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The objective of the unified lunar control network is to combine a series of control networks into one compatible network with its origin at the center of mass of the Moon and its coordinates referred to the mean Earth/polar axis system. The initial unified system contained 130 nearside points from Apollo data and 1026 from telescopic data. It also contained ten Mariner 10 points. The total number of points was 1166. The current network includes modifications to the past network and extends the coverage. Coordinates of points north of the Apollo region have been recomputed based on Galileo images from the second Earth-Moon flyby. Coordinates of points in the Apollo region were held fixed; however, coordinates of points north of the Apollo region in the telescopic region and many Mariner 10 points were recomputed. All of the Mariner 10 points were remeasured and integrated into the network. Additional points in the Apollo region including the farside have been added. The unified network now contains 1478 points. Apollo, Mariner 10, and Galileo pictures all contained some farside points. The coordinates of the 1478 points are available only in the microfiche supplement to this paper.

A distribution for the mass of the meteoroids is developed from flux equations assuming a homogeneous filtered Poisson process. Other random variable information required for analyses are derived from data or taken from literature. First-order, second-moment reliability analyses are performed for complete penetration of a meteoroid through exposed and covered lunar structures. Several failure functions are used to model this high speed impact event. Cumulative damage by meteoroid impacts to a radiation cover and an exposed structure are also examined. The results show cumulative damage may be a problem for structures with long design lives.

Preliminary descriptions and analyses of a precision lunar landing using various navigation scenarios are presented. The scenerios assume the Common Lunar Lander (CLL) as a reference mission. Current state-of-the-art or off-the-shelf technology is emphasized to keep mission cost to a minimum—an important driver in the possible funding of future space missions. It is concluded that precision navigation sensor suites are required to meet certain stringent mission navigation requirements.

Georges Melies is usually accorded pride of place for his pioneering work in the science fiction/speculative/horror genres.1 But one wonders whether the prosaic events filmed by those protorealists, the Lumiere brothers–and Melies himself–nearly a decade before Le Voyage dans la Lune (1902) were experienced as equally fantastic voyages by a fin-de-siecle viewer. Contrary to cineaste urban legend, L'Arivee d'un Train en Gare de la Ciotat (1895) did not send audiences screaming into Parisian streets. Nevertheless, to an audience at that brief historical moment before the introjection of standard cinematic tropes, the flickering vision of a train pulling into a station on a screen in a darkened cafe exhibition space may well have seemed as uncanny as the Jupiter landing of the space pod in 2001 (1968).

Dear Sir, The following observation was made at Hluh- lune, Zululand, Souh Africa, December 11, 1951, and might be of interest to you. DOI: 10.1111/j.2153-3490.1952.tb01029.x

The elliptical instability takes place in any rotating fluid with elliptical streamlines. Its existence in geo- or astrophysical flows raises many issues. This is the starting point of this theoretical, numerical and experimental work. After introducing basics of the rotating flows, chapter 1 presents the three considered planetary mechanical forcings: tides, precession and libration. Chapter 2 presents first numerical simulations of the elliptical instability in an ellipsoidal geometry. These simulations allow to derive the scaling laws needed to bridge the gap between numerics and planetary applications. Section 2.4 shows that the simultaneous presence of tides and libration can excite an elliptical instability inside synchronized celestial bodies. In section 2.5, a theoretical analysis of the interaction between tides and precession is developed and validated. Finally, in section 2.6, we prove that the elliptical instability can still develop over convective flows. Chapter 3 focuses on the magnetohydrodynamics of the elliptical instability. New results on the magnetic induction by the elliptical instability are obtained and validated numerically. An experimental work, based on a MHD setup, is then described. Our measurements allow to study the dynamics of the instability under an external imposed magnetic field. The experimental setup is then modified to set up a synthetic dynamo. Chapter 4 study the presence of the elliptical instability in known planets, moons, and stars. The particular case of the Moon is first considered and a scenario, based on the elliptical instability, is proposed and evaluated to explain the early lunar dynamo. Telluric bodies are then considered, and an adapted stability analysis shows that the instability can be expected in the Early Earth, Europa and three exoplanets (55CnCe, CoRoT-7b et GJ1214b). Finally, the possible development of the instability in extra-solar Hot-Jupiters systems is considered, showing its relevance for some of them, such as the system of Tau-boo., L'instabilité elliptique peut apparaître dès qu'un écoulement présente des lignes de courant elliptiques. Sa prise en compte en géo- et astrophysique pose de nombreuses questions qui constituent la motivation principale de ce travail théorique, numérique et expérimental. Après une introduction aux écoulements tournants, le chapitre 1 présente les trois forçages mécaniques qui seront considérés dans ce travail: les marées, la précession et la libration. Le chapitre 2 présente les premières simulations de l'instabilité en géométrie ellipsoïdale, qui nous permettent d'obtenir des lois d'échelles la caractérisant. La section 2.4 montre que la présence simultanée de marées et de libration est susceptible d'exciter une instabilité elliptique au sein des astres synchronisés. La section 2.5 développe et valide une théorie analytique sur l'interaction des marées et de la précession. La section 2.6 démontre que l'instabilité elliptique peut se développer à partir d'écoulements convectifs ou stratifiés. Le chapitre 3 s'intéresse à la magnétohydrodynamique (MHD) de l'instabilité. De nouveaux résultats sur l'aspect inductif de l'instabilité sont obtenus et validés numériquement. Une partie expérimentale liée à ce travail est ensuite décrite, basée sur un dispositif MHD. Après une étude de l'instabilité sous champ, le dispositif est modifié afin de mettre en place une dynamo synthétique. Le chapitre 4 étudie la présence de l'instabilité elliptique au sein de planètes, lunes et étoiles connues. Le cas particulier de la Lune est d'abord considéré et un scénario, basé sur l'instabilité elliptique, est proposé puis évalué pour expliquer la dynamo lunaire primitive. Les astres telluriques sont ensuite considérés dans un cadre plus général, et une étude de stabilité adaptée montre que l'instabilité est possible sur la Terre primitive, Europe et trois exoplanètes (55CnCe, CoRoT-7b et GJ1214b). Enfin, la possible existence de l'instabilité au sein de certains systèmes extra-solaires est considérée.

This thesis describes the set up of the dynamical model of the planetary an lunar ephemeris INPOP, and its adjustment to Lunar laser telemetry data. The first part contains general considerations about the modeling of forces and torques exerted upon Solar System bodies. These interactions, leading to the equations of motions, take into account the Newtonian main term, corrections due to the general relativity, perturbations due to some non spherical bodies or their deformation due to intern constraints (tidal effects). The second part deals with adjustments to Lunar Laser Ranging observations, the measurement of the light time travel between a station on the Earth and a reflector on the Moon. Their intrinsic precision reaches a few centimeters for the most recent ones. In the reduction process, it is thus necessary to take into account some very small physical effects, such as the displacement of the terrestrial crust or the relativistic deviation of light. Finally, the third part describes the constructions of three particular solutions. The first one, designed to retrieve the Jet Propulsion Laboratory's solution DE405, allows to validate the dynamical model. The second one corrects some inconsistancies and includes the Earth's orientation, in order to compute long time solutions. The third one, which model is improved, is fitted to LLR observations. The LLR residuals and fitted parameters values are compared to other published solutions.; Cette thèse décrit la mise en place du modèle dynamique de l'éphéméride planétaire et lunaire INPOP (Intégration Numérique Planétaire de l'Observatoire de Paris) et son ajustement aux données de télémétrie laser Lune. Dans une première partie sont exposées des généralités sur la modélisation des forces et moments qui s'exercent entre les corps du Système solaire. Ces interactions, qui conduisent aux équations du mouvement, comprennent les termes principaux newtoniens, des corrections induites par la relativité générale, des perturbations liées à la non sphéricité de certains corps ou au fait qu'il peuvent se déformer sous l'effet de contraintes internes (effets de marées). La deuxième partie traite des ajustements aux données Lunar Laser Ranging (LLR), mesure du temps de trajet de la lumière entre une station terrestre et un réflecteur déposé à la surface de la Lune. Leur précision intrinsèque de quelques centimètres pour les plus récentes nécessite de tenir compte pour leur réduction d'effets physiques faibles, comme les mouvements de la croûte terrestre ou la déviation relativiste des rayons lumineux. Enfin, la troisième partie décrit les constructions de trois solutions particulières. La première, conçue pour retrouver la solution DE405 du Jet Propulsion Laboratory, permet de valider le modèle dynamique. La deuxième, en corrige quelques inconsistances et intègre l'orientation de la Terre, dans le but de produire des solutions à long terme. La troisième version, dont le modèle dynamique est amélioré, est ajustée aux données LLR. Les résidus LLR et valeurs de paramètres ajustés sont comparés à ceux d'autres solutions publiées.

L’observation des planètes est à l’origine de l’astronomie. Elle a connu un véritable essor au XVIIe siècle, avec l’apparition des premiers instruments et des grands observatoires. Puis, avec l’apparition de la spectroscopie, l’exploration des étoiles et des galaxies s’est développée à son tour, notamment dans la première moitié du XXe siècle, et l’intérêt des astronomes pour les planètes est passé momentanément au second plan. The observation of planets goes back to Antiquity. It strongly developed in the 17th century with the emergence of the first refractors and telescopes. Since the 1950s, the study of solar-system objects has known a new revolution, with the development of space planetary exploration. A new image of the solar system has emerged, with the in situ observations of planets and comets, and the discovery of a new class of objects beyond Neptune’s orbit. The French scientific community has played a significant role in this adventure, thanks in particular to its organization within CNRS and CNES.

Textes recueillis et présentés par Mariella Colin.; International audience; Peu d'auteurs consacrés se sont " risqués " à l'écriture de contes pour enfants, parmi eux T. Landolfi (1908-1979), l'un des écrivains contemporains les plus originaux de la littérature italienne. Dans Il principe infelice, Landolfi se livre à un exercice hardi, il introduit un récit de rêve dans le conte. La présence d'une scène de rêve dans le récit n'est pas anodine, le motif du rêve n'apparaît que très rarement dans les contes italiens et invite le lecteur à un travail d'interprétation complémentaire, en racontant une histoire qui se présente comme un rébus à déchiffrer. Le motif du rêve retient d'autant plus l'attention du lecteur qu'il occupe entièrement la scène narrative : la quête de l'héroïne étant conditionnée par ce désir de rêve qui la pousse à entreprendre un voyage initiatique au Pays de rêves . Le choix d'insérer une scène de rêve dans un conte peut sembler redondant, la composante onirique du conte étant quasiment " de rigueur ", mais il ajoute un arcane au récit merveilleux, lequel semble alors s'enlacer sur lui même : un rêve dans le conte, comme un lieu dans un lieu, une énigme dans une énigme. Le texte de Landolfi semble vouloir interroger le rapport entre connaissance et désir : il guide le lecteur dans le clair-obscur d'un itinéraire placé " sous le signe de la lune ", figurant les différents états de la conscience humaine pour explorer le mécanisme de la fabrication des rêves.

The 18.6 yr nodal cycle modulates tidal amplitudes and currents, and consequently sedimentation in tide-influenced sedimentary environments. Data are presented which show that such effects are obvious along the coast of the Dutch barrier islands and in the sedimentary fill of abandoned channels.

In accordance with 140 Chinese ancient records of lunar eclipses with magnitude and time a study and analysis of the accuracy of these records is made in this paper. We conclude: (1). The accounts of magnitude and time of lunar eclipses are quite accurate and the records are reliable. (2). The ancient phenomenon in China was recorded with dawn as the beginning of a day. (3). That whether the penumbral lunar eclipses were recorded in China's ancient times is analyzed. The answer is in the affirmative basically.

Summary This paper examines the purport of epact tables encountered on scientific instruments, and explains their use. The epact is a valuable chronological aid for calculating the age of the moon. In handbooks of chronology, usually two types of epacts are distinguished: the epact used in medieval times, and the so-called Lilian epact used after 1582 in the Gregorian perpetual calendar. By examining the rules for calculating the age of the moon, it turns out that the Julian and Gregorian epacts encountered on instruments must be distinguished from the medieval and Lilian epacts. It is shown that the Julian epact was already in use in 1478, and that, by adjusting for the shift of ten days in the date of the vernal equinox, the Gregorian epact was derived from it in 1582. The common association of the latter with the Lilian epact employed in the Gregorian perpetual calendar is incorrect. It is further shown that in contrast to the medieval and Lilian epacts, which served purely ecclesiastical purposes, the...

Data from the Tibet air-shower array were used to examine the cosmic-ray shadows of the Moon and the Sun at energies around 10 TeV. The shadowing effect was clearly observed at the $5.8\ensuremath{\sigma}$ level for the Moon, while the shadow of the Sun was found in the direction away from the Sun by 0.86\ifmmode^\circ\else\textdegree\fi{} to the west and 0.43\ifmmode^\circ\else\textdegree\fi{} to the south. The effect of the geomagnetic field has also been observed in the shadow of cosmic rays by the Moon. The observed deflection of the Sun's shadow is briefly discussed in connection with the effect of the magnetic fields between the Sun and the Earth. This is the first observation of the effects of such magnetic fields on the cosmic-ray shadow. The maximum-likelihood analysis of the Moon data set shows that the angular resolutions of the array for showers with its mode energies 7 and 35 TeV are 0.87${\mathrm{\ifmmode^\circ\else\textdegree\fi{}}}_{\ensuremath{-}0.10\mathrm{\ifmmode^\circ\else\textdegree\fi{}}}^{+0.13\mathrm{\ifmmode^\circ\else\textdegree\fi{}}}$ and 0.54${\mathrm{\ifmmode^\circ\else\textdegree\fi{}}}_{\ensuremath{-}0.08\mathrm{\ifmmode^\circ\else\textdegree\fi{}}}^{+0.11\mathrm{\ifmmode^\circ\else\textdegree\fi{}}}$, respectively.

One of the most important inferences of the Lunar Prospector mission data was the existence of subsurface water ice in the permanently shadowed craters near both lunar poles [Feldman et al., 1998]. We propose and substantiate an alternative explanation that hydrogen can exist in the shallow lunar subsurface in the form of clathrate hydrates: CH4 . 6H(2)o and/or CO2 . 6H(2)o.

Future space exploration missions aim at landing and returning samples from moon, planets and asteroids. Autonomous precision landing capabilities will have to reach pre-selected landing sites which may lie near hazardous terrain features such as craters, rocks. However, past and current robotic landers are still far from this ability. For example, the rover Mars Science Laboratory, to be launched in 2011, is programmed to land on a position with an error of several kilometers. The first goal of thesis is to propose a vision-based absolute navigation system, named "Landstel", for interplanetary landers, especially for missions on Mars or on Moon. Contrary to current absolute navigation systems proposed in the literature which rely either on the usage of image intensity or on specific surface landmarks like craters, Landstel employs the topological property of generic surface landmarks. As a result, Landstel is not restricted to any particular terrain. Landstel also exhibits a high robustness with respect to illumination variations and sensor noise. In addition, the use of surface landmarks allows Landstel to drastically reduce the required onboard memory. Besides Landstel, the second goal of the thesis is to propose a framework to integrate Landstel inside a complete navigation system called VIBAN, including absolute localization, inertial navigation and/or visual odometry. The absolute position estimate returned by Landstel is firstly verified using the visual odometry tracked points. Then, the verified position estimate is fused with the velocity estimate of the visual odometry in a Kalman filter to improve the estimated position. The updated position is later returned back to Landstel which increases the speed of Landstel by focusing the search for matches and reduces the probability of false estimations. Finally, the points tracked by visual odometry are fed to Landstel to augment the number of matches returned by Landstel. Besides these interests, the integrat ion scheme does not impose any constraints on the spacecraft velocity or angular rate. Extensive experiments with PANGU, a surface simulator, and with Earth images validate the proposed system.; Les missions d'exploration planétaires dans l'avenir demandent une grande précision sur la position de l'atterrissage à la surface de Mars, de la Lune ou d'astéroïdes. Les technologies utilisées dans les sondes interplanétaires récentes ou dans le futur proche sont encore loin de cette capacité: par exemple, le robot Mars Science Laboratory, qui sera lancé en 2011, se posera en un endroit qui n'est connu qu'avec une précision de l'ordre de 10 km. Le premier objectif de cette thèse est de proposer un système de navigation absolue pour les sondes interplanétaires lunaires ou martiennes qui se base sur la vision, nommé "Landstel". Contrairement aux systèmes de navigation absolue qui se basent sur la détection et l'appariement des cratères ou directement sur l'intensité des images perçues, Landstel exploite la topologie des amers détectés dans les images. Par conséquent, il n'est pas restreint à aucune surface particulière. Landstel montre aussi une grande robustesse par rapport aux variations de condition d'illumination et au bruit des capteurs embarqués, et ne requiert que très peu de mémoire. Le deuxième objectif de la thèse est de proposer un cadre pour intégrer Landstel dans un système de navigation complète, appelé VIBAN, qui comprend des capteurs inertiels et/ou un système d'odométrie visuelle. La position absolue estimée par Landstel est d'abord validée avec les appariements de l'odomètre visuel, puis elle est combinée avec l'estimation de l'odomètre visuel avec un filtre de Kalman pour améliorer sa précision. La position mise à jour est ensuite retournée à Landstel pour accélérer le système de navigation en réduisant la zone de recherche des appariements et aussi le taux de fausses estimations. Finalement, les amers suivis par l'odomètre visuel sont fournis à Landstel pour augmenter le nombre des appariements. De très nombreuses expériences avec PANGU, un simulateur de terrain, et avec des images réelles, valident le système proposé.

Les missions d'exploration planétaires dans l'avenir demandent une grande précision sur la position de l'atterrissage à la surface de Mars, de la Lune ou d'astéroïdes. Les technologies utilisées dans les sondes interplanétaires récentes ou dans le futur proche sont encore loin de cette capacité : par exemple, le robot Mars Science Laboratory, qui sera lancé en 2011, se posera en un endroit qui n'est connu qu'avec une précision de l'ordre de 10 km. Le premier objectif de cette thèse est de proposer un système de navigation absolue pour les sondes interplanétaires lunaires ou martiennes qui se base sur la vision, nommé "Landstel". Contrairement aux systèmes de navigation absolue qui se basent sur la détection et l'appariement des cratères ou directement sur l'intensité des images perçues, Landstel exploite la topologie des amers détectés dans les images. Par conséquent, il n'est pas restreint à aucune surface particulière. Landstel montre aussi une grande robustesse par rapport aux variations de condition d'illumination et au bruit des capteurs embarqués, et ne requiert que très peu de mémoire. Le deuxième objectif de la thèse est de proposer un cadre pour intégrer Landstel dans un système de navigation complète, appelé VIBAN, qui comprend des capteurs inertiels et/ou un système d'odométrie visuelle. La position absolue estimée par Landstel est d'abord validée avec les appariements de l'odomètre visuel, puis elle est combinée avec l'estimation de l'odomètre visuel avec un filtre de Kalman pour améliorer sa précision. La position mise à jour est ensuite retournée à Landstel pour accélérer le système de navigation en réduisant la zone de recherche des appariements et aussi le taux de fausses estimations. Finalement, les amers suivis par l'odomètre visuel sont fournis à Landstel pour augmenter le nombre des appariements. De très nombreuses expériences avec PANGU, un simulateur de terrain, et avec des images réelles, valident le système proposé. Future space exploration missions aim at landing and returning samples from moon, planets and asteroids. Autonomous precision landing capabilities will have to reach pre-selected landing sites which may lie near hazardous terrain features such as craters, rocks. However, past and current robotic landers are still far from this ability. For example, the rover Mars Science Laboratory, to be launched in 2011, is programmed to land on a position with an error of several kilometers. The first goal of thesis is to propose a vision-based absolute navigation system, named “Landstel”, for interplanetary landers, especially for missions on Mars or on Moon. Contrary to current absolute navigation systems proposed in the literature which rely either on the usage of image intensity or on specific surface landmarks like craters, Landstel employs the topological property of generic surface landmarks. As a result, Landstel is not restricted to any particular terrain. Landstel also exhibits a high robustness with respect to illumination variations and sensor noise. In addition, the use of surface landmarks allows Landstel to drastically reduce the required onboard memory. Besides Landstel, the second goal of the thesis is to propose a framework to integrate Landstel inside a complete navigation system called VIBAN, including absolute localization, inertial navigation and/or visual odometry. The absolute position estimate returned by Landstel is firstly verified using the visual odometry tracked points. Then, the verified position estimate is fused with the velocity estimate of the visual odometry in a Kalman filter to improve the estimated position. The updated position is later returned back to Landstel which increases the speed of Landstel by focusing the search for matches and reduces the probability of false estimations. Finally, the points tracked by visual odometry are fed to Landstel to augment the number of matches returned by Landstel. Besides these interests, the integration scheme does not impose any constraints on the spacecraft velocity or angular rate. Extensive experiments with PANGU, a surface simulator, and with Earth images validate the proposed system.

Lunar patterns of settlement of 15 Caribbean reef fishes were assessed from daily collections of newly arrived fishes from each of two small (A=63 and B=28 m2) patch reefs at Punta de San Blas (Panama) during two consecutive 2 yr periods (1984, 1985 and 1986, 1987). In 12 species settlement was lunar-cyclic, with a broad peak of activity around the new moon in 11 cases, and at first quarter in 1 species. However, 3 of these “lunar-cyclic” species displayed intermittent semilunar periodicity in settlement, with peaks around the quarter moons. One other species had a semilunar cycle of settlement with peaks at both quarter moons. Two species apparently lacked lunar settlement cycles. In some, but not all, paris of congeners: (a) monthly variation in settlement intensity was positively correlated, (b) the duration of settlement pulses in the same month consistently differed, and (c) the timing of settlement pulses in the same month often differed (although one species did not consistently arrive before the other). Recruitment of juvenile fish that survived to the end of the lunar cycle in which they settled was monitored monthly, concurrently with settlement, at a number of large sites scattered up to 2 km apart. The levels of variation in the amount of settlement and recruitment each month differed in only 2 of 17 cases, with settlement variation exceeding recruitment variation in only one of these. The intensity of recruitment was positively correlated with the intensity of settlement in 16 of 17 cases. In 15 of those 16 cases, R 2 values for linear regressions of recruitment on settlement exceeded R 2 values for curvilinear regressions that would indicate either increasing or decreasing recruitment success with increasing intensity of settlement. Thus it appears that variation in recruitment can be used to estimate variation in settlement, and that recruitment success may be density-independent.

In this paper the problem of the classification of natural samples is discussed. An updated version of the G-mode multivariate statistical method for the classification of natural samples, applicable to a wide range of research fields, is discussed in this paper. This method allows an automatic classification in terms of homogeneous taxonomic units, without any a priori knowledge of the taxonomic structure of the natural observations; it provides informations on the different levels of classification present in the data set under study (classes and subclasses), on the level of information residing in each variable, on the level of similarity and/or difference among homogeneous classes.

It is pointed out that the implication of the popular giant impact model of lunar origin (e.g., Hartmann and Davis, 1975; Cameron and Ward, 1976; Stevenson, 1987) is that any depth-related silicate differentiation within the impactor (and/or the earth) at the time of the impact must be partly inherited by the preferentially peripheral matter that forms the moon. This paper presents calculations of the magnitude of the net differentiation of the protolunar matter for a variety of elements and scenarios, with different assumptions regarding the geometries of the 'sampled' peripheral zones, the relative proportions of the earth-derived to impactor-derived matter in the final moon, and the degree to which the impactor mantle had crystallized prior to the giant impact. It is shown that these differention effects constrain the overall plausibility of the giant impact hypothesis.

Durant le premier millénaire, entre le VIIe/VIe et le IIe siècle avant Jésus-Christ, les Carthaginois ont élevé des stèles votives dans un sanctuaire à ciel ouvert. Dédiées à la dyade Baal Hamon et Tinnit Pane Baal, ces sculptures montrent sur leur surface décorée une iconographie qui se compose, en grande partie, de signes et symboles géométriques: un losange, une image céleste composée d’un disque et d’un croissant, une « idole-bouteille », le signe dit « de Tinnit » et un étendard nommé « caducée » dans la littérature. À ce jour, les informations liées à l’interprétation de ces images sont restées largement disparates et fragmentaires et aucune synthèse approfondie n’a encore été publiée à leur sujet. Afin d’aboutir à des résultats tangibles, il s’avère indispensable de mettre à plat l’ensemble des connaissances acquises sur le sujet. À cette fin, une nouvelle approche méthodologique basée sur une typologie raisonnée, c’est-à-dire diachronique et limitée à la seule métropole carthaginoise, sera mise en place. En outre, cette démarche doit être définie en adéquation avec le contexte régional tyrien, berceau de l’idéologie religieuse carthaginoise. Au-delà du rapport de ces images avec les divinités invoquées, la typologie à promouvoir doit, en même temps, nous permettre de clarifier le contexte chronologique propre à chacun de ces éléments figurés. / During the first millennium, between the VIIth/VIth and IInd century bc, the Carthaginians have erected votive stelae in an open air precinct. Dedicated to the dyad Baal Hamon and Tinnit Pane Baal, those sculptures show on their decorated surface an iconography mostly composed of geometric signs and symbols: a lozenge, a celestial pattern made up of a disk and a crescent, a “bottle idol”, the “Tinnit sign” and a standard named “caduceus” in the literature. To date, the information tied up with the interpretation of those images are largely disparate and fragmentary and no thorough synthesis has been published on their subject. In order to reach tangible results, it is necessary to gather all known data’s on the subject. To that end, a new methodological approach, based on a diachronic typology limited to the sole Carthaginian metropolis, will be put in place. Moreover, this approach must be defined in adequacy with the Tyrian regional context, cradle of the Carthaginian religious ideology. Beyond the links of those images with of the invoked divinities, the typology to promote must allow us, in the same time, to clarify the chronological context peculiar to each of the studied items., Doctorat en Histoire, art et archéologie, info:eu-repo/semantics/published

To understand the possible large scale influence of Titan on its plasma environment, we study the magnetic fields and plasma measurements, both when Cassini flies close to Titan and when Cassini crosses the moon's orbit far from it. Using 98 Cassini passes from 06/2004 to 12/2008, we examine the plasma environments at the orbit of Titan with the moon present and absent. In particular, the presence of Titan appears to affect the magnetopause location. Near noon, the Saturn magnetopause is more frequently inside of Titan's orbit with the moon absent than with it present. Titan's presence near noon appears to locally enhance the total pressure and reduce the magnetosphere compressibility, possibly by mass-loading. Near local midnight, the stretching and sweepback angles for cases with Titan present and absent suggest that the moon enhances the tail reconnection rate, in agreement with previous studies of the moon's influence on the Saturnian magnetosphere.

Accepted: 2009-09-02, 資料番号: SA1000796000

[1] We have calculated evaporation rates for a range of organic compounds that may be cold-trapped at the poles of the Moon and Mercury. Organics vary widely in their volatilities and thus can be stable to evaporation at higher and lower temperatures than water. The detection of cold-trapped organics would point to volatile delivery by impacts, as comets and asteroids are the only plausible sources for organic molecules. The characterization of cold-trapped organics on both bodies may provide constraints on the thermal evolution of cold traps over time and the history of volatiles in the inner solar system.

Measuring the neutron and gamma ray fluxes produced by the interaction of galactic cosmic rays with planetary surfaces allow constraining the chemical composition of the upper tens of centimeters of material. Two different angles are proposed to study neutron and gamma spectroscopy: data processing and data interpretation. The present work is in line with two experiments, the Mars Odyssey Neutron Spectrometer and the Selene Gamma Ray Spectrometer. A review of the processing operations applied to the MONS dataset is proposed. The resulting dataset is used to determine the depth of the hydrogen deposits below the Martian surface. In water depleted regions, neutron data allow constraining the concentration in elements likely to interact with neutrons. The confrontation of these results to those issued from the Gamma Ray Spectrometer onboard Mars Odyssey provides interesting insight on the geologic context of the Central Elysium Planitia region. These martian questions are followed by the study of the Selene gamma ray data. Although only preliminary processing has been done to date, qualitative lunar maps of major elements (Fe, Ca, Si, Ti, Mg, K, Th, U) have already been realized.; La mesure des flux de neutrons et de rayonnements gamma issus de l'interaction du rayonnement cosmique galactique avec les surfaces planétaires permet de contraindre la composition chimique des premières dizaines de centimètres de régolite. Deux angles d'approche de la spectroscopie neutron et gamma ont été abordés : le traitement des données et l'interprétation des résultats. Les études menées s'inscrivent dans le cadre de deux missions : le spectromètre neutron à bord de Mars Odyssey et le spectromètre gamma à bord de Selene. Une revue détaillée des opérations de réduction des données MONS est proposée. Le jeu de données résultant est utilisé pour déterminer la profondeur des dépôts d'hydrogène sous la surface martienne. Dans les régions dépourvues d'eau, les données neutron permettent de contraindre la concentration des éléments susceptibles d'interagir avec les neutrons. La confrontation de ces résultats avec ceux du spectromètre gamma à bord de Mars Odyssey permet d'éclairer le contexte géologique de la région de Central Elysium Planitia. Toutes ces problématiques martiennes sont suivies de l'étude des données gamma de Selene. Bien que seuls les traitements préliminaires aient été réalisés à ce jour, des cartes qualitatives des éléments majeurs (Fe, Ca, Si, Ti, Mg, K, Th, U) ont pu être extraites des données.

Measuring the neutron and gamma ray fluxes produced by the interaction of galactic cosmic rays with planetary surfaces allow constraining the chemical composition of the upper tens of centimeters of material. Two different angles are proposed to study neutron and gamma spectroscopy: data processing and data interpretation. The present work is in line with two experiments, the Mars Odyssey Neutron Spectrometer and the Selene Gamma Ray Spectrometer. A review of the processing operations applied to the MONS dataset is proposed. The resulting dataset is used to determine the depth of the hydrogen deposits below the Martian surface. In water depleted regions, neutron data allow constraining the concentration in elements likely to interact with neutrons. The confrontation of these results to those issued from the Gamma Ray Spectrometer onboard Mars Odyssey provides interesting insight on the geologic context of the Central Elysium Planitia region. These martian questions are followed by the study of the Selene gamma ray data. Although only preliminary processing has been done to date, qualitative lunar maps of major elements (Fe, Ca, Si, Ti, Mg, K, Th, U) have already been realized.; La mesure des flux de neutrons et de rayonnements gamma issus de l'interaction du rayonnement cosmique galactique avec les surfaces planétaires permet de contraindre la composition chimique des premières dizaines de centimètres de régolite. Deux angles d'approche de la spectroscopie neutron et gamma ont été abordés : le traitement des données et l'interprétation des résultats. Les études menées s'inscrivent dans le cadre de deux missions : le spectromètre neutron à bord de Mars Odyssey et le spectromètre gamma à bord de Selene. Une revue détaillée des opérations de réduction des données MONS est proposée. Le jeu de données résultant est utilisé pour déterminer la profondeur des dépôts d'hydrogène sous la surface martienne. Dans les régions dépourvues d'eau, les données neutron permettent de contraindre la concentration des éléments susceptibles d'interagir avec les neutrons. La confrontation de ces résultats avec ceux du spectromètre gamma à bord de Mars Odyssey permet d'éclairer le contexte géologique de la région de Central Elysium Planitia. Toutes ces problématiques martiennes sont suivies de l'étude des données gamma de Selene. Bien que seuls les traitements préliminaires aient été réalisés à ce jour, des cartes qualitatives des éléments majeurs (Fe, Ca, Si, Ti, Mg, K, Th, U) ont pu être extraites des données.

[1] Dust is the Number 1 environmental hazard on the Moon, yet its movements and adhesive properties are little understood. Matchbox-sized, 270-gram Dust Detector Experiments (DDEs) measured contrasting effects triggered by rocket exhausts of Lunar Modules (LM) after deployment 17 m and 130 m from Apollo 11 and 12 LMs. Apollo 11 Lunar Seismometer was contaminated, overheated and terminated after 21 days operation. Apollo 12 hardware was splashed with collateral lunar dust during deployment. DDE horizontal solar cell was cleansed of nominally 0.3 mg cm−2 dust by 80% promptly at LM ascent and totally within 7 minutes. A vertical cell facing East was half-cleaned promptly then totally over hundreds of hours. Each cell cooled slightly. For the first time lunar electrostatic adhesive forces on smooth silicon were directly measured by comparison with lunar gravity. Analyses imply this adhesive force weakens as solar angle of incidence decreases. If valid, future lunar astronauts may have greater problems with dust adhesion in the middle half of the day than faced by Apollo missions in early morning. A sunproof shed may provide dust-free working environments on the Moon. Low-cost laboratory tests with DDEs and simulated lunar dust can use DDE benchmark lunar data quickly, optimising theoretical modelling and planning of future lunar expeditions, human and robotic.

Mémoire numérisé par la Division de la gestion de documents et des archives de l'Université de Montréal., [À l'origine dans / Was originally part of : Thèses et mémoires - FAS - Département de littérature comparée]

O objetivo deste artigo é mostrar o quanto as relações da televisão com a realidade são mais sutis do que nós costumamos acreditar. Assim, através da análise de Opération Lune, um filme de William Karel que investiga a autenticidade das imagens dos primeiros passos do homem na Lua, questionamos o estatuto desse programa apresentado como um “falso” pela crítica, desembaraçando as múltiplas construções semióticas: imagens de arquivo, testemunhos verdadeiro-falsos, mudança de tonalidade, procedimentos paródicos. Qual é, então, seu estatuto? Mentira? Paródia? Fraude? Opération Lune mostra o quanto, em mediação referencial, a crítica das imagens parece conduzir ao questionamento dos acontecimentos reais que elas narram. Certos telespectadores não hesitam em passar da dúvida sobre a veracidade das imagens à suspeita sobre a realidade dos fatos, com a ajuda cúmplice dos dispositivos presentes no filme.

Control laws obtained by combining a least squares parameter estimator and a minimum variance strategy based on the estimated parameters have asymptotically optimal performance.

A look at what it might be like on a lunar farm in the year 2020 is provided from the point of view of the farmer. Of necessity, the farm would be a Controlled Ecological (or Environment) Life-Support System (CELSS) or a bioregenerative life-support system. Topics covered in the imaginary trip through the farm are the light, water, gasses, crops, the medium used for plantings, and the required engineering. The CELSS is designed with four functioning parts: (1) A plant-production facility with higher plants and algae; (2) food technology kitchens; (3) waste processing and recycling facilities; and (4) control systems. In many cases there is not yet enough information to be sure about matters discussed, but the exercise in imagination pinpoints a number of areas that still need considerable research to resolve the problems perceived.

SUMMARY. 1. The chief objective was to construct a thermal tolerance polygon for juvenile Atlantic salmon, Salmo salar L., using fish from four groups and two populations: two age groups from one population (0+, 1+ parr from River Leven), two size groups from the other population (slow and Fast growing 1+ parr from River Lune). 2. Fish were acclimated to constant temperatures of 5, 10, 15, 20, 25 and 27°C; then the temperature was raised or lowered at 1°C h−1 to determine the upper and lower limits for feeding and survival over 10 min, 100 min, 1000 min and 7 days. As they were not significantly different between the four groups of fish, values at each acclimation temperature were pooled to provide arithmetic means (with SE) for the thermal tolerance polygon. 3. Incipient lethal levels (survival over 7 days) defined a tolerance zone within which salmon lived for a considerable time; upper mean incipient values increased with increasing acclimation temperature to reach a maximum of 27.8±0.2°C, lower mean incipient values were below 0°C and were therefore undetermined at acclimation temperatures

We describe the reasons of proceeding Thermal-Vacuum tests for space electronic. We will answer on following questions: why teams are doing TV tests, what kind of phases should be simulated, which situations are the most critical during TV tests, what kind of results should be expected, which errors can be detect. As an example, will be shown TV-test of SIR-2 instrument for Chandrayaan-1 moon mission.

[1] Using new SMART-1 AMIE images and Arecibo and Goldstone high resolution radar images of the Moon, we investigate the geological relations of the south pole, including the 20 km-diameter crater Shackleton. The south pole is located inside the topographic rim of the South Pole-Aitken (SPA) basin, the largest and oldest impact crater on the Moon and Shackleton is located on the edge of an interior basin massif. The crater Shackleton is found to be older than the mare surface of the Apollo 15 landing site (3.3 Ga), but younger than the Apollo 14 landing site (3.85 Ga). These results suggest that Shackleton may have collected extra-lunar volatile elements for at least the last 2 billion years and is an attractive site for permanent human presence on the Moon.

[1] Substorms play an important role in the energization and transport of plasmas in planetary magnetospheres, including the shedding of the mass added by moons in the case of Jupiter and Saturn. Mass shedding occurs through rapid reconnection in the near tail resulting in dipolarization on the magnetospheric side of the reconnection point and plasmoid formation down tail. Observations of these sudden reconnection events in Saturn’s near-tail region provide additional insight into this process. Saturnian substorms, at least on occasion, have a plasmoid formation phase leading to a traveling compression region. Changes in the field strength across reconnection events suggest that open flux has been removed from the tail. The timing of tail reconnection events appears to be controlled by both the orbital phase of Titan, and the variable stretching of the near-tail field as Saturn rotates.

Earth's composition, evolution and structure are in part a legacy of provenance (where it happened to form) and chance (the stochastics of that formation).

The oscillating peak model of basin and crater formation proposed by Murray is analysed mathematically. The results could be compared with some basins in order to confirm the basic ideas of this model.

We studied factors influencing variation in nightly levels of activity (birds arriving and vocalizing) and numbers of birds staging offshore at a colony of Ancient Murrelets at Reef Island, British Columbia, during 1984, 1985, and 1986. Activity was restricted to the hours of darkness and extremely variable in magnitude from night to night. The rate of entry into burrows tended to decrease, and the amount of vocalization and numbers of birds at the staging area increased during the nesting season. We detected an underlying 4-day cyclical pattern of attendance. Nightly variability of activity at the colony was affected by moonlight and weather conditions. Since activity, particularly vocalization, was reduced on moonlit nights, we suggest that nocturnal colony attendance is a strategy to avoid diurnal predators in this species. The largest numbers of birds were present and vocalizing at the colony on calm moonless nights. Weather conditions explained a substantial proportion of the night to night variability in murrelet activity. Among weather variables, wind speed had the most consistent effect and was particularly important in 1985. Both short-term, i.e., of a particular night, and long-term, i.e., over the previous 3 days, conditions influenced activity. Our observations suggest that direct weather effects at the colony may be more important than weather effects related to foraging conditions. Interyear differences in activity may have resulted from the interaction of weather and general foraging conditions.

Traduction du Linéaire B dans les tablettes 39=AS 1517 (LXXXVIII), de Cnosos et 31 = AE 04 [134], de Pylos.; Dans le domaine des recherches archéologiques menées sur la période mycénienne, il existe une richesse telle de documentation qu'elle oblige à admettre l'importance de la pratique religieuse dans le monde mycénien. Toutefois, il y a un hiatus important entre cette évidence et les données qui se déduisent à la lecture du Linéaire B. Cette situation nous amène à penser que le point de faiblesse dans la recherche réside dans un problème de méthode de la traduction des textes. La seule solution consiste à reprendre les textes en considérant les avancées produites par l'archéologie et l'iconologie, en l'augmentant d'une critique philologique, historique, herméneutique outre une réflexion interprétative sur les symboles religieux et les mythes. Le mot "kreetízoo" signifie "imiter les habitants de la Crète, tromper", ce qui s'applique au Linéaire B: le système d'écriture, fait d'un héritage d'un grand passé historique, est trompeur pour cacher le sens de ce qui est écrit. On peut avancer qu'il était intentionnellement écrit de manière à ressembler à de simples listes de personnel ou d'approvisionnement car un fort tabou frappait la manifestation religieuse écrite. Ici on présente deux tablettes, les premières à être traduites sans la moindre lacune, et on démontre il s'agit d'une écriture sacrée qui traite de rites de sacrifices, mythes et rites d'initiation.

A new combined rhenium-osmium– and platinum-group element data set for basalts from the Moon establishes that the basalts have uniformly low abundances of highly siderophile elements. The data set indicates a lunar mantle with long-term, chondritic, highly siderophile element ratios, but with absolute abundances that are over 20 times lower than those in Earth's mantle. The results are consistent with silicate-metal equilibrium during a giant impact and core formation in both bodies, followed by post–core-formation late accretion that replenished their mantles with highly siderophile elements. The lunar mantle experienced late accretion that was similar in composition to that of Earth but volumetrically less than (∼0.02% lunar mass) and terminated earlier than for Earth.

17 p.; International audience