Endoscopic sleeve gastroplasty (the Apollo method): a new approach to obesity management

Background: Many obese patients cannot lose weight or reject conventional obesity management. Endoscopic sleeve gastroplasty (the Apollo method) is a pioneering coadjuvant, interventionist technique for the integral management of obesity. Objectives: The goals of this study were to report safety and efficacy results obtained at 6 months in patients undergoing endoscopic sleeve gastroplasty. Material and methods: A prospective study was performed in 55 patients (13 males, 42 females) who were subjected to the Apollo technique; mean age was 43.5 years (range 25-60) and mean BMI was 37.7 kg/m² (range 30-48). All received multidisciplinary follow-up for weight loss. Weight changes and presence of complications were assessed. Through the endoscope a triangular pattern suture is performed consisting of approximately 3-6 transmural (mucosa to serosa) stitches, using a cinch device to bring them nearer and form a plication. Results: A total of 6-8 plications are used to provide a tubular or sleeve-shaped restriction to the gastric cavity. No major complications developed and patients were discharged at 24 hours following the procedure. Endoscopic and radiographic follow-up at 6 months post-procedure showed a well preserved tubular form to the stomach. After 6 months patients had lost 18.9 kg and 55.3% of excess weight. Conclusions: Endoscopic sleeve gastroplasty, together with dietary and psycho-behavioral changes, is a safe, effective technique in the coadjuvant management of obese patients.

Super-orbital re-entry in Australia : laboratory measurement, simulation and flight observation

There are large uncertainties in the aerothermodynamic modelling of super-orbital re-entry which impact the design of spacecraft thermal protection systems (TPS). Aspects of the thermal environment of super-orbital re-entry flows can be simulated in the laboratory using arc- and plasma jet facilities and these devices are regularly used for TPS certification work [5]. Another laboratory device which is capable of simulating certain critical features of both the aero and thermal environment of super-orbital re-entry is the expansion tube, and three such facilities have been operating at the University of Queensland in recent years[10]. Despite some success, wind tunnel tests do not achieve full simulation, however, a virtually complete physical simulation of particular re-entry conditions can be obtained from dedicated flight testing, and the Apollo era FIRE II flight experiment [2] is the premier example which still forms an important benchmark for modern simulations. Dedicated super-orbital flight testing is generally considered too expensive today, and there is a reluctance to incorporate substantial instrumentation for aerothermal diagnostics into existing missions since it may compromise primary mission objectives. An alternative approach to on-board flight measurements, with demonstrated success particularly in the ‘Stardust’ sample return mission, is remote observation of spectral emissions from the capsule and shock layer [8]. JAXA’s ‘Hayabusa’ sample return capsule provides a recent super-orbital reentry example through which we illustrate contributions in three areas: (1) physical simulation of super-orbital re-entry conditions in the laboratory; (2) computational simulation of such flows; and (3) remote acquisition of optical emissions from a super-orbital re entry event.

Electron microscopy of micron-sized lunar soil

We have performed electron-microscopic analysis on 0.5-1.0µm grains in order to study radiation damage by the solar-wind. We are reporting some interesting results we have found in monomineralic grains from core sample 15010,1130. This is a submature soil which has been studied for rare gas abundance and ferromagnetic resonance by (1) and modal petrology by (2).

Studio portait of Ralph Grahme.

Verso: 93-8-1 Ralph Grahme Donated by Joan Grahme to T. Krakauer; Apollo Photography no longer exists (note by 10/6/1986)

Studio portait of Ralph Grahme.

Verso: 93-8-1 Ralph Grahme Donated by Joan Grahme to T. Krakauer; Apollo Photography no longer exists (note by 10/6/1986)

Physical properties of meteorites and their role in planetology

Together with cosmic spherules, interplanetary dust particles and lunar samples returned by Apollo and Luna missions, meteorites are the only source of extraterrestrial material on Earth. The physical properties of meteorites, especially their magnetic susceptibility, bulk and grain density, porosity and paleomagnetic information, have wide applications in planetary research and can reveal information about origin and internal structure of asteroids. Thus, an expanded database of meteorite physical properties was compiled with new measurements done in meteorite collections across Europe using a mobile laboratory facility. However, the scale problem may bring discrepancies in the comparison of asteroid and meteorite properties. Due to inhomogenity, the physical properties of meteorites studied on a centimeter or millimeter scale may differ from those of asteroids determined on kilometer scales. Further difference may arise from shock effects, space and terrestrial weathering and from difference in material properties at various temperatures. Close attention was given to the reliability of the paleomagnetic and paleointensity information in meteorites and the methodology to test for magnetic overprints was prepared and verified.

Multiwavelength studies of regolith effects in planetary remote sensing

A large proportion of our knowledge about the surfaces of atmosphereless solar-system bodies is obtained through remote-sensing measurements. The measurements can be carried out either as ground-based telescopic observations or space-based observations from orbiting spacecraft. In both cases, the measurement geometry normally varies during the observations due to the orbital motion of the target body, the spacecraft, etc.. As a result, the data are acquired over a variety of viewing and illumination angles. Surfaces of planetary bodies are usually covered with a layer of loose, broken-up rock material called the regolith whose physical properties affect the directional dependence of remote-sensed measurements. It is of utmost importance for correct interpretation of the remote-sensed data to understand the processes behind this alteration. In the thesis, the multi-angular effects that the physical properties of the regolith have on remote-sensing measurements are studied in two regimes of electromagnetic radiation, visible to near infrared and soft X-rays. These effects are here termed generally the regolith effects in remote sensing. Although the physical mechanisms that are important in these regions are largely different, notable similarities arise in the methodology that is used in the study of the regolith effects, including the characterization of the regolith both in experimental studies and in numerical simulations. Several novel experimental setups have been constructed for the thesis. Alongside the experimental work, theoretical modelling has been carried out, and results from both approaches are presented. Modelling of the directional behaviour of light scattered from a regolith is utilized to obtain shape and spin-state information of several asteroids from telescopic observations and to assess the surface roughness and single-scattering properties of lunar maria from spacecraft observations. One of the main conclusions is that the azimuthal direction is an important factor in detailed studies of planetary surfaces. In addition, even a single parameter, such as porosity, can alter the light scattering properties of a regolith significantly. Surface roughness of the regolith is found to alter the elemental fluorescence line ratios of a surface obtained through planetary soft X-ray spectrometry. The results presented in the thesis are among the first to report this phenomenon. Regolith effects need to be taken into account in the analysis of remote-sensed data, providing opportunities for retrieving physical parameters of the surface through inverse methods.

Numerical Analysis of the Effects of Free-Stream Thermo-Chemical State on the Test Model Flow Field in High-Enthalpy Tunnel

The effects of the free-stream thermo-chemical state on the test model flow field in the high-enthalpy tunnel are studied numerically. The properties of the free-stream, which is in thermo-chemical non-equilibrium, are determined by calculating the nozzle flow field. A free-stream with total enthalpy equal to the real one in the tunnel while in thermo-chemical equilibrium is constructed artificially to simulate the natural atmosphere condition. The flow fields over the test models (blunt cone and Apollo command capsule model) under both the non-equilibrium and the virtual equilibrium free-stream conditions are calculated. By comparing the properties including pressure, temperature, species concentration and radiation distributions of these two types of flow fields, the effects of the non-equilibrium state of the free-stream in the high-enthalpy shock tunnel are analyzed.

The distribution and ages of regional lithologies in the lunar maria

A research program was designed (1) to map regional lithological units of the lunar surface based on measurements of spatial variations in spectral reflectance, and, (2) to establish the sequence of the formation of such lithological units from measurements of the accumulated affects of impacting bodies.

Spectral reflectance data were obtained by scanning luminance variations over the lunar surface at three wavelengths (0.4µ, 0.52µ, and 0.7µ). These luminance measurements were reduced to normalized spectral reflectance values relative to a standard area in More Serenitotis. The spectral type of each lunar area was identified from the shape of its reflectance spectrum. From these data lithological units or regions of constant color were identified. The maria fall into two major spectral classes: circular moria like More Serenitotis contain S-type or red material and thin, irregular, expansive maria like Mare Tranquillitatis contain T-type or blue material. Four distinct subtypes of S-type reflectances and two of T-type reflectances exist. As these six subtypes occur in a number of lunar regions, it is concluded that they represent specific types of material rather than some homologous set of a few end members.

The relative ages or sequence of formation of these more units were established from measurements of the accumulated impacts which have occurred since more formation. A model was developed which relates the integrated flux of particles which hove impacted a surface to the distribution of craters as functions of size and shape. Erosion of craters is caused chiefly by small bodies which produce negligible individual changes in crater shape. Hence the shape of a crater can be used to estimate the total number of small impacts that have occurred since the crater was formed. Relative ages of a surface can then be obtained from measurements of the slopes of the walls of the oldest craters formed on the surface. The results show that different maria and regions within them were emplaced at different times. An approximate absolute time scale was derived from Apollo 11 crystallization ages under an assumption of a constant rote of impacting for the last 4 x 10^9 yrs. Assuming, constant flux, the period of mare formation lasted from over 4 x 10^9 yrs to about 1.5 x 10^9 yrs ago.

A synthesis of the results of relative age measurements and of spectral reflectance mapping shows that (1) the formation of the lunar maria occurred in three stages; material of only one spectral type was deposited in each stage, (2) two distinct kinds of maria exist, each type distinguished by morphology, structure, gravity anomalies, time of formation, and spectral reflectance type, and (3) individual maria have complicated histories; they contain a variety of lithic units emplaced at different times.

Depth-sensitive analysis of fluorine on lunar sample surfaces and in carbonaceous chondrites by a nuclear resonant reaction technique

The nuclear resonant reaction ¹⁹F(ρ,αγ)¹⁶O has been used to perform depth-sensitive analyses of fluorine in lunar samples and carbonaceous chondrites. The resonance at 0.83 MeV (center-of-mass) in this reaction is utilized to study fluorine surface films, with particular interest paid to the outer micron of Apollo 15 green glass, Apollo 17 orange glass, and lunar vesicular basalts. These results are distinguished from terrestrial contamination, and are discussed in terms of a volcanic origin for the samples of interest. Measurements of fluorine in carbonaceous chondrites are used to better define the solar system fluorine abundance. A technique for measurement of carbon on solid surfaces with applications to direct quantitative analysis of implanted solar wind carbon in lunar samples is described.

Discurso e representação sobre as práticas rituais dos esparciatas e dos seus basileus na Lacedemônia, do século V a.C.

A história da pólis de Esparta como, por vezes, nos foi apresentada tomou uma perspectiva historiográfica dotada de pressupostos Atenocêntricos, os quais acabaram apresentando-a como rústica, dotada de uma economia e uma cultura estática e demasiadamente inclinada às atividades militares. No entanto, através de nossa pesquisa verificamos que as práticas político-culturais dos cidadãos de Esparta eram dinâmicas, para sua época. Seguindo por esse viés, verificamos que as representações de Esparta, sobretudo dos esparciatas e dos seus basileus, variaram de acordo com o grupo social e o contexto histórico em que foram empregadas. Com isso, observamos que embora os cidadãos de Esparta tenham sido, em algumas circunstâncias, criticados pelos pensadores antigos, esta não foi uma tendência hegemônica. Sendo assim, mediante os indícios da documentação literária do período Clássico, notamos que os esparciatas e os seus basileus teriam sido homens dotados de um habitus tradicional, o qual valorizava o aprimoramento físico e mental, assim como a responsabilidade com os deveres sagrados. Através da interação entre os vestígios documentais e dos estudos historiográficos mapeamos parte das representações de Esparta que figuraram os diversos discursos no decorrer da história do Ocidente, no intuito de materializarmos as possíveis motivações político-culturais nas apropriações do habitus espartano. Por conseguinte, recorremos à documentação literária para entendermos como parte dos pensadores clássicos concebeu, por meio de uma memória ancestral, a formação da região da Lacedemônia e da pólis de Esparta, a qual teria se dado concomitantemente com a legitimação político-cultural da identidade étnica dos basileus e dos esparciatas. Por fim, analisamos as práticas rituais em honra ao deus Apolo como um mecanismo empregado pelos segmentos sociais hegemônicos da Lacedemônia para ratificar o seu poder político frente a grupos sociais submetidos.

中国5种珍稀绢蝶非损伤性取样的mtDNA序列及系统进化

应用非损伤性取样DNA测序技术测定了4种来自云南白马雪山和1种来自新疆天山的5种珍稀绢蝶的线粒体DNA细胞色素b基因部分DNA序列。PAUP3.1.1(简约法)数据分析软件构建该5个种绢蝶的分子系统树显示,爱珂绢蝶(Parnassius acco)和巴裔绢蝶(Parnassius baileyi)的亲缘关系比较接近,阿波罗绢蝶(Parnassius apollo)、珍珠绢蝶(Parnassius orlears)和西猴绢蝶(Parnassius simo)3种绢蝶均为相对独立的一支,其中西猴绢蝶分化较早,与形态学研究结果相吻合。

Large Gene Family Expansions and Adaptive Evolution for Odorant and Gustatory Receptors in the Pea Aphid, Acyrthosiphon pisum

Gaining insight into the mechanisms of chemoreception in aphids is of primary importance for both integrative studies on the evolution of host plant specialization and applied research in pest control management because aphids rely on their sense of smell

CAS-1模拟月壤

模拟月壤是与月球月壤具有相似的矿物组成、化学成分和物理力学性质的地球物质,是月球样品的地球化学复制品.长白山龙岗火山群金龙顶子火山喷发的四海火山渣具有与阿波罗14号采集的月球样品相似的化学和矿物组成,并含有20%～40 %的玻璃物质.以四海火山渣为初始物质,研制成功CAS-1模拟月壤,并测量了CAS-1模拟月壤的主量和微量元素组成、矿物组成、密度、颗粒形态、粒度分布、抗剪性和复介电常数等参数.结果表明,CAS-1模拟月壤与Apollo 14号采集的月球样品具有相似的化学成分、矿物组成和物理力学性质,是一种理想的低钛玄武岩质模拟月壤.

伽马射线谱仪探测月球表面元素的分布——以“嫦娥一号”伽马射线谱仪为例

Apollo���Lunar Prospector(LP) 携带的伽马射线谱仪探测了月球表面的氧（O）、硅（Si）、铝（Al）、铁（Fe）、钛（Ti）、钙（Ca）、钾（K）、镁（Mg）、钍（Th）和铀（U）等10种元素的全球分布，对于了解月球的形成与演化有重要的意义。在我国首颗月球探测卫星“嫦娥一号”上搭载了伽马射线谱仪将进一步探测月球表面14种元素的分布特征。本论文的选题紧密结合“嫦娥一号”伽马射线谱仪数据处理和科学反演工作的工程需求，系统研究了伽马射线谱仪探测数据的处理流程和反演方法，并利用LP的数据开展了月球元素、岩石类型及其分布特征的反演工作，为嫦娥一号卫星伽马射线谱仪的数据处理和反演奠定了技术基础。论文主要包括如下几个方面的内容： （1）概述了伽马射线谱仪探测月球表面元素的发展历程，特别是阐述了伽马射线产生的机理和伽马射线谱仪元素探测的原理； （2）讨论了伽马射线谱仪数据反演及其模型，以及在“嫦娥一号”伽马射线谱仪数据反演中的应用； （3）阐述了“嫦娥一号”伽马射线谱仪性能指标，数据处理流程，地面验证实验（模拟月壤的研制及其试验）和初步的探测成果； （4）以LP伽马射线谱仪探测数据为例，讨论了伽马射线谱仪探测数据科学反演工作，阐述了全球Th的分布特征以及月球化学不均一性的相关性；用LP探测数据首次划分出月球岩石类型的分布，探讨了月球演化对岩石类型分布特征的影响。