiento, todo ello facilitado con herramientas innovadoras de la Web 2.0. como son la publicación de contenidos, la votación, comentarios sobre los contenidos, la sindicación de contenidos y la creación de comunidades abiertas de trabajo colaborativo. El proyecto OPIMEC cuenta con una cadena de procesos de gestión de la información de los que podemos destacar su forma colaborativa de crear conocimiento por todas las personas usuarias de la plataforma, un equipo editorial encargado de asegurar la calidad de los contenidos y una evaluación por pares de las prácticas y organizaciones propuestas en la Web. Desde la edición, hasta la publicación y su distribución final el conocimiento es examinado metódicamente. Este proceso es automatizado a través de herramientas de software libre creadas para OPIMEC y asesorado por su Consejo Asesor Internacional. Así pues, la plataforma Web 2.0 que da soporte al observatorio OPIMEC está construida sobre tecnologías libres como: Framework Web Django (impulsado por Google Inc. entre otros), MySQL y GNU/Linux. La elección de esta combinación tecnológica se ha realizado tras un análisis exhaustivo sobre las tecnologías abiertas disponibles, en base a criterios de eficiencia, productividad y adaptabilidad a las necesidades actuales y futuras de OPIMEC. La Web OPIMEC tiene intención y vocación de convertirse en un destacado proyecto a nivel mundial con clara vertiente de cooperación internacional e innovación, mejorando la calidad de vida de la ciudadanía, aprovechando las herramientas que ofrece la difundida red global de Internet y promocionando la participación e iniciativa de los y las profesionales. Nuestra Web OPIMEC está estructurada en espacios que facilitan y propician la participación y consecución de los objetivos del proyecto, con el fin de que la asimilación de sus contenidos por parte de las personas usuarias sea eficiente y efectiva. Podemos encontrar en ella, herramientas existentes en las redes sociales así como algunas nuevas desarrolladas específicamente para OPIMEC, como son los “documentos colaborativos”, que facilitarán el trabajo, la conexión y la participación de profesionales desde cualquier parte del mundo, pudiendo así aprovechar los recursos al máximo, Se dispone por tanto de destacadas herramientas como una base de datos actualizada de eventos, noticias, recursos y documentos, directorios y mapas de organizaciones, prácticas y personas innovadoras, espacios de comunidad en las que los equipos de trabajo pueden desarrollarse, comunicarse y complementarse con otras personas usuarias, compartiendo buenas prácticas, innovación y contenidos novedosos en el manejo de enfermedades crónicas complejas. El aspecto importante de la plataforma es que las personas usuarias son de forma democrática, creadores, evaluadores y consumidores de los contenidos publicados, siendo así una herramienta de trabajo construida, ampliada, valorada y seguida por toda la comunidad de profesionales; facilitando la difusión del conocimiento construido por y para todos y todas los profesionales sanitarios, personal investigador, ciudadanos y ciudadanas en general en el manejo de enfermedades crónicas complejas. Un conocimiento ampliamente compartido es la clave para aumentar y mejorar el bienestar social y la calidad de vida

Echelle long-slit optical spectroscopy of evolved stars

We present echelle long-slit optical spectra of a sample of objects evolving off the AGB, most of them in the pre-planetary nebula (pPN) phase, obtained with the ESI and MIKE spectrographs at Keck-II and Magellan-I, respectively. The total wavelength range covered with ESI (MIKE) is ~3900 to 10900 A (~3600 to 7200A). In this paper, we focus our analysis mainly on the Halpha profiles. Prominent Halpha emission is detected in half of the objects, most of which show broad Halpha wings (up to ~4000 km/s). In the majority of the Halpha-emission sources, fast, post-AGB winds are revealed by P-Cygni profiles. In ~37% of the objects Halpha is observed in absorption. In almost all cases, the absorption profile is partially filled with emission, leading to complex, structured profiles that are interpreted as an indication of incipient post-AGB mass-loss. All sources in which Halpha is seen mainly in absorption have F-G type central stars, whereas sources with intense Halpha emission span a larger range of spectral types from O to G. Shocks may be an important excitation agent of the close stellar surroundings for objects with late type central stars. Sources with pure emission or P Cygni Halpha profiles have larger J-K color excess than objects with Halpha mainly in absorption, which suggests the presence of warm dust near the star in the former. The two classes of profile sources also segregate in the IRAS color-color diagram in a way that intense Halpha-emitters have dust grains with a larger range of temperatures. (abridged)Comment: 68 pages, 14 figures, accepted for publication in ApJS (abstract abridged

Experimental and theoretical assessment of native oxide in the superconducting TaN

In this manuscript, we show through an experimental-computational proof of concept the native oxide formation into superconducting TaN films. First, TaN was synthesized at an ultra-high vacuum system by reactive pulsed laser deposition and characterized in situ by X-ray photoelectron spectroscopy. The material was also characterized ex situ by X-ray diffraction, transmission electron microscopy, and the four-point probe method. It was detected that TaN contained considerable oxygen impurities (up to 26 %O) even though it was grown in an ultra-high vacuum chamber. Furthermore, the impurified TaN evidence a face-centered cubic crystalline structure only and exhibits superconductivity at 2.99 K. To understand the feasibility of the native oxide in TaN, we study the effect of incorporating different amounts of O atoms in TaN using ab-initio calculations. A thermodynamic stability analysis shows that a TaOxN1-x model increases its stability as oxygen is added, demonstrating that oxygen may always be present in TaN, even when obtained at ultra-high vacuum conditions. All analyzed models exhibit metallic behavior. Charge density difference maps reveal that N and O atoms have a higher charge density redistribution than Ta atoms. The electron localization function maps and line profiles indicate that Ta-O and Ta-N bonds are mainly ionic. As expected, stronger ionic behavior is observed in the Ta-O bonds due to the electronegativity difference between O and N atoms. Recent evidence points to superconductivity in bulk TaO, confirming the asseverations of superconductivity in our samples. The results discussed here highlight the importance of considering native oxide when reporting superconductivity in TaN films since the TaO regions formed in the compound may be key to understanding the different critical temperatures reported in the literature.Comment: 23 pages, 7 figure

Rotten Egg Nebula: The magnetic field of a binary evolved star

Most of PNe are not spherical. The loss of spherical symmetry occurs somewhere between the AGB and PN phase. The cause of this change of morphology is not yet well known, but magnetic fields are one of the possible agents. Its origin remains to be determined, and potentially requires the presence of a massive companion to the AGB star. Therefore, further detections of the magnetic field around evolved stars (in particular those thought to be part of a binary system) are crucial to improve our understanding of the origin and role of magnetism on evolved stars. One such binaries is the pre-PN OH231.8, around which a magnetic field was detected in the OH maser region of the outer circumstellar envelope. We aim to detect and infer the properties of the magnetic field of this source in the water maser region. We observed the 6_{1,6}-5_{2,3} water maser rotational transition to determine its linear and circular polarization. These emissions are located within the inner regions of OH231.8 (at few tens of AU). We detected 30 water maser features, which occur in two distinct regions that are moving apart with a velocity on the sky of 2.3 mas/year. Taking into account the inclination angle of the source, this corresponds to an average separation velocity of 21 km/s. Based on the velocity gradient of the maser emission, the masers appear to be dragged along the direction of the nebula jet. Linear polarization is present in 3 of the features, and circular polarization was detected in the 2 brightest ones. We found that the strength of the magnetic field is |B_{||}|~45 mG which, when assuming a toroidal magnetic field, implies B~2.5 G on the stellar surface. The morphology of the field is not yet determined, but the high scatter found on the directions of the linear polarization vectors could indicate that the masers occur near the tangent points of a toroidal field.Comment: 7 pages, 4 figure

Solitary waves in nonlinear phononic crystals

[EN] We discuss two possible regimes of solitary wave formation in acoustic layered media. In the weakly dispersive limit, KdV-type solitons are formed, consisting of broad pulses with a width much larger than the lattice periodicity. Such KdV solitons are shown to exist even far from the weakly dispersive conditions. On the other hand, in the strongly dispersive regime, gap acoustic solitons are demonstrated. They are formed by a fast carrier wave inside the band-gap of the structure, near the Bragg frequency (whose propagation is not allowed in the case of linear waves), modulated by a wide envelope, whose width lies inside the gap. Gap solitons propagate slower than linear waves, or can be even reach a stationary non-propagating state within the medium. The parameters for a realistic acoustic medium supporting both types of solitary waves are discussedThe work was supported by Spanish Ministry of Economy and Innovation (MINECO) and European Union FEDER through project FIS2015-65998-C2-2.Mehrem, A.; Picó Vila, R.; Sánchez Morcillo, VJ.; García-Raffi, LM.; Salmerón-Contreras, LJ.; Jimenez, N.; Staliunas, K. (2016). Solitary waves in nonlinear phononic crystals. Universidade do Porto. 1-7. http://hdl.handle.net/10251/183355S1

A high resolution line survey of IRC+10216 with Herschel. First results: Detection of warm silicon dicarbide SiC2

We present the first results of a high-spectral-resolution survey of the carbon-rich evolved star IRC+10216 that was carried out with the HIFI spectrometer onboard Herschel. This survey covers all HIFI bands, with a spectral range from 488 to 1901GHz. In this letter we focus on the band-1b spectrum, in a spectral range 554.5-636.5GHz, where we identified 130 spectral features with intensities above 0.03 K and a signal-to-noise ratio >5. Detected lines arise from HCN, SiO, SiS, CS, CO, metal-bearing species and, surprisingly, silicon dicarbide (SiC2). We identified 55 SiC2 transitions involving energy levels between 300 and 900 K. By analysing these rotational lines, we conclude that SiC2 is produced in the inner dust formation zone, with an abundance of ~2x10^-7 relative to molecular hydrogen. These SiC2 lines have been observed for the first time in space and have been used to derive an SiC2 rotational temperature of ~204 K and a source-averaged column density of ~6.4x10^15 cm^-2. Furthermore, the high quality of the HIFI data set was used to improve the spectroscopic rotational constants of SiC2.Comment: A&A HIFI Special Issue, 201