Contents Volume 15     

R. M. Sharples  S. K. Ramsay  R. Davies  M. Lehnert 《Experimental Astronomy》2003,15(3):197-198

Volume Contents

Contents Volume 15  相似文献   

Structure of Cl-containing silicate and aluminosilicate glasses: A Cl MAS-NMR study     

Travis O. Sandland  Jonathan F. Stebbins  James D. Webster 《Geochimica et cosmochimica acta》2004,68(24):5059-5069

Chlorine-35 magic angle spinning (MAS) nuclear magnetic resonance (NMR) spectra were collected at 14.1 and 18.8 Tesla fields to determine the atomic scale structural environments of the chloride ions in anhydrous and hydrous silicate and aluminosilicate glasses containing 0.2 to 0.7 wt% Cl. NMR peaks are broad and featureless, but are much narrower than the total chemical shift range for the nuclide in inorganic chlorides. Peak widths are primarily due to quadrupole interactions and to a lesser extent to chemical shift distributions. Peak positions are quite different for the Na- and Ca-containing glasses, suggesting that most Cl⁻ coordination environments contain network modifier cations. Comparison of peak positions and shapes for silicate and aluminosilicate glasses containing either Na or Ca suggests that there is no obvious contribution from Cl⁻ bonded to Al, and relative quantitation of peak areas indicates that there is no systematic undercounting of ³⁵Cl spins in the aluminous vs. the Al-free samples. In Ca-Na silicate glasses with varying Ca/(Ca + Na), the mixed-cation glasses have intermediate chemical shifts between those of the end members, implying that there is not a strong preference of either Ca²⁺ or of Na⁺ around Cl⁻. Hydrous Na-aluminosilicate glasses with H₂O contents up to 5.9 wt% show a shift to higher frequency NMR signal with increasing H₂O content, while the quadrupole coupling constant (C_Q) remains constant at ∼3.3 MHz. However, the change in frequency is much smaller than that expected if H₂O systematically replaced Na⁺ in the first-neighbor coordination shell around Cl⁻. A series of hydrous Ca-aluminosilicate glasses with H₂O contents up to 5.5 wt% show no shift in NMR signal with increasing H₂O content. The C_Q remains constant at ∼4.4 MHz, again suggesting no direct interaction between Cl⁻ and H₂O in these samples.  相似文献   

Hydrothermal convection in carbonaceous chondrite parent bodies     

Bryan J. Travis  Gerald Schubert 《Earth and Planetary Science Letters》2005,240(2):234-250

Numerical simulations of the thermal evolution of carbonaceous chondrite parent bodies indicate a period of several million years during which convective motion of water could occur. The present study considers variations of permeability, radiogenic heating, and body radius. The model accounts for the radial variation of gravity within the body, melting of ice, freezing of liquid water, and variable water properties and incorporates a realistic equation of state for water. Some regions of a parent body experience no pore water flow while other regions experience hundreds of pore volumes of liquid water flow. The spatial heterogeneity in pore water flow reflects the convective pattern in the body. Hydrothermal alteration of minerals inside the parent body will accordingly vary greatly with location in the body, and one parent body could be the source of chemically diverse meteorites.  相似文献   

White dwarf masses in magnetic cataclysmic variables: multi-temperature fits to Ginga data     

Mark Cropper  Gavin Ramsay  & Kinwah Wu 《Monthly notices of the Royal Astronomical Society》1998,293(3):222-232

One method of obtaining the mass of the white dwarf in magnetic cataclysmic variables (mCVs) is through their hard X-ray spectra. However, previous mass estimates using this method give lower limits because the temperature of the plasma in the post-shock region (where the hard X-rays are emitted) is lower than the temperature of the shock itself. In AM Her systems, the additional cooling of the post-shock plasma by cyclotron emission will further lower the derived mass. Here we present estimates of the masses of the white dwarf in 13 mCVs derived using Ginga data and a model in which X-rays are emitted from a multi-temperature emission region with the appropriate temperature and density profile. We include in the model reflection from the surface of the white dwarf and a partially ionized absorber. We are able to achieve good fits to the data. We compare the derived masses with previous estimates and the masses for larger samples of isolated white dwarfs and those in CVs.  相似文献   

Mineralogy,geochemistry and petrogenesis of the Metters Bore No. 1 lamproite pipe,Calwynyardah Field,West Kimberley Province,Western Australia     

Hwang  P.  Taylor  W. R.  Rocky  N. M. S.  Ramsay  R. R. 《Mineralogy and Petrology》1994,51(2-4):195-226

Summary The Metters Bore No. 1 lamproite (MB1) is a small unexposed pipe located in the Calwynyardah field of the Miocene West Kimberley lamproite province. Microdiamonds have been recovered from bulk sampling of the pipe but no macrodiamonds (>0.8 mm) have been found. The pipe contains both volcaniclastic and magmatic (i.e. non-fragmental, extrusive-to-hypabyssal facies) lamproite. The latter rock is dominantly olivine-leucite-diopside lamproite and comprises phenocrysts and microphenocrysts of diopside, altered olivine ( Fo₉₁), and rare phlogopite, together with phenocrysts and glomeroporphyritic aggregates of altered leucite. These are set in an altered, fine-grained to glassy groundmass including diopside, leucite, priderite, apatite, less abundant chrome-spine', perovskite, interstitial richterite with minor calcic amphibole, ilmenite, sphene and wadeite. Mineral compositions are complex and variable: for example: five compositionally distinct fields can be recognizedamong the diopsides, and three among the phlogopites. The Ti-rich, Al-poor diopsides, Ti-F-rich, Al-poor phlogopites, and potassium titanian richterites all have apparent tetrahedral site deficiencies which can best be explained by tetrahedral substitution of Ti⁴⁺ and/or Mg²⁺; no substitution of Fe³⁺ is indicated. Three major types of spinel are recognized: olivine-included titaniferous magnesiochromite (TMC), xenocrystic aluminous magnesiochromite (AMC) and leucite-included pleonaste. Spinel-olivine-melt oxygen barometry indicates that the TMC spine's crystallized from evolving lamproite magma under low oxygen fugacity conditions (MW to IW). Manganiferous groundmass ilmenite has low calculated Fe₂O₃ (< 1 wt%), also consistent with reduced conditions. The maintenance of a low oxidation state during magmatic crystallization, a feature shared with the Argyle olivine-lamproite, is considered a significant factor in preservation of the MB1 microdiamond population. Xenocrystic minerals encountered in heavy mineral concentrates (HMC) indicate that the MB1 lamproite sampled upper mantle spinel ±garnet lherzolite from >60 km depth and crustal mafic rocks. Geochemically, MB1 is typical of West Kimberley leucite-lamproites, which are characterized by high TiO₂ (> 4 wt%), low CaO (< 5 wt%), MgO < 10wt%, and enrichment in incompatible elements (Rb, Sr, Ba, LREE, etc.). Although MB1 is an olivine-bearing lamproite, it has source-related geochemical features, e.g. mantle-normalized Sc/V and Zr/Nb ratios of < 0.75 and > 0.6, respectively, that are similar to other West Kimberley leucite-lamproites and distinct from olivine-lamproites. Petrogenetically, the bulk composition and low magmatic oxidation state of MB1 supports an origin by melting of phlogopite-bearing harzburgitic source under reduced fO₂ (< MW) conditions.

---

Mineralogie, geochemie und petrogenese der lamproit-pipe Metters Bore No. 1, Kalwynyardah Field, West Kimberley Provinz, West-Australien

Zusammenfassung Der Lamproit Metters Bore No. 1 (MB1) ist eine kleine, nicht an der Oberfläche aufgeschlossene Pipe im Kalwynyardah Gebiet der miozänen Lamproit-Provinz von West Kimberley. Mikrodiamanten sind bei der Untersuchung von Proben aus der Pipe gefunden worden, jedoch keine Makrodiamanten (> 0.8 mm). Die Pipe enthält sowohl vulkanoklastischen wie magmatischen Lamproit (nicht-fragmentierte extrusive bis hypabyssische Fazies). Bei dem magmatischen lamproit handeltes sich um einen Olivin-Leuzit-Diopsid-Lamproit mit Kristallen und Mikrokristallen von Diopsid, umgewandeltem Olivin ( Fo₉₁), seltener Phlogopit, zusammen mit Kristallen und glomeroporphyritischen Aggregaten von umgewandeltem Leuzit. Diese sitzen in einer umgewandelten, feinkörnigen bis glasigen Grundmasse mit Diopsid, Leuzit, Priderit, Apatit, seltener Chromspinell, Perovskit, Richterit mit geringen Mengen an Kalziumamphibol, Ilmenit, Titanit und Wadeit. Die Mineralzusammensetzungen sind komplex und variabel: so können z.B. fünf der Zusammensetzung nach eindeutig definierte Felder für die Diopside nachgewiesen werden und drei solche für die Phlogopite. Die Ti-reichen Al-armen Diopside, Ti-F-reiche Al-arme Phlogopite und Kalium-Titan-Richterite haben alle reduzierte Besetzungen von Tetraederstellen, die am besten durch tetraedrische Substitution von Ti⁴⁺ und/oder Mg` erklärt werden können. Es gibt keine Hinweise für Substition von Fe³⁺. Drei Haupttypen von Spinellen kommen vor: Titan-führender Magnesiochromit (TMC) als Einschlüsse in Olivin, aluminiumführender Magnesiochromit (AMC) und Pleonast, der in Leuzit eingeschlossen ist. Sauerstoffbarometrie (Spinell-Olivin-Schmelze) zeigt, daß die TMC Spinelle von einem fraktionierten lamproitischen Magma bei niedriger Sauerstofffugazität (MW bis IW) kristallisiert sind. Manganführender Ilmenit der Grundmasse hat niedrige berechnete Fe₂O₃ Gehalte (< 1 %), und auch das entspricht reduzierenden Bedingungen. Die Erhaltung eines niedrigen Oxydationsstatus während der magmatischen Kristallisation ist eine Eigenschaft, die auch im Olivin-Lamproit der Argyle Pipe zu beobachten ist. Dies wird als ein signifikanter Faktor für den Erhalt der Mikrodiamanten in MBI gesehen. Xenokristalle die in Schwermineral-Konzentraten (HMC) vorkommen, weisen darauf hin, daß der MB1 Lamproit Material des oberen Mantels (Spinell ± Granatlherzolit) aus mehr als 60 km Tiefe, sowie mafische Gesteine der Kruste aufgenommen hat. Geochemisch gesehen ist MB1 typisch für die Leuzit-Lamproite von West Kimberley, welche durch hohe TiO₂ (> 4 wt.%), niedrige CaO (< 5 wt.%), MgO (< 10 wt.%) und Anreicherung von inkompatiblen Elementen (Rb, Sr, Ba, LSEE, etc.) charakterisiert werden. Obwohl MB1 ein Olivin-führender Lamproit ist, zeigt er geochemische Eigenschaften, wie Mantel-normalisierte Sc/V und Zr/Nb Verhältnisse von < 0.75 und > als 0.6, die ähnlich anderen Leuzit-Lamproiten von West Kimberley sind und sich von Olivin-Lamproiten unterscheiden. Petrogenetisch gesehen weisen sowohl die Gesamtzusammensetzung als auch der niedrige magmatische Oxydationsstatus von MBI auf eine genese durch Aufschmelzen von Phlogopit-führendem Harzburgit unter reduzierenden f0₂ (< MW) Bedingungen hin.

---

---

Deceased

---

With 12 Figures  相似文献   

Geometrical constraints upon the unipolar model of V407 Vul and RXJ0806.3+1527     

S. C. C. Barros  T. R. Marsh  P. Groot  G. Nelemans  G. Ramsay  G. Roelofs  D. Steeghs  J. Wilms 《Monthly notices of the Royal Astronomical Society》2005,357(4):1306-1312

  相似文献   

Near-infrared spectroscopic search for the close orbiting planet HD 75289b     

J. R. Barnes  C. J. Leigh  H. R. A. Jones  Travis S. Barman  D. J. Pinfield  A. Collier Cameron  J. S. Jenkins 《Monthly notices of the Royal Astronomical Society》2007,379(3):1097-1107

We present a search for the near-infrared spectroscopic signature of the close orbiting extrasolar giant planet HD 75289b. We obtained ∼230 spectra in the wavelength range 2.18–2.19 μm using the Phoenix spectrograph at Gemini South. By considering the direct spectrum, derived from irradiated model atmospheres, we search for the absorption profile signature present in the combined star and planet light. Since the planetary spectrum is separated from the stellar spectrum at most phases, we apply a phase-dependent orbital model and tomographic techniques to search for absorption signatures.
Because the absorption signature lies buried in the noise of a single exposure we apply a multiline deconvolution to the spectral lines available in order to boost the effective signal-to-noise ratio (S/N) of the data. The wavelength coverage of 80 Å is expected to contain ∼100 planetary lines, enabling a mean line with S/N of 800 to be achieved after deconvolution. We are nevertheless unable to detect the presence of the planet in the data and carry out further simulations to show that broader wavelength coverage should enable a planet like HD 75289b to be detected with 99.9 per cent confidence. We investigate the sensitivity of our method and estimate detection tolerances for mismatches between observed and model planetary atmospheres.  相似文献   

Spin up in RX J0806+15: the shortest period binary     

Pasi Hakala  Gavin Ramsay  Kinwah Wu  Linnea Hjalmarsdotter  Silva Järvinen  Arto Järvinen  Mark Cropper 《Monthly notices of the Royal Astronomical Society》2003,343(1):L10-L14

  相似文献   

X-ray spectroscopy of the intermediate polar PQ Gem     

Cynthia H. James  Gavin Ramsay  Mark Cropper  Graziella Branduardi-Raymont 《Monthly notices of the Royal Astronomical Society》2002,336(2):550-558

  相似文献   

STJ observations of the eclipsing polar HU Aqr     

C. M. Bridge  Mark Cropper  Gavin Ramsay  M. A. C. Perryman  J. H. J. de Bruijne  F. Favata  A. Peacock  N. Rando  A. P. Reynolds 《Monthly notices of the Royal Astronomical Society》2002,336(4):1129-1138

  相似文献