Thermochromatography study of volatile polonium species in various gas atmospheres

Phenomena related to the volatilization of polonium and its compounds are critical issues for the safety assessment of the innovative lead–bismuth cooled type of nuclear reactor or accelerator driven systems. The formation and volatilization of different species of polonium and their interaction with fused silica was studied by thermochromatography using carrier gases with varied redox potential. The obtained results show that under inert and reducing conditions in the absence of moisture, elemental polonium is formed. Polonium compounds more volatile than elemental polonium can be formed if traces of moisture are present in both inert and reducing carrier gas. The use of dried oxygen as carrier gas leads to the formation of polonium oxides, which are less volatile than elemental polonium. It was also found that the volatility of polonium oxides increases with increasing oxidation state. In the presence of moisture in an oxidizing carrier gas, species are formed that are more volatile than the oxides and less volatile than the elemental polonium. Considering the redox potential of the carrier gas those species are likely oxyhydroxides.

High Resolution Transmission Spectroscopy as a Diagnostic for Jovian Exoplanet Atmospheres: Constraints from Theoretical Models

We present high resolution transmission spectra of giant planet atmospheres from a coupled 3-D atmospheric dynamics and transmission spectrum model that includes Doppler shifts which arise from winds and planetary motion. We model jovian planets covering more than two orders of magnitude in incident flux, corresponding to planets with 0.9 to 55 day orbital periods around solar-type stars. The results of our 3-D dynamical models reveal certain aspects of high resolution transmission spectra that are not present in simple 1-D models. We find that the hottest planets experience strong substellar to anti-stellar (SSAS) winds, resulting in transmission spectra with net blue shifts of up to 3 km s−1, whereas less irradiated planets show almost no net Doppler shifts. Compared to 1-D models, peak line strengths are significantly reduced for the hottest atmospheres owing to Doppler broadening from a combination of rotation (which is faster for close-in planets under the assumption of tidal locking) and atmospheric winds. Finally, high resolution transmission spectra may be useful in studying the atmospheres of exoplanets with optically thick clouds since line cores for very strong transitions should remain optically thick to very high altitude. High resolution transmission spectra are an excellent observational test for the validity of 3-D atmospheric dynamics models, because they provide a direct probe of wind structures and heat circulation. Ground-based exoplanet spectroscopy is currently on the verge of being able to verify some of our modeling predictions, most notably the dependence of SSAS winds on insolation. We caution that interpretation of high resolution transmission spectra based on 1-D atmospheric models may be inadequate, as 3-D atmospheric motions can produce a noticeable effect on the absorption signatures.

ANALYTICAL MODELS OF EXOPLANETARY ATMOSPHERES. I. ATMOSPHERIC DYNAMICS VIA THE SHALLOW WATER SYSTEM

Within the context of exoplanetary atmospheres, we present a comprehensive linear analysis of forced, damped, magnetized shallow water systems, exploring the effects of dimensionality, geometry (Cartesian, pseudo-spherical, and spherical), rotation, magnetic tension, and hydrodynamic and magnetic sources of friction. Across a broad range of conditions, we find that the key governing equation for atmospheres and quantum harmonic oscillators are identical, even when forcing (stellar irradiation), sources of friction (molecular viscosity, Rayleigh drag, and magnetic drag), and magnetic tension are included. The global atmospheric structure is largely controlled by a single key parameter that involves the Rossby and Prandtl numbers. This near-universality breaks down when either molecular viscosity or magnetic drag acts non-uniformly across latitude or a poloidal magnetic field is present, suggesting that these effects will introduce qualitative changes to the familiar chevron-shaped feature witnessed in simulations of atmospheric circulation. We also find that hydrodynamic and magnetic sources of friction have dissimilar phase signatures and affect the flow in fundamentally different ways, implying that using Rayleigh drag to mimic magnetic drag is inaccurate. We exhaustively lay down the theoretical formalism (dispersion relations, governing equations, and time-dependent wave solutions) for a broad suite of models. In all situations, we derive the steady state of an atmosphere, which is relevant to interpreting infrared phase and eclipse maps of exoplanetary atmospheres. We elucidate a pinching effect that confines the atmospheric structure to be near the equator. Our suite of analytical models may be used to develop decisively physical intuition and as a reference point for three-dimensional magnetohydrodynamic simulations of atmospheric circulation.

Analytical Models of Exoplanetary Atmospheres. II. Radiative Transfer via the Two-Stream Approximation

We present a comprehensive analytical study of radiative transfer using the method of moments and include the effects of non-isotropic scattering in the coherent limit. Within this unified formalism, we derive the governing equations and solutions describing two-stream radiative transfer (which approximates the passage of radiation as a pair of outgoing and incoming fluxes), flux-limited diffusion (which describes radiative transfer in the deep interior) and solutions for the temperature-pressure profiles. Generally, the problem is mathematically under-determined unless a set of closures (Eddington coefficients) is specified. We demonstrate that the hemispheric (or hemi-isotropic) closure naturally derives from the radiative transfer equation if energy conservation is obeyed, while the Eddington closure produces spurious enhancements of both reflected light and thermal emission. We concoct recipes for implementing two-stream radiative transfer in stand-alone numerical calculations and general circulation models. We use our two-stream solutions to construct toy models of the runaway greenhouse effect. We present a new solution for temperature-pressure profiles with a non-constant optical opacity and elucidate the effects of non-isotropic scattering in the optical and infrared. We derive generalized expressions for the spherical and Bond albedos and the photon deposition depth. We demonstrate that the value of the optical depth corresponding to the photosphere is not always 2/3 (Milne's solution) and depends on a combination of stellar irradiation, internal heat and the properties of scattering both in optical and infrared. Finally, we derive generalized expressions for the total, net, outgoing and incoming fluxes in the convective regime.

ON THE EXISTENCE OF SHOCKS IN IRRADIATED EXOPLANETARY ATMOSPHERES

Supersonic flows are expected to exist in the atmospheres of irradiated exoplanets, but the question of whether shocks develop lingers. Specifically, it reduces to whether continuous flow in a closed loop may become supersonic and if some portions of the supersonic flow steepen into shocks. We first demonstrate that continuous, supersonic flow may exist in two flavors: isentropic and non-isentropic, with shocks being included in the latter class of solutions. Supersonic flow is a necessary but insufficient condition for shocks to develop. The development of a shock requires the characteristics of neighboring points in a flow to intersect. We demonstrate that the intersection of characteristics may be quantified via the knowledge of the Mach number. Finally, we examine three-dimensional simulations of hot Jovian atmospheres and demonstrate that shock formation is expected to occur mostly on the dayside hemisphere, upstream of the substellar point, because the enhanced temperatures near the substellar point provide a natural pressure barrier for the returning flow. Understanding the role of shocks in irradiated exoplanetary atmospheres is relevant to correctly modeling observables such as the peak offsets of infrared phase curves.

ON THE STABILITY OF SUPER-EARTH ATMOSPHERES

We investigate the stability of super-Earth atmospheres around M stars using a seven-parameter, analytical framework. We construct stability diagrams in the parameter space of exoplanetary radius versus semimajor axis and elucidate the regions in which the atmospheres are stable against the condensation of their major constituents, out of the gas phase, on their permanent nightside hemispheres. We find that super-Earth atmospheres that are nitrogen-dominated (Earth-like) occupy a smaller region of allowed parameter space, compared to hydrogen-dominated atmospheres, because of the dual effects of diminished advection and enhanced radiative cooling. Furthermore, some super-Earths which reside within the habitable zones of M stars may not possess stable atmospheres, depending on the mean molecular weight and infrared photospheric pressure of their atmospheres. We apply our stability diagrams to GJ 436b and GJ 1214b, and demonstrate that atmospheric compositions with high mean molecular weights are disfavored if these exoplanets possess solid surfaces and shallow atmospheres. Finally, we construct stability diagrams tailored to the Kepler data set, for G and K stars, and predict that about half of the exoplanet candidates are expected to harbor stable atmospheres if Earth-like conditions are assumed. We include 55 Cancri e and CoRoT-7b in our stability diagram for G stars

THE EFFECTS OF IRRADIATION ON HOT JOVIAN ATMOSPHERES: HEAT REDISTRIBUTION AND ENERGY DISSIPATION

Hot Jupiters, due to the proximity to their parent stars, are subjected to a strong irradiating flux that governs their radiative and dynamical properties. We compute a suite of three-dimensional circulation models with dual-band radiative transfer, exploring a relevant range of irradiation temperatures, both with and without temperature inversions. We find that, for irradiation temperatures T irr lsim 2000 K, heat redistribution is very efficient, producing comparable dayside and nightside fluxes. For T irr ≈ 2200-2400 K, the redistribution starts to break down, resulting in a high day-night flux contrast. Our simulations indicate that the efficiency of redistribution is primarily governed by the ratio of advective to radiative timescales. Models with temperature inversions display a higher day-night contrast due to the deposition of starlight at higher altitudes, but we find this opacity-driven effect to be secondary compared to the effects of irradiation. The hotspot offset from the substellar point is large when insolation is weak and redistribution is efficient, and decreases as redistribution breaks down. The atmospheric flow can be potentially subjected to the Kelvin-Helmholtz instability (as indicated by the Richardson number) only in the uppermost layers, with a depth that penetrates down to pressures of a few millibars at most. Shocks penetrate deeper, down to several bars in the hottest model. Ohmic dissipation generally occurs down to deeper levels than shock dissipation (to tens of bars), but the penetration depth varies with the atmospheric opacity. The total dissipated Ohmic power increases steeply with the strength of the irradiating flux and the dissipation depth recedes into the atmosphere, favoring radius inflation in the most irradiated objects. A survey of the existing data, as well as the inferences made from them, reveals that our results are broadly consistent with the observational trends.

Mechanical Degradation of Tungsten Alloys at Extreme Temperatures in Vacuum and Oxidation Atmospheres

Mechanical degradation of tungsten alloys at extreme temperatures in vacuum and oxidation atmospheres.

Máquinas o atmósferas: La estética de la energía en la arquitectura, 1750-2000 = From Machines to Atmospheres: The Aesthetics of Energy in Architecture, 1750-2000

La energía es ya un tema arquitectónico, pero su incorporación al proyecto ha sido hasta ahora fundamentalmente técnica, dando pie a una especie de funcionalismo ecológico cuyo destino es acaso repetir los errores de los viejos funcionalismos en su confianza de encontrar modos ‘objetivos’ de transmutar la energía en forma construida, pero sin que en tal proceso parezca haber hueco para mediaciones de tipo estético. Sin embargo, son precisamente tales mediaciones las que necesitan analizarse para que la adopción de los temas energéticos resulte fructífera en la arquitectura, y asimismo para dar cuenta de otras perspectivas complementarias —filosóficas, científicas, artísticas— que hoy forman el complejo campo semántico de la energía. Partiendo de la fecha de 1750 —que da comienzo simbólicamente al proceso de contaminaciones ‘modernas’ entre la arquitectura y otras disciplinas—, esta tesis analiza los diferentes modos con los que proyectos y edificios han expresado literal y analógicamente ciertos temas o ideales energéticos, demostrando la existencia de una ‘estética de la energía’ en la arquitectura y también de una tradición proyectual e intelectual sostenida en ella. Con este fin, se han seleccionados siete metáforas que vinculan tanto técnica como ideológicamente a la arquitectura con la energía: la metáfora de la máquina, asociada al ideal de movimiento y la autorregulación; las metáforas del arabesco, del cristal y del organismo, afines entre sí en su modo de dar cuenta del principio de la morfogénesis o energía creadora de la naturaleza; la metáfora de la actividad interna de los materiales; la metáfora del gradiente, que expresa la condición térmica y climática de la arquitectura, y, finalmente, la de la atmósfera que, recogiendo los sentidos anteriores, los actualiza en el contexto de la estética contemporánea. La selección de estas siete metáforas se ha llevado a cabo después de un barrido exhaustivo de la bibliografía precedente, y ha estructurado un relato cuyo método combina la perspectiva general —que permite cartografiar las continuidades históricas— con la cercana —que atiende a las problemas específicos de cada tema o metáfora—, complementándolas con una aproximación de sesgo iconográfico cuyo propósito es incidir en los vínculos que se dan entre lo ideológico y lo morfológico. El análisis ha puesto de manifiesto cómo detrás de cada una de estas metáforas se oculta un principio ideológico común —la justificación de la arquitectura desde planteamientos externos procedentes de la ciencia, la filosofía y el arte—, y cómo en cada uno de los casos estudiados las asimilaciones más fructíferas de la energía se han producido según mecanismos de mímesis analógica que inciden más en los procesos que en las formas que estos generan, y que en último término son de índole estética, lo cual constituye un indicio de los métodos de la arquitectura por venir. ABSTRACT Although it is already an architectural theme, the matter of incorporating energy into projects has up to now been mainly technical, giving rise to a kind of ecological functionalism which may be bound to old funcionalist mistakes in hopes of finding “objective” ways of transmuting energy into built forms without aesthetic considerations. However, it is precisely such considerations that need to be analyzed if the adoption of energy issues in architecture is to bear fruit and also to account for other complementary perspectives – philosophical, scientific, artistic – which today form the complex fabric of the energy semantic field. Beginning in 1750 – symbolic start of ‘modern’ contaminations between architecture and other disciplines –, this thesis analyzes the different ways in which projects and buildings have literally and analogically expressed certain subjects or ideals on energy, and demonstrates the existence of an “aesthetics of energy” in architecture, as well as of an intellectual and design tradition based on such aesthetics. For this purpose, seven metaphors are selected to link energy to architecture both technically and ideologically: the machine’s metaphor, associated with the ideal of mouvement and self-regulation; the arabesque, glass and the organism’s metaphors, which account for the morphogenesis principle, i.e. creative energy of nature; the metaphor linked to matter and the ideal of internal activity; the gradient’s metaphor, which expressed the thermal and climatic condition of architecture, and, finally, that of the atmosphere which, collecting the above meanings, updates them in the context of contemporary aesthetics. The selection of these seven metaphors was carried out after a thorough scan of the preceding literature, and has structured a reasoning that combines the overview method – which accounts for historical continuities – with the nearby one – which meets the specifics problems of each theme or metaphor –, both supplemented with an iconographic bias, the purpose of which is to visually express the links existing between the ideological and the morphological. So presented, the analysis shows how, behind each of these metaphors, lies a common ideological principle – the justification of architecture from scientific, philosophical and artistic “external” angles –, and how in each of the studied cases the most successful assimilation of energy were those produced by aesthetic mechanisms of analogical mimesis not focused in forms but in processes that generate them: an indication of the methods of architecture to come.

Sonic anemometry of planetary atmospheres

The application of a recently developed model of sonic anemometers measuring process has revealed that these sensors cannot be considered as absolute ones when measuring spectral characteristics of turbulent wind speed since it is demonstrated that the ratios of measured to real spectral density functions depend on the composition and temperature of the considered planetary atmosphere. The new model of the measuring process of sonic anemometers is applied to describe the measuring characteristics of these sensors as fluid/flow dependent (against the traditional hypothesis of fluid/flow independence) and hence dependent on the considered planetary atmosphere. The influence of fluid and flow characteristics (quantified via the Mach number of the flow) and the influence of the design parameters of sonic anemometers (mainly represented by time delay between pulses shots and geometry) on turbulence measurement are quantified for the atmospheres of Mars, Jupiter, and Earth. Important differences between the behavior of these sensors for the same averaged wind speed in the three considered atmospheres are detected in terms of characteristics of turbulence measurement as well as in terms of optimum values of anemometer design parameters for application on the different considered planetary atmospheres. These differences cannot be detected by traditional models of sonic anemometer measuring process based on line averaging along the sonic acoustic paths.