A Maximum Radius for Habitable Planets

We compute the maximum radius a planet can have in order to fulfill two constraints that are likely necessary conditions for habitability: 1- surface temperature and pressure compatible with the existence of liquid water, and 2- no ice layer at the bottom of a putative global ocean, that would prevent the operation of the geologic carbon cycle to operate. We demonstrate that, above a given radius, these two constraints cannot be met: in the Super-Earth mass range (1-12 M-earth), the overall maximum that a planet can have varies between 1.8 and 2.3 R-earth. This radius is reduced when considering planets with higher Fe/Si ratios, and taking into account irradiation effects on the structure of the gas envelope.

The unstable CO2 feedback cycle on ocean planets

Ocean planets are volatile-rich planets, not present in our Solar system, which are thought to be dominated by deep, global oceans. This results in the formation of high-pressure water ice, separating the planetary crust from the liquid ocean and, thus, also from the atmosphere. Therefore, instead of a carbonate-silicate cycle like on the Earth, the atmospheric carbon dioxide concentration is governed by the capability of the ocean to dissolve carbon dioxide (CO2). In our study, we focus on the CO2 cycle between the atmosphere and the ocean which determines the atmospheric CO2 content. The atmospheric amount of CO2 is a fundamental quantity for assessing the potential habitability of the planet's surface because of its strong greenhouse effect, which determines the planetary surface temperature to a large degree. In contrast to the stabilizing carbonate-silicate cycle regulating the long-term CO2 inventory of the Earth atmosphere, we find that the CO2 cycle feedback on ocean planets is negative and has strong destabilizing effects on the planetary climate. By using a chemistry model for oceanic CO2 dissolution and an atmospheric model for exoplanets, we show that the CO2 feedback cycle can severely limit the extension of the habitable zone for ocean planets.

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.

In search of planets and life around other stars

The discovery of over a dozen low-mass companions to nearby stars has intensified scientific and public interest in a longer term search for habitable planets like our own. However, the nature of the detected companions, and in particular whether they resemble Jupiter in properties and origin, remains undetermined.

Brown dwarfs: At last filling the gap between stars and planets

Until the mid-1990s a person could not point to any celestial object and say with assurance that “here is a brown dwarf.” Now dozens are known, and the study of brown dwarfs has come of age, touching upon major issues in astrophysics, including the nature of dark matter, the properties of substellar objects, and the origin of binary stars and planetary systems.

Extrasolar planets

The first known extrasolar planet in orbit around a Sun-like star was discovered in 1995. This object, as well as over two dozen subsequently detected extrasolar planets, were all identified by observing periodic variations of the Doppler shift of light emitted by the stars to which they are bound. All of these extrasolar planets are more massive than Saturn is, and most are more massive than Jupiter. All orbit closer to their stars than do the giant planets in our Solar System, and most of those that do not orbit closer to their star than Mercury is to the Sun travel on highly elliptical paths. Prevailing theories of star and planet formation, which are based on observations of the Solar System and of young stars and their environments, predict that planets should form in orbit about most single stars. However, these models require some modifications to explain the properties of the observed extrasolar planetary systems.

EChO. Exoplanet characterisation observatory

A dedicated mission to investigate exoplanetary atmospheres represents a major milestone in our quest to understand our place in the universe by placing our Solar System in context and by addressing the suitability of planets for the presence of life. EChO—the Exoplanet Characterisation Observatory—is a mission concept specifically geared for this purpose. EChO will provide simultaneous, multi-wavelength spectroscopic observations on a stable platform that will allow very long exposures. The use of passive cooling, few moving parts and well established technology gives a low-risk and potentially long-lived mission. EChO will build on observations by Hubble, Spitzer and ground-based telescopes, which discovered the first molecules and atoms in exoplanetary atmospheres. However, EChO’s configuration and specifications are designed to study a number of systems in a consistent manner that will eliminate the ambiguities affecting prior observations. EChO will simultaneously observe a broad enough spectral region—from the visible to the mid-infrared—to constrain from one single spectrum the temperature structure of the atmosphere, the abundances of the major carbon and oxygen bearing species, the expected photochemically-produced species and magnetospheric signatures. The spectral range and resolution are tailored to separate bands belonging to up to 30 molecules and retrieve the composition and temperature structure of planetary atmospheres. The target list for EChO includes planets ranging from Jupiter-sized with equilibrium temperatures T_ eq up to 2,000 K, to those of a few Earth masses, with T _eq \u223c 300 K. The list will include planets with no Solar System analog, such as the recently discovered planets GJ1214b, whose density lies between that of terrestrial and gaseous planets, or the rocky-iron planet 55 Cnc e, with day-side temperature close to 3,000 K. As the number of detected exoplanets is growing rapidly each year, and the mass and radius of those detected steadily decreases, the target list will be constantly adjusted to include the most interesting systems. We have baselined a dispersive spectrograph design covering continuously the 0.4–16 μm spectral range in 6 channels (1 in the visible, 5 in the InfraRed), which allows the spectral resolution to be adapted from several tens to several hundreds, depending on the target brightness. The instrument will be mounted behind a 1.5 m class telescope, passively cooled to 50 K, with the instrument structure and optics passively cooled to \u223c45 K. EChO will be placed in a grand halo orbit around L2. This orbit, in combination with an optimised thermal shield design, provides a highly stable thermal environment and a high degree of visibility of the sky to observe repeatedly several tens of targets over the year. Both the baseline and alternative designs have been evaluated and no critical items with Technology Readiness Level (TRL) less than 4–5 have been identified. We have also undertaken a first-order cost and development plan analysis and find that EChO is easily compatible with the ESA M-class mission framework.