Isotopes in cosmochemistry: recipe for a Solar System

Extreme isotopic variations among extraterrestrial materials provide great insights into the origin and evolution of the Solar System. In this tutorial review, we summarize how the measurement of isotope ratios can expand our knowledge of the processes that took place before and during the formation of our Solar System and its subsequent early evolution. The continuous improvement of mass spectrometers with high precision and increased spatial resolution, including secondary ion mass spectrometry (SIMS), thermal ionization mass spectrometry (TIMS) and multi collector-inductively coupled plasma-mass spectrometry (MC-ICP-MS), along with the ever growing amounts of available extraterrestrial samples have significantly increased the temporal and spatial constraints on the sequence of events that took place since and before the formation of the first Solar System condensates (i.e., Ca-Al-rich inclusions). Grains sampling distinct stellar environments with a wide range of isotopic compositions were admixed to, but possibly not fully homogenized in, the Sun's parent molecular cloud or the nascent Solar System. Before, during and after accretion of the nebula, as well as the formation and subsequent evolution of planetesimals and planets, chemical and physical fractionation processes irrevocably changed the chemical and isotopic compositions of all Solar System bodies. Since the formation of the first Solar System minerals and rocks 4.568 Gyr ago, short-and long-lived radioactive decay and cosmic ray interaction also contributed to the modification of the isotopic framework of the Solar System, and permit to trace the formation and evolution of directly accessible and inferred planetary and stellar isotopic reservoirs.

COST AND PERFORMANCE TRADEOFFS OF ALTERNATIVE SOLAR-DRIVEN S-CO2 BRAYTON CYCLE CONFIGURATIONS

This paper evaluates cost and performance tradeoffs of alternative supercritical carbon dioxide (s-CO2) closed-loop Brayton cycle configurations with a concentrated solar heat source. Alternative s-CO2 power cycle configurations include simple, recompression, cascaded, and partial cooling cycles. Results show that the simple closed-loop Brayton cycle yielded the lowest power-block component costs while allowing variable temperature differentials across the s-CO2 heating source, depending on the level of recuperation. Lower temperature differentials led to higher sensible storage costs, but cycle configurations with lower temperature differentials (higher recuperation) yielded higher cycle efficiencies and lower solar collector and receiver costs. The cycles with higher efficiencies (simple recuperated, recompression, and partial cooling) yielded the lowest overall solar and power-block component costs for a prescribed power output.

COUPLED OPTICAL-THERMAL-FLUID MODELING OF A DIRECTLY HEATED TUBULAR SOLAR RECEIVER FOR SUPERCRITICAL CO2 BRAYTON CYCLE

Recent studies have evaluated closed-loop supercritical carbon dioxide (s-CO2) Brayton cycles to be a higher energy density system in comparison to conventional superheated steam Rankine systems. At turbine inlet conditions of 923K and 25 MPa, high thermal efficiency (similar to 50%) can be achieved. Achieving these high efficiencies will make concentrating solar power (CSP) technologies a competitive alternative to current power generation methods. To incorporate a s-CO2 Brayton power cycle in a solar power tower system, the development of a solar receiver capable of providing an outlet temperature of 923 K (at 25 MPa) is necessary. The s-CO2 will need to increase in temperature by similar to 200 K as it passes through the solar receiver to satisfy the temperature requirements of a s-CO2 Brayton cycle with recuperation and recompression. In this study, an optical-thermal-fluid model was developed to design and evaluate a tubular receiver that will receive a heat input similar to 2 MWth from a heliostat field. The ray-tracing tool SolTrace was used to obtain the heat-flux distribution on the surfaces of the receiver. Computational fluid dynamics (CFD) modeling using the Discrete Ordinates (DO) radiation model was used to predict the temperature distribution and the resulting receiver efficiency. The effect of flow parameters, receiver geometry and radiation absorption by s-CO2 were studied. The receiver surface temperatures were found to be within the safe operational limit while exhibiting a receiver efficiency of similar to 85%.

A quantum dot sensitized solar cell based on vertically aligned carbon nanotube templated ZnO arrays

We report on a quantum dot sensitized solar cell (QDSSC) based on ZnO nanorod coated vertically aligned carbon nanotubes (VACNTs). Electrochemical impedance spectroscopy shows that the electron lifetime for the device based on VACNT/ZnO/CdSe is longer than that for a device based on ZnO/CdSe, indicating that the charge recombination at the interface is reduced by the presence of the VACNTs. Due to the increased surface area and longer electron lifetime, a power conversion efficiency of 1.46% is achieved for the VACNT/ZnO/CdSe devices under an illumination of one Sun (AM 1.5G, 100 mW/cm2). © 2010 Elsevier B.V.

High-resolution TEM characterization of ZnO core-shell nanowires for dye-sensitized solar cells

Recently ZnO nanowire films have been used in very promising and inexpensive dye-sensitized solar cells (DSSC). It was found that the performance of the devices can be enhanced by functionalising the nanowires with a thin metal oxide coating. This nm-scale shell is believed to tailor the electronic structure of the nanowire, and help the absorption of the dye. Core-shell ZnO nanowire structures are synthesised at low temperature (below 120°C) by consecutive hydrothermal growth steps. Different materials are investigated for the coating, including Mg, Al, Cs and Zr oxides. High resolution TEM is used to characterise the quality of both the nanowire core and the shell, and to monitor the thickness and the degree of crystallisation of the oxide coating. The interface between the nanowire core and the outer shell is investigated in order to understand the adhesion of the coating, and give valuable feedback for the synthesis process. Nanowire films are packaged into dye-sensitised solar cell prototypes; samples coated with ZrO2 and MgO show the largest enhancement in the photocurrent and open-circuit voltage and look very promising for further improvement. © 2010 IOP Publishing Ltd.

Determinación del índice de área foliar, radiación solar no interceptada por especies forestales y concentración de magnesio en hojas de café (Coffea arabica L.) en sistemas agroforestales, localizados en Masaya, Nicaragua

La presente investigación se realizó en sistemas agroforestales con Café Coffea arábiga L.)en el Municipio de Masatepe, Nicaragua, determinando el índice de área foliar, radiación solar no interceptada por especies forestales y concentración de magnesio en hojas de Café. Para determinar índice de área foliar se utilizó una metodología no destructiva y una destructiva; la medición no destructiva se basó en la técnica de fotografías hemisféricas para lo cual se utilizó una cámara Nikon Coolpix 4500 que permitió tomar fotografías de cuatro árboles de Samanea saman, Inga laurina, Simarouba glauca, Tabebuia rosea respectivamente. Porcada árbol se tomaron cuatro imágenes sobre lados opuestos del tronco (Norte, Sur, Este y Oeste), para el análisis de fotografías hemisféricas se empleó el software Gap Light Analyzer. Para contrastar la medición de índice de área foliar por método no destructivo (fotografías hemisféricas) se empleó un método destructivo basado en la recolección de 300 hojas, se tomó el peso húmedo del total de hojas de cada uno de los árboles en estudio. Del total de hojas de cada árbol se pesaron separadamente tres muestras; utilizando el planímetro LI-3000 se calculó en cada caso el área de la hoja. Una vez obtenida el área foliar de la hoja, las muestras se secaron en horno a 65° C, durante 72 h y promediadas para obtener biomasa del follaje. Dividiendo el área foliar de las muestras entre su peso seco se obtuvo el área foliar específica, posteriormente el promedio de área foliar específica de las muestras multiplicado por el peso seco total de hojas permitió calcular el área foliar del árbol. Finalmente, se obtuvo el índice de área foliar dividiendo área foliar entre el área de suelo asignada . La medición de la cantidad de radiación incidente sobre el follaje de las plantas de Café se realizó en la réplica II en CENECOOP en dos puntos de muestreo; el criterio de selección de los sitios se basó en la combinación de árboles ubicados diagonalmente y en la uniformidad de distancia entre las especies para la combinación T. rosea + S. glaucae I. laurina + S. saman. En esta réplica se realizaron análisis del contenido de magnesio en hojas de Café en las subparcelas 5, 6, 7, 8, 9, 10, 11 y 12 más dos muestras testigos en las subparcelas 13 y 14 a pleno sol. El índice de área foliar promedio para especies tropicales estimado por el método destructivo fue de 2,52 y por el método no destructivo fue de 0,85; debido a estas diferencias es necesario aplicar un factor de corrección o calibración al método no destructivo para validar ambos resultados. En la combinación I. laurina + S. saman se detectó un mayor paso de radiación solar al cafetal (29911,11lux) posiblemente debido a las características morfológicas del dosel. La concentración de magnesio más alta es de 2% la cual se encontró en las hojas de Café de la combinación T. rosea + S. glauca en nivel de insumo orgánico moderado.

Efecto del presecador solar tipo domo en el secado de granos de café orgánico (Coffea arabica L.) en fincas de pequeños productores de las cooperativas San Isidro R.L. Boaco y PROCOSER Nueva Segovia. Noviembre 2010-Febrero 2011

La obtención del producto final del rubro café conlleva una serie de procesos, entre ellos está el beneficiado (húmedo y seco). El beneficiado seco es un proceso para reducir la humedad los frutos del cafeto de su estado café pergamino mojado obtenido del beneficiado húmedo, este se realiza en patio exponiendo los granos húmedos durante varios días a los rayos directos del sol, sobre una superficie de cemento o madera. Exponiendo el café a los efectos negativos del ambiente, reduciendo la calidad, elevando los costos, mayor uso de mano de obra y corriendo riesgos constantes de contaminación y a castigos impuestos por la acopiadora en el pesaje por merma de humedad. Como una propuesta a estos riesgos se evaluó el efecto del presecador solar tipo domo en el presecado de granos de café orgánico (Coffea arabica L.), en fincas de pequeños productores de las cooperativas San Isidro R.L Boaco y PROCOSER Nueva Segovia. En el ciclo 2010-2011. Se realizó en dos fases: primera, correspondió a una investigación no experimental donde se utilizo una encuesta semi-estructurada para determinar las características de los productores (datos del productor, datos de la finca, área de café, altura de la finca, variedades de café presentes y actividades que realizan en el beneficiado húmedo). Calidad de corte y prueba de rendimiento de las diferentes localidades seleccionadas. En la segunda, se estableció un experimento unifactorial, al comparar la tecnología (pre secador tipo domo). Las variables a evaluadas fueron: área y altura de la finca, variedades de café, actividades del beneficiado húmedo, temperatura, humedad relativa, peso del grano y rendimientos. Los resultados obtenidos fueron que hubo diferencias en algunas actividades del proceso de beneficiado húmedo entre los productores de los departamentos. La pérdida de humedad en el grano de café fue mayor en el volumen de 11.36 kg/m2 en ambas localidades igualmente la pérdida del peso del grano, los menores costos variables y mayores beneficios netos se los obtuvo el tratamiento de 22.72 kg / m2 fuera del presecador tradicional en el departamento de Boaco mientras que en el departamento de Nueva Segovia fue el de 11.36 kg/m2 dentro del presecador solar tipo domo.

Enquadrar o protetor solar na categoria de medicamento?

Consultoria Legislativa - Área XVI - Saúde Pública, Sanitarismo.

O aproveitamento da energia solar no Brasil - situação e perspectivas

Consultoria Legislativa - Área XII - Recursos Minerais, Hídricos e Energéticos.

The tangential discontinuous surface of velocity in solar chromosphere

The data of velocity and magnetic fields in the solar photosphere (5324 angstrom) and the chromosphere (4861 angstrom) clearly show the features of tangential discontinuity of velocity in the chromosphere. The velocity fields in and near the solar active region named No. 88029 by the Huairou Station have been analyzed in detail. A lot of magnetohydrodynamic discontinuous surfaces, especially the tangential discontinuities, are shown from the observations. The calculations of the thickness of discontinuous layer and the evolution time of instability agree with the observational results. The variations of the flow field will directly influence the evolutions and changes of the active region as the magnetic field are coupled closely with the plasma motion.

The progress of solar-terrestrial sciences in china

 SOLAR-TERRESTRIAL SCIENCESThe solar-terrestrial sciences study how the solar energy, momentum and mass transfer through the interplanetary space, the earth magnetosphere, the ionosphere and the neutral atmosphere, and their influence on earth environment. The solar-terrestrial sciences are also called, sometimes, the solar-terrestrial physics, solar-terrestrial relations, solar-terrestrial 更多还原

Energy conversions and storage caused by an unsteady poloidal flow in active solar regions

In this paper we discuss coupling processes between a magnetic field and an unsteady plasma motion, and analyze the features of energy storage and conversions in active region. It is pointed out that the static force-free field is insufficient for a discussion of storage processes, and also the pure unsteady plasma rotation is not a perfect approach. In order to analyze the energy storage, we must consider the addition of poloidal plasma motion. The paper shows that because the unsteady poloidal flow is added and coupling occurs between the magnetic field and both the toroidal and the poloidal plasma flows, an unsteady process is maintained which changes the force-free factor with time. Hence, the energy in the lower levels can be transferred to the upper levels, and a considerable energy can be stored in the active region. Finally, another storage process is given which is due to the pure poloidal flow. The article shows that even if there is no twisted magnetic line of force, the energy in the lower levels may still be transferred to the upper levels and stored there.

The mechanism of energy storage by shearing the solar magnetic field

In this paper, a complete set of MHD equations have been solved by numerical calculations in an attempt to study the dynamical evolutionary processes of the initial equilibrium configuration and to discuss the energy storage mechanism of the solar atmosphere by shearing the magnetic field. The initial equilibrium configuration with an arch bipolar potential field obtained from the numerical solution is similar to the configuration in the vicinity of typical solar flare before its eruption. From the magnetic induction equation in the set of MHD equations and dealing with the non-linear coupling effects between the flow field and magnetic field, the quantitative relationship has been derived for their dynamical evolution. Results show that plasma shear motion at the bottom of the solar atmosphere causes the magnetic field to shear; meanwhile the magnetic field energy is stored in local regions. With the increase of time the local magnetic energy increases and it may reach an order of 4×10^25 J during a day. Thus the local storage of magnetic energy is large enough to trigger a big solar flare and can be considered as the energy source of solar flares. The energy storage mechanism by shearing the magnetic field can well explain the slow changes in solar active regions.