Does the momentum flux generated by gravitational contraction drive AGB mass-loss?

Gravitational contraction always generates a radially directed momentum flux. A particularly simple example occurs in the electron-degenerate cores of AGB stars, which contract steadily under the addition of helium ashes from shell hydrogen burning. The resulting momentum flux is quantified here. And since the cores of AGB stars lack efficient momentum cancellation mechanisms, they can maintain equilibrium by exporting their excess momentum flux to the stellar envelope, which disposes of much of it in a low velocity wind. Gravitational contraction easily accounts for the momentum flux in the solar wind, as well as the flux required to lift mass into the dust formation zone of every AGB star, whereon radiation pressure continues its ejection as a low velocity wind. This mechanism explains the dependence of the AGB mass-loss rate on core mass; its generalization to objects with angular momentum and/or strong magnetic fields suggests a novel explanation of why most planetary nebulae and proto planetary nebulae exhibit axial symmetry. Quasistatic contraction is inherently biased to the generation of the maximum possible momentum flux. Its formalism is therefore readily adapted to providing an upper limit to the momentum flux needed to sustain mass loss when this begins from a semi-continuous rather than impulsive process.Comment: 35 pages, including 1 fig and 2 tables, to appear in Astrophysical Journal -- ps documen

The Infrared Continuum Spectrum of VY CMa

We combine spectra of VY CMa obtained with the short- and long-wavelength spectrometers, SWS and LWS, on the Infrared Space Observatory to provide a first detailed continuum spectrum of this highly luminous star. The circumstellar dust cloud through which the star is observed is partially self-absorbing, which makes for complex computational modeling. We review previous work and comment on the range of uncertainties about the physical traits and mineralogical composition of the modeled disk. We show that these uncertainties significantly affect the modeling of the outflow and the estimated mass loss. In particular, we demonstrate that a variety of quite diverse models can produce good fits to the observed spectrum. If the outflow is steady, and the radiative repulsion on the dust cloud dominates the star's gravitational attraction, we show that the total dust mass-loss rate is $\sim 4\times 10^{-6}M_{\odot}$ yr$^{-1}$, assuming that the star is at a distance of 1.5 kpc. Several indications, however, suggest that the outflow from the star may be spasmodic. We discuss this and other problems facing the construction of a physically coherent model of the dust cloud and a realistic mass-loss analysis

HI in circumstellar environments

We present new results of a spectroscopic survey of circumstellar HI in the direction of evolved stars made with the Nancay Radiotelescope. The HI line at 21 cm has been detected in the circumstellar shells of a variety of evolved stars: AGB stars, oxygen-rich and carbon-rich, Semi-Regular and Miras, and Planetary Nebulae. The emissions are generally spatially resolved, i.e. larger than 4', indicating shell sizes of the order of 1 pc which opens the possibility to trace the history of mass loss over the past ~ 10^4-10^5 years. The line-profiles are sometimes composite. The individual components have generally a quasi-Gaussian shape; in particular they seldom show the double-horn profile that would be expected from the spatially resolved optically thin emission of a uniformly expanding shell. This probably implies that the expansion velocity decreases outwards in the external shells (0.1-1 pc) of these evolved stars. The HI line-profiles do not necessarily match those of the CO rotational lines. Furthermore, the centroid velocities do not always agree with those measured in the CO lines and/or the stellar radial velocities. The HI emissions may also be shifted in position with respect to the central stars. Without excluding the possibility of asymmetric mass ejection, we suggest that these two effects could also be related to a non-isotropic interaction with the local interstellar medium. HI was detected in emission towards several sources (rho Per, alpha Her, delta^2 Lyr, U CMi) that otherwise have not been detected in any radio lines. Conversely it was not detected in the two oxygen-rich stars with substantial mass-loss rate, NML Tau and WX Psc, possibly because these sources are young with hydrogen in molecular form, and/or because the temperature of the circumstellar HI gas is very low (< 5 K).Comment: Accepted for publication in The Astronomical Journa

The Effective Temperature Scale of Galactic Red Supergiants: Cool, But Not As Cool As We Thought

We use moderate-resolution optical spectrophotometry and the new MARCS stellar atmosphere models to determine the effective temperatures of 74 Galactic red supergiants. From these we find a new effective temperature scale that is significantly warmer than those in the literature. We show that this temperature scale, along with the newly derived bolometric corrections, gives much better agreement between our red supergiants and stellar evolutionary tracks. This agreement provides an independent verification of our new temperature scale. The combination of effective temperature and bolometric luminosities allows us to calculate stellar radii; the coolest and most luminous stars have radii of roughly 1500 solar radii (7 AU), in excellent accordance with the largest stellar radii predicted from current evolutionary theory. We find that similar results are obtained for the effective temperatures and bolometric luminosities using only the de-reddened V-K colors, providing a powerful demonstration of the self-consistency of the MARCS models.Comment: 32 pages, 16 figures; Accepted by the Astrophysical Journa

Improving policy coherence for food security and nutrition in South Africa: a qualitative policy analysis

Like most other low and middle-income countries, South Africa must address a rising burden of diet-related chronic disease in a situation of persistent food insecurity and undernutrition. Supply-side policy interventions are a critical component of action to address the double burden of malnutrition. However, the food supply is governed by a number of different policy sectors, and policy incoherence can occur between government action to promote a healthy food supply and objectives for economic liberalization. We analysed the coherence of food supply policy content with respect to nutrition and food security in South Africa, and conducted 14 in-depth interviews with 22 public and private sector actors to identify opportunities to improve policy coherence across sectors governing the food supply. Drawing on Sabatier’s conceptualization of actors as influential in shaping policy outcomes, we identified three coalitions of actors related to food security and nutrition in South Africa: the dominant Economic Growth coalition, the Food Security coalition, and the Health coalition. Understanding the frames, beliefs and resources held by these coalitions offers insights into the policy tensions faced by the Government of South Africa with respect to the food supply. The analysis indicates that the current reconsideration of economic policy agendas favouring liberalization in SouthAfrica, including the termination of most bilateral investment treaties, may present an opportunity for increased recognition of food security and nutrition priorities in food supply policy making. Opportunities to strengthen policy coherence across the food supply for food security and nutrition include: specific changes to economic policy relating to the food supply that achieve both food security/nutrition and economic objectives; creating links between producers and consumers, through markets and fiscal incentives that make healthy / fresh foods more accessible and affordable; increasing formal avenues for engagement by Civil Society in nutrition and food security policy making; and including consideration of the nutritional quality of the food supply in policy objectives across sectors, to create a framework for policy coherence across sectors relating to the food supply

La fabrication de composants nucléaires et son impact sur l'environnement à Chalon-sur-Saône

Entrée en service en octobre 1975, l'usine Framatome de Chalon-sur-Saône a une capacité de réalisation de huit chaudières nucléaires par an. Les auteurs décrivent la façon dont cette grande unité industrielle a été intégrée à l'environnement de la Saône-et-Loire, sur le plan de son implantation et de son impact extérieur. Ils présentent également l'environnement interne de l'usine

Interoperable Mars atmosphere data Services

International audienceModern space borne instruments produce huge datasets, especially on long-lived missions such as Mars-Express. This calls for new ways to handle the data, not only to perform mass processing, but also more basically to access them easily and efficiently. Virtual Observatory (VO) techniques developed in Astronomy during the past 15 years can be adapted to address this problem, provided they are enlarged to include specificities of Solar System studies such as coordinate systems, target-related time scales (lo- cal time and season), or measured quantities. An effort to adapt VO techniques to Solar System stud- ies has been started in the frame of the Europlanet program, first in FP7 (2009-2012) as a demonstrator, and now in Horizon2020 (2015-2019) in a more ex- tensive way. In the current program Europlanet 2020, the VESPA activity deals with the infrastructure and implements new data services. VESPA stands for Virtual European Solar and Planetary Access and supports all aspects of Solar System science. Its de- velopments are essentially based on the standards of the IVOA (International Virtual Observatory Alli- ance).As part of this enlargement, several data services related to the Martian atmosphere were recently de- signed and released, including a set of SPICAM de- rived data and a demonstrator of VO access to the Mars Climate Database. In both cases, vertical pro- files are distributed with the basic VESPA architec- ture. In this abstract, we present the two services and assess this type of access to a simulation service