Launch window study for the highly eccentric orbit satellite HEOS-1

A satellite with a high eccentricitye0.95 is strongly perturbed by the sun and the moon. This fact and mission constraints restrict considerably the possible launch times for such a satellte. The launch window calculations can be performed in two steps in order to save computing time. An approximate analytical solution provides a general survey of the launch opportunities. An accurate numerical approach is then necessary for the exact definition of the launch window. In the case of the orbit of HEOS-1 (satellite 68 10901), moreover the consideration of the injection errors has been of great importance.Presented at the Conference on Celestial Mechanics, Oberwolfach, Germany, August 17–23, 1969.     

Navigation formula to A. Busemann's variation problem of space travel

The indicatrix of the variation problem is given (1) by the perturbation differential equation for the semi-major axis and eccentricity, and (2) by a relation between the momentum and eccentric anomaly. The Hamiltonian equations of an extremal solution, therefore, reduce to a navigation equation. The remaining perturbation equations for the longitude of perihelion and the mean longitude at epoch, finally, yield the time dependence that gives the most economic fuel consumption.     

Interstellar graphite in meteorites: Isotopic compositions and structural properties of single graphite grains from Murchison

Abstract— One hundred forty-three carbon grains, ranging in size from 2 to 8 μm, from two chemical and physical separates from the Murchison CM2 chondrite, were analyzed by ion microprobe mass spectrometry for their C- and N-isotopic compositions. Both separates are enriched in the exotic noble gas component Ne-E(L). Ninety grains were also analyzed for their H and O contents and 118, for Si. Thirteen grains were analyzed by micro-sampling laser Raman spectroscopy. Round grains have large C-isotopic anomalies with ¹²C/¹³C ratios ranging from 7 to 4500 (terrestrial ratio = 89). Nitrogen in these grains is also anomalous but shows much smaller deviations from the terrestrial composition, ¹⁴N/¹⁵N ratios ranging from 193 to 680 (terrestrial ratio = 272). Spherulitic aggregates and non-round compact grains have normal C-isotopic ratios but ¹⁵N excesses (up to 35%). Raman spectra of the analyzed grains indicate varying degrees of crystalline disorder of graphite with estimated in-plane crystallite dimensions varying from 18 Å (highly disordered, similar to terrestrial kerogen) to ～750 Å (well-crystallized graphite). Element contents of H, O, and Si are correlated with one another, and H and O are probably present in the form of organic molecules. On the basis of morphology, the round grains fall into two groups: grains with smooth, shell-like surfaces (“onions”) and grains that appear to be dense aggregates of small scales (“cauliflowers”). “Onions” tend to have lower trace element contents, isotopically light C (¹²C/¹³C > 89) and a high degree of crystalline order, whereas “cauliflowers” have a larger spread in trace element contents and C-isotopic ratios (they range from isotopically light to heavy) but tend to have a low degree of crystalline order. However, these differences exist only on average, and no clear distinction can be made for individual grains. A few limited conclusions can be drawn about the astrophysical origin of the carbon grains of this study. The ¹⁵N excesses in spherulitic aggregates and non-round grains can be explained as the result of ion-molecule reactions in molecular clouds. The round grains, on the other hand, must have formed in stellar atmospheres (circumstellar grains). Grains with isotopically light C must have formed in stellar environments characterized by He-burning, either in the atmosphere of Wolf-Rayet stars during the WC phase or in the He-burning, ¹²C-rich zone of a massive star, ejected by a supernova explosion. Isotopically heavy C is produced by H-burning in the CNO cycle. Possible sources for grains with heavy C are carbon stars (AGB stars during the thermally pulsing phase) or novae, but the detailed distribution of ¹²C/¹³C ratios agree neither with the distribution observed in carbon stars nor with theoretical predictions for these two types of stellar sources.     

Interstellar Grains in Primitive Meteorites: Diamond,Silicon Carbide,and Graphite

Abstract— Primitive meteorites contain a few parts per million (ppm) of pristine interstellar grains that provide information on nuclear and chemical processes in stars. Their interstellar origin is proven by highly anomalous isotopic ratios, varying more than 1000-fold for elements such as C and N. Most grains isolated thus far are stable only under highly reducing conditions (C/O > 1), and apparently are “stardust” formed in stellar atmospheres. Microdiamonds, of median size ～ 10 Å, are most abundant (～ 400–1800 ppm) but least understood. They contain anomalous noble gases including Xe-HL, which shows the signature of the r- and p-processes and thus apparently is derived from supernovae. Silicon carbide, of grain size 0.2–10 μm and abundance ～ 6 ppm, shows the signature of the s-process and apparently comes mainly from red giant carbon (AGB) stars of 1–3 solar masses. Some grains appear to be ≥10⁹ a older than the Solar System. Graphite spherules, of grain size 0.8–7 μm and abundance <2 ppm, contain highly anomalous C and noble gases, as well as large amounts of fossil ²⁶Mg from the decay of extinct ²⁶Al. They seem to come from at least three sources, probably AGB stars, novae, and Wolf-Rayet stars.     

Alpine and Pacific styles of Phanerozoic mountain building: subduction-zone petrogenesis of continental crust

A broad continuum exists between two distinct end-member types of mountain building. Alpine-type orogenic belts develop during subduction of an ocean basin between two continental blocks, resulting in collision. They are characterized by an imbricate sequence of oceanward verging nappes; some Alpine belts exhibit superimposed late-stage backthrusting. Sediments are chiefly platform carbonates and siliciclastics, in some cases associated with minor amounts of bimodal volcanics; pre-existing granitic gneisses and related continental rocks constitute an autochthonous–parautochthonous basement. Metamorphism of deeply subducted portions of the orogen ranges from relatively high-pressure (HP) to ultrahigh-pressure (UHP). Calcalkaline volcanic–plutonic rocks are rare, and have peraluminous, S-type bulk compositions. In contrast, Pacific-type orogens develop within and landward from long-sustained oceanic subduction zones. They consist of an outboard oceanic trench–accretionary prism, and an inboard continental margin–island arc. The oceanic assemblage consists of first-cycle, in-part mélanged volcaniclastics, and minor but widespread cherts ± deep-water carbonates, intimately mixed with disaggregated ophiolites. The section recrystallized under HP conditions. Recumbent fold vergence is oceanward. A massive, slightly older to coeval calcalkaline arc is sited landward from the trench complex on the stable, non-subducted plate. It consists of abundant, dominantly intermediate, metaluminous, I-type volcanics resting on old crust; both assemblages are thrown into open folds, intruded by comagmatic I-type granitoids, and metamorphosed locally to regionally under high-T, low-P conditions. In the subduction channel of collisional and outboard Circumpacific terranes, combined extension above and subduction below allows buoyancy-driven ascent of ductile, thin-aspect ratio slices of HP–UHP complexes to midcrustal levels, where most closely approached neutral buoyancy; exposure of rising sheets caused by erosion and gravitational collapse results in moderate amounts of sedimentary debris because exhumed sialic slivers are of modest volume. At massive sialic buildups associated with convergent plate cuSPS (syntaxes), tectonic aneurysms may help transport HP–UHP complexes from mid- to upper-crustal levels. The closure of relatively small ocean basins that typify many intracratonic suture zones provides only limited production of intermediate and silicic melts, so volcanic–plutonic belts are poorly developed in Alpine orogens compared with Circumpacific convergent plate junctions. Generation of a calcalkaline arc mainly depends on volatile evolution at the depth of magma generation. Phase equilibrium studies show that, under typical subduction-zone P–T trajectories, clinoamphibole ± Ca–Al hydrous silicates constitute the major hydroxyl-bearing phases in deep-seated metamorphic rocks of MORB composition; other hydrous minerals are of minor abundance. Ca and Na clinoamphiboles dehydrate at pressures of above approximately 2 GPa, but low-temperature devolatilization may be delayed by pressure overstepping; thus metabasaltic blueschists and amphibolites expel H₂O at melt-generation depths, and commonly achieve stable eclogitic assemblages. Partly serpentinized mantle beneath the oceanic crust dehydrates at roughly comparable conditions. For reasonable subduction-zone geothermal gradients however, white micas ± biotites remain stable to pressures >3 GPa. Accordingly, attending descent to depths of >100 km, mica-rich quartzofeldspathic lithologies that constitute much of the continental crust fail to evolve substantial amounts of H₂O, and transform incompletely to stable eclogite-facies assemblages. Underflow of amphibolitized oceanic lithosphere thus generates most of the deep-seated volatile flux, and the consequent partial melting to produce the calcalkaline suite, along and above a subduction zone; where large volumes of micaceous intermediate and felsic crustal materials are carried down to great depths, volatile flux severely diminishes. Thus, continental collision in general does not produce a volcanic–plutonic arc whereas in contrast, the long-continued contemporaneous underflow of oceanic lithosphere does.     

A menagerie of graphite morphologies in the Acapulco meteorite with diverse carbon and nitrogen isotopic signatures: Implications for the evolution history of acapulcoite meteorites

Morphologies, petrographic settings and carbon and nitrogen isotopic compositions of graphites in the Acapulco meteorite, the latter determined by secondary ionization mass spectrometry, are reported. Seven different graphite morphologies were recognized, the majority of which occur enclosed exclusively in kamacite. Individual graphite grains also rarely occur in the silicate matrix. Kamacite rims surrounding taenite cores of metal grains are separated from the Ni-rich metal cores by graphite veneers. These graphite veneers impeded or prevented Ni-Fe interdiffusion during cooling. In addition, matrix FeNi metal contains considerable amounts of phosphorous (≈ 700 ppm) and silicon (≈ 300 ppm) (Pack et al., 2005 in preparation) thus indicating that results of laboratory cooling experiments in the Fe-Ni binary system are inapplicable to Acapulco metals. Graphites of different morphologies display a range of carbon and nitrogen isotopic compositions, indicating a diversity of source regions before accretion in the Acapulco parent body. The isotopic compositions point to at least three isotopic reservoirs from which the graphites originated: (1) A reservoir with heavy carbon, represented by graphite in silicates (δ¹³C = 14.3 ± 2.4 ‰ and δ¹⁵N = −103.4 ± 10.9 ‰), (2) A reservoir with isotopically light carbon and nitrogen, characteristic for the metals. Its C- and N-isotopic compositions are probably preserved in the graphite exsolutions that are isotopically light in carbon and lightest in nitrogen (δ¹³C = −17 to −23 ‰ δ¹⁵N = −141 to −159 ‰). (3) A reservoir with an assumed isotopic composition (δ¹³C ∼ −5 ‰; δ¹⁵N ∼ −50 ‰). A detailed three-dimensional tomography in reflected light microscopy of the decorations of metal-troilite spherules in the cores of orthopyroxenes and olivines and metal-troilite veins was conducted to clarify their origin. Metal and troilite veins are present only near the fusion crust. Hence, these veins are not pristine to Acapulco parent body but resulted during passage of Acapulco in Earth’s atmosphere. A thorough search for symplectite-type silicate-troilite liquid quench textures was conducted to determine the extent of closed-system partial silicate melting in Acapulco.Metal-troilite spherules in orthopyroxenes and olivines are not randomly distributed but decorate ferromagnesian silicate restite cores, indicating that the metal-spherule decoration around restite silicates took place in a silicate partial melt. Graphite inclusions in these spherules have C- and N- isotopic compositions (δ¹³C = −2.9 ± 2.5 ‰ and δ¹⁵N = −101.2 ± 32 ‰) close to the average values of graphite in metals and in the silicate matrix, thus strongly suggesting that they originated from a mixture of graphite inclusions in metals and silicate matrix graphite during a closed system crystallization process subsequent to silicate-metal-sulfide partial melting. Troilite-orthopyroxene quench symplectite textures in orthopyroxene rims are clear evidence that silicate-sulfide partial melting took place in Acapulco. Due to petrographic heterogeneity on a centimeter scale, bulk REE abundances of individual samples or of individual minerals provide only limited information and the REE abundances alone are not entirely adequate to unravel the formational processes that prevailed in the acapulcoite-lodranite parent body. The present investigations demonstrate the complexity of the evolutionary stages of acapulcoites from accretion to parent body processes.     

CO2-poor composition of the fluid attending Franciscan and Sanbagawa low-grade metamorphism

Previous phase equilibrium and oxygen isotopic researches on the high-pressure, low-temperature metamorphic rocks of the Franciscan and Sanbagawa blueschist type terranes have demonstrated the near ubiquity of a fluid at high (≈ total) pressure and its oxygen-rich nature during metamorphism. The coexistence of quartz with a CaCO₃ polymorph instead of wollastonite, and of sphene rather than rutile + quartz + calcium carbonate in these rocks places narrow, rather low limits on the partial pressures of CO₂, as computed in this note; equilibrium calculations indicate that the mole fraction of carbon dioxide in the fluid must have been less than about 0.04 in the Sanbagawa terrane and less than 0.01 in the Franciscan terrane. The rocks are not sulfated or strongly oxidized, hence the only other likely component which could comprise the balance of this phase is H₂O. Evidently metamorphism in the Sanbagawa belt and particularly in the Franciscan terrane must have taken place in the presence of a highly aqueous fluid.     

Distribution of gold,silver, copper,lead and zinc in the productive Marysville stock,Montana

125 whole rock samples from the productive Marysville, Montana, granodiorite and the surrounding metamorphic rocks were analyzed by neutron activation analysis for gold and silver, and by atomic absorption for copper, lead and zinc. In the vicinity of known gold veins, anomalous values for gold and silver were found in both types of bedrock. Anomalies for the base metals were much less pronounced. The results indicate that systematic analysis of igneous bodies could be useful in exploration for hydrothermal ore deposits.

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Zusammenfassung 125 Gesteinsproben des sogenannten produktiven Granodiorits in Marysville (Montana) wurden durch Neutronenaktivierungsanalyse auf Gold und Silber und mittels Atomabsorptionsanalyse auf Kupfer, Blei und Zink analysiert. In der Nähe bekannter Goldadern wurden in beiden Gesteinsarten ungewöhnlich hohe Gold- und Silber-Werte gefunden. Anomale Werte für Kupfer, Blei und Zink waren seltener. Die Ergebnisse zeigen, daß eine systematische Untersuchung magmatischer Gesteinskomplexe bei der Suche nach hydrothermalen Erzlagerstätten von Nutzen sein kann.

     

Folgerungen für die Entstehung der Basalte aus dem speziellen Auftreten der Pyroxene in diesen Gesteinen

Zusammenfassung Die früheren Angaben über die Pyroxenführung, besonders über den Gehalt an rhombischem Pyroxen, wurden in den Basalten der südwestlichen Ausläufer des Vogelsberges überprüft. Es kann in Abhängigkeit vom SiO₂-Gehalt dieser Gesteine eine Beziehung über die Zusammensetzung der Basalte und die Art der auftretenden Pyroxene aufgestellt werden. Vereinfacht ergibt sich, daß die Olivinbasalte keinen rhombischen Pyroxen in der Grundmasse führen - abgesehen von den Olivinknollen - und die Gesteine mit Bronzitführung dem gabbrodioritischen bzw. dioritischen Magmentyp angehören. Daneben kommt Pigeonit in weiter Verbreitung vor. Diese Befunde unterstützen die Auffassung, daß die Olivinknollen der Basalte Reste von assimilierten Peridotiten sind. die dem basaltischen primären Magma zugefügt werden. Dadurch wird ein Hinweis auf den Ort der Bildung der basaltischen Magmen gegeben.