On the solar oblateness: The combined effect of a pole-equator difference in effective temperature and mechanical heating

With the help of a model atmosphere of the Sun we evaluate the pole-equator difference in flux (as measured by Dicke and Goldenberg) assuming the following type of pole-equator temperature difference (T=T _e –T _p ): (a) T 2K for > ₀ (₀ 0.05); (b) T 10K for < ₀.The small T at all optical depths given by (a) could, for example, be due to a pole-equator difference in effective temperatures. At small optical depths a difference in mechanical heating could give rise to the larger temperature difference given by (b). We compare the results of our calculations with Dicke and Goldenberg's observations.The National Center for Atmospheric Research is sponsored by the National Science Foundation.     

Some maps of isanomalies in energy balance climatology

Summary A series of world maps of isanomalies of annual and seasonal global radiation, net radiation, latent heat flux, sensible heat flux, maps of residuals from regression, radiation efficiency, and the Bowen Ratio have been constructed on the data base ofBudyko's Atlas of the Heat Balance of the Earth, 1963. Among the major features observed was the dissimilarity in patterns of isanomalies for the eastern and western sectors of the world's semi-permanent subtropical highs and the great difference between oceanic and continental surfaces.

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Zusammenfassung Auf Grund der Werte vonBudykos Atlas der Wärmebilanz der Erde (1963) wurden eine Anzahl Weltkarten der Isanomalien der jährlichen und der jahreszeitlichen Werte für die Globalstrahlung, die totale Strahlungsbilanz, den latenten und den fühlbaren Wärmefluß sowie Karten für die Abweichungen von der Regressionsgeraden, für den Strahlungsgenuß und für den Bowen-Quotienten konstruiert. Als Hauptergebnisse sind die Unähnlichkeit im Verlauf der Isanomalien zwischen dem östlichen und dem westlichen Sektor der semipermanenten Hochdruckgebiete der Subtropen sowie die großen Unterschiede zwischen ozeanischen und kontinentalen Gebieten zu nennen.

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Résumé En partant des valeurs publiées parBudyko dans son Atlas du bilan thermique de la Terre (1963), on a établi un certain nombre de cartes du globe. Sur celles-ci, on a reporté les isanomalies des valeurs annuelles et saisonières de la radiation globale, du bilan total radiatif, du flux des chaleurs latente et sensible ainsi que l'écart à la droite de régression pour le rayonnement reçu et pour le rapport de Bowen. Le résultat principal en est l'appararition de dissemblances dans le cours des isanomalies entre les secteurs oriental et occidental des anticyclones semipermanents des zones subtropicales ainsi que de différences importantes entre les régions océaniques et continentales.

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With 28 Figures     

Geothermal gas equilibria

Comparison of theoretical and analytical equilibrium constants based on the reactions CH₄ + 2H₂O = CO₂ + 4H₂, 2NH₃ = N₂ + 3H₂ and iron(II)-aluminium-silicate + 2H₂S = FeS₂ + H₂ + aluminium-silicate, shows that the composition of fluids discharged from geothermal areas in New Zealand (Wairakei, Kawerau, Broadlands) reflects close to complete attainment of chemical equilibrium within the system H₂O, CO₂, H₂S, NH₃, H₂, N₂ and CH₄. Under conditions prevailing in explored geothermal systems in New Zealand, the minerals graphite (elemental carbon), anhydrite, pyrrhotite, magnetite do not appear to take part in the overall equilibrium system. The three physical parameters required to evaluate geothermal gas reactions are temperature, pressure and vapor-liquid ratios within the gas equilibration zone.     

Response of rocks to impact loading by bars with pointed ends

SummaryResponse of Rocks to Impact Loading by Bars with Pointed Ends An experimental investigation was undertaken to study the response of three rocks — shale, limestone and diorite — to dynamic loading modelling hammer drilling. A long transmission rod subjected to pendulum impact at its distal end transmitted stress waves to six different heads whose tips consisted of 60°, 90°, and 120° cones or wedges in initial contact with the rock surface. Force and linear penetration histories monitored near the interface were found to be in good agreement with predicted values based on strain measurements at the center and distal end of the transmission bar and use of a one-dimensional theory of elastic wave propagation. The dynamic indentation measurements were also found to be in good agreement witha posteriori determination of the crater depth.Effects of multiple wave reflections and repeated impact on the contact force and rock deformation were determined as a function of the input energy. It was found that an optimum value of this energy exists for most efficient penetration for each of the heads utilized. Dynamic force-penetration curves were compared with corresponding static values obtained from an Instron testing machine. The force history resulting from the impact of a commercial pick-ax suspended in a pendulum arrangement was measured for both the conical and wedge-shaped tips of the device.

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ZusammenfassungDas Verhalten von Gesteinen unter stoartiger Belastung mittels gespitzter Stäbe Es wurde eine experimentelle Untersuchung des Verhaltens dreier Gesteine, nämlich grüner Tonschiefer, Kalkstein und Diorit, unter stoßartiger Belastung, die als Modell der Wirkung eines Bohrhammers dienen soll, durchgeführt. Ein langer Stab war vorne mit einer Spitze in Keil- oder Kegelform mit einem Öffnungswinkel von 60°, 90° oder 120° versehen, welche bei Versuchsbeginn gerade die Probe berührte. Am anderen Ende wurde der Stab von einem fallenden Pendel getroffen. Der zeitliche Verlauf der Kraft und der Eindringung, die in der Nähe der Spitze des Stabes gemessen wurde, stimmte gut mit jenen Werten überein, die auf Grund von Dehnungsmessungen in der Mitte und am Stoßpunkt mittels einer eindimensionalen Theorie der Wellenfortpflanzung errechnet wurden. Die dynamischen Tiefenmessungen des Kraters ergaben auch eine gute Übereinstimmung mit den Werten, die nach dem Experiment bestimmt wurden.Die Wirkung von mehreren Wellenreflexionen und wiederholtem Stoß auf die Kontaktkraft und die Gesteinsdeformation wurde als Funktion der Anfangsenergie bestimmt. Es zeigte sich, daß es für jede verwendete Spitzenform einen optimalen Energiebetrag gibt, bei dem die günstigste Eindringung erfolgt. Dynamische Kraft-Eindringungskurven werden verglichen mit den entsprechenden statischen Werten, die mittels einer Instron-Testapparatur gemessen wurden. Überdies wurde der Kraftverlauf an Keil- und Kegelende einer Spitzhacke, die als Pendel auf eine Steinprobe aufschlug, gemessen.

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RésuméReponses de certaines roches aux chocs exercés par des barres à extremités pointues Des expériences ont èté entreprises pour étudier la reponse de trois roches — schiste vert, calcaire, diorite — aux percussions exercées par un modèle de marteau perforateur. Un pendule ballistique heurte l'extremité libre d'une longue barre, à travers laquelle des ondes de contrainte se propagent et atteignent à l'autre extrémité une tête constitutée suivant les cas par une cône ou un dièdre d'angle 60°, 90° ou 120°, en contact avec la roche à l'instant initial. Les résultats obtenus en ce qui concerne l'évolution de la rorce et l'évolution de la pénétration lineaire sont en bon accord avec les valeurs prédites par le théorie unidimensionelle de la propagation des ondes élastiques, à partir des constrainte mesurées au centre et à l'extremité libre de la barre. Les mesures de la pénétration pendant l'experiénce sont également en bon accord avec la détermination à postériori de la profondeur des cratères.L'effet des réflexions multiples des ondes et l'effet de la répétition des impacts sur la force de contact et sur la déformation de la roche sont déterminés en fonction de l'énergie d'impact. Pour chacune des têtes utilisées on a trouvé qu'il existe une énergie optimale, c'est à dire une energie permettant d'obtenir la meilleure pénétration. Les courbes représentant la pénétration dynamique en fonction de la force sont comparées aux courbes correspondant en cas statique, obtenus par une machine d'Instron. L'évolution de la force résultant de l'impact d'une pioche ordinaire a èté mesurée pour des têtes constituées soit par des cônes soit par des dièdres.

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With 27 Figures     

Über Den Aufbau Der Stern- Und Galaxienhaufen

In star clusters and in galaxy clusters the exponentn of the generalized law of Schuster statistically decreases with increasing masses of the clusters or increasing numbersL of their members. In most casesn(gal. cl.) is smaller thann(st. cl.). It is confirmed, that in larger galaxy clusters the brighter members are somewhat more concentrated at the center than the fainter members.

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Mitteilungen Serie A.     

A multi-proxy record of the Last Glacial Maximum and last 14,500?years of paleoenvironmental change at Lone Spruce Pond, southwestern Alaska

Sediment cores from Lone Spruce Pond (60.007°N, 159.143°W), southwestern Alaska, record paleoenvironmental changes during the global Last Glacial Maximum (LGM), and during the last 14,500 calendar years BP (14.5?cal?ka). We analyzed the abundance of organic matter, biogenic silica, carbon, and nitrogen, and the isotope ratios of C and N, magnetic susceptibility, and grain-size distribution of bulk sediment, abundance of alder shrub (Alnus) pollen, and midge (Chironomidae and Chaoboridae) assemblages in a 4.7-m-long sediment sequence from the depocenter at 22?m water depth. The basal unit contains macrofossils dating to 25?C21?cal?ka (the global LGM), and is interpreted as glacial-lacustrine sediment. The open water requires that the outlet of the Ahklun Mountain ice cap had retreated to within 6?km of the range crest. In addition to cladocerans and diatoms, the glacial-lacustrine mud contains chironomids consistent with deep, oligotrophic conditions; several taxa associated with relatively warm conditions are present, suggestive of relative warmth during the global LGM. The glacial-lacustrine unit is separated from the overlying non-glacial lake sediment by a possible disconformity, which might record a readvance of glacier ice. Non-glacial sediment began accumulating around 14.5?cal?ka, with high flux of mineral matter and fluctuating physical and biological properties through the global deglacial period, including a reversal in biogenic-silica (BSi) content during the Younger Dryas (YD). During the global deglacial interval, the ??¹³C values of lake sediment were higher relative to other periods, consistent with low C:N ratios (8), and suggesting a dominant atmospheric CO₂ source of C for phytoplankton. Concentrations of aquatic faunal remains (chironomids and Cladocera) were low throughout the deglacial interval, diversity was low and warm-indicator taxa were absent. Higher production and air temperatures are inferred following the YD, when bulk organic-matter (OM) content (LOI 550?°C) increased substantially and permanently, from 10 to 30?%, a trend paralleled by an increase in C and N abundance, an increase in C:N ratio (to about 12), and a decrease in ??¹³C of sediment. Post-YD warming is marked by a rapid shift in the midge assemblage. Between 8.9 and 8.5?cal?ka, Alnus pollen tripled (25?C75?%), followed by the near-tripling of BSi (7?C19?%) by 8.2?cal?ka, and ??¹⁵N began a steady rise, reflecting the buildup of N and an increase in denitrification in soils. Several chironomid taxa indicative of relatively warm conditions were present throughout the Holocene. Quantitative chironomid-based temperature inferences are complicated by the expansion of Alnus and resulting changes in lake nutrient status and production; these changes were associated with an abrupt increase in cladoceran abundance and persistent shift in the chironomid assemblage. During the last 2,000?years, chironomid-assemblage changes suggest cooler temperatures, and BSi and OM values were generally lower than their maximum Holocene values, with minima during the seventh and eighth centuries, and again during the eighteenth century.     

Die Galaktische BeschleunigungK(z) Und Das Lokale System

The galactic accelerationK(z) calculated by Perry (1969) is explained by the influence of a local galactic mass concentration.

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Mitteilungen Serie A, Nr. 46.     

On the possibility of earth-type habitable planets around 47 UMa

We investigate whether Earth-type habitable planets can in principle exist in the planetary system of 47 UMa. The system of 47 UMa consists of two Jupiter-size planets beyond the outer edge of the stellar habitable zone, and thus resembles our own Solar System most closely compared to all exosolar planetary systems discovered so far. Our study of habitability deliberately follows an Earth-based view according to the concept of Franck and colleagues, which assumes the long-term possibility of photosynthetic biomass production under geodynamic conditions. Consequently, a broad variety of climatological, biogeochemical, and geodynamical processes involved in the generation of photosynthesis-driven life conditions is taken into account. The stellar luminosity and the age of the star/planet system are of fundamental importance for planetary habitability. Our study considers different types of planetary continental growth models and takes into account a careful assessment of the stellar parameters. In the event of successful formation and orbital stability, two subjects of intense research, we find that Earth-type habitable planets around 47 UMa are in principle possible! The likelihood of those planets is increased if assumed that 47 UMa is relatively young (?6 Gyr) and has a relatively small stellar luminosity as permitted by the observational range of those parameters.     

Galaxies in Interaction

Posters: Because of the large number of contributions, some oral presentations had to be transferred into Posters. The reader is referred to the final programme for the actual allocation of Posters. A01 Chemical Enrichment of the Intracluster Medium A02 Structural analysis of high‐velocity clouds – Evidence for an interaction between the Milky Way and the Magellanic System A03 Multi‐Phase Chemo‐Dynamical SPH code for galaxy evolution A04 The proper motion of M33 A05 Wavelet analysis of Intra–group Light in Hickson Compact Groups A06 Evidence for an evolutionary connection between early and late type dwarf galaxies A07 Dwarf Galaxies in the NGC 5846 Group A08 X‐ray spectroscopy of serendipitous clusters of galaxies in XMM‐Newton observations A09 Evolution of smale scale systems of galaxies: X‐ray detected E+S galaxy pairs A10 Modelling Star Formation in Interacting Galaxies A11 NGC 1427A – the beginning of the end: a lonely dwarf irregular entering the dense core of the Fornax cluster A12 Dwarf galaxies in galaxy groups: Photo‐evaporation, orbits and gas stripping A13 High resolution stellar kinematics for the central component of the Polar Ring Galaxy NGC 4650A A14 The Influence of Environment on the Morphological Evolution of Disk‐Dominated Galaxies A15 Interactions and star formation in galaxies A16 Dust Condensations and Molecular Clouds in Interacting Spirals A17 Star formation rates and kinematics of modelled interacting galaxies A18 Evolution of Galaxies and the Tully–Fisher Relation A19 Evolution and Collision of Galaxies on the GRID A20 Multiwavelength observations of two S+E merger candidates: the Medusa and NGC 4441 A21 Interacting Galaxies in Small Galaxy Groups A22 Virial and total masses of galaxy triplets in the Local Supercluster A23 Simulations of Interaction Processes of Galaxies with the Intra‐Cluster Medium A24 Chemical evolution of the thick and thin disks of our Galaxy A25 Dust properties of UV‐bright galaxies at z ∼ 2 A26 Simulation of the Gravitational Collapse and Fragmentation of Rotating Molecular Clouds A27 NGC 5719/13: interacting spirals forming a counter‐rotating stellar disc A28 Starbursts in very metal‐poor dwarfs due to interactions and mergers: link to the processes in the high‐redshift young galaxies A29 Testing galaxy evolution in the field: morphology and properties of the diffuse X‐ray emission in shell galaxies A30 Effects of galactic winds on dIrrs with particular emphasis on NGC 1569 and the refill of superbubble cavities A31 Galaxy formation through merging at z ≈ 2 A32 3D simulations of the ISM‐ICM interaction of disk galaxies in clusters A33 Gas replenishment in ram pressure stripped disk galaxies A34 New Results on the Kinematics of the Outer Cluster System of NGC 1399 A35 Chemical gradient evolution in massive galaxy disk due to its minor merger with dwarf galaxy A36 The complex kinematics of galaxies in Hickson 62 A37 Dust in the outer regions of interacting galaxies A38 Dynamical interaction of M31 and M32 A39 A comparative study of galaxy properties in low‐ and high density environment A40 Compact Groups in Dense Environment: The Case of IC1370 A41 The Star Formation History of CG J1720‐67.8 A42 Galaxy populations in the infall regions of intermediate redshift clusters A43 The study of gravitational fragmentation in two‐clumps collisions A44 Star Formation Activity in Galaxy Clusters Near and Far A45 An Exploration of the Merging History of the Local Starburst Galaxy, NGC 3310 A46 The high‐velocity clouds of M31: tracers of galactic evolution A47 The Properties of Fossil Groups     

A simple model for lensing by black holes in galactic nuclei

The lensing properties of the Plummer model with a central point mass and external shear are derived, including the image multiplicities, critical curves and caustics. This provides a simple model for a flattened galaxy with a central supermassive black hole. For the Plummer model with black hole, the maximum number of images is four, provided the black hole mass is less than an upper bound which is calculated analytically. This introduces a method to constrain black hole masses by counting images, thus applicable at cosmological distance. With shear, the maximum number of images is six and we illustrate the occurrence of an astroid caustic and two metamorphoses.