The $\text{D}\text{H}$ ratio in the atmosphere of Uranus: Detection of the R₅(1) line of HD     

L. Trafton  D.A. Ramsay 《Icarus》1980,41(3):423-429

Observations of Uranus during the 1975, 1976, and 1978 apparitions reveal a weak absorption at the wavelength of the R₅(1) line of HD with equivalent width $\text{1.0 ± 0.4}\text{m}\text{A}\text{?}$. The $\text{D}\text{H}$ ratio in Uranus' atmosphere implied by this line and other published spectra is (4.8 ± 1.5) × 10^?5, and may not be significantly different from that in the atmospheres of Jupiter and Saturn. In addition, the spectra exhibit two weak absorption at $\text{6044.76 ± 0.02}\text{and}\text{6045.54 ± 0.02}\text{A}\text{?}$ which we were unable to identify. No trace of absorption is visible near these wavelengths or near the HD wavelength in a laboratory spectrum of 4.92 km-am CH₄ which we obtained in an attempt to identify these absorption features and to verify that the HD feature does not arise from CH₄.  相似文献   

RApid Temporal Survey (RATS) – I. Overview and first results     

Gavin Ramsay  Pasi Hakala 《Monthly notices of the Royal Astronomical Society》2005,360(1):314-321

We present the aim and first results of the RApid Temporal Survey (RATS) made using the Wide Field Camera on the Isaac Newton Telescope. Our initial survey covers 3 square degrees, reaches a depth of   V ∼ 22.5  and is sensitive to variations on time-scales as short as 2 min: this is a new parameter space. Each field was observed for over 2 h in white light, with 12 fields being observed in total. Our initial analysis finds 45 targets which show significant variations. Around half of these systems show quasi-sinusoidal variations: we believe they are contact or short period binaries. We find four systems which show variations on a time-scale less than 1 h. The shortest period system has a period of 374 s. We find two systems which show a total eclipse. Further photometric and spectroscopic observations are required to fully identify the nature of these systems. We outline our future plans and objectives.  相似文献   

XMM–Newton EPIC and Optical Monitor observations of Her X-1 over the 35-d beat period     

Silvia Zane  Gavin Ramsay  Mario A. Jimenez-Garate  Jan Willem den Herder  Charles J. Hailey 《Monthly notices of the Royal Astronomical Society》2004,350(2):506-516

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On the multi-periodicities in the X-ray dipper XB 1916–053     

L. Homer  †  P. A. Charles  P. Hakala  P. Muhli    I.-C. Shih  A. P. Smale  G. Ramsay 《Monthly notices of the Royal Astronomical Society》2001,322(4):827-842

Using the Rossi X-ray Timing Explorer and the Nordic Optical Telescope, we have obtained the highest ever quality X-ray/white-light high-speed photometry of XB 1916–053. We refine the X-ray period ( P _X) to 3000.6±0.2 s via a restricted cycle counting approach. Using our complete optical light curve, we have extended the optical period ( P _opt) ephemeris by another 4 yr, providing further evidence for its stability, although a slightly longer period of 3027.555±0.002 s now provides a marginally better fit. Moreover, modulations at both P _X and P _opt are present in the optical data, with the former dominating the nightly light curves (i.e. a few cycles of data). We have also attempted to determine the 'beat' period, as seen in the repeating evolution of the X-ray dip structure, and the variation in primary dip phase. We find that a quasi-period of 4.74±0.05 d provides the best fit to the data, even then requiring phase shifts between cycles, with the expected 3.90-d 'beat' of P _X and P _opt appearing to be less likely. Finally, considering the nature of each of these temporal phenomena, we outline possible models, which could explain all of the observed behaviour of this enigmatic source, focusing on which of P _X or P _opt is the binary period.  相似文献   

Evidence for pole switching in the magnetic cataclysmic variable BY Camelopardalis     

Paul A. Mason  Gavin Ramsay  Ivan Andronov  Sergey Kolesnikov  Nickolay Shakhovskoy  & Elana Pavlenko 《Monthly notices of the Royal Astronomical Society》1998,295(3):511-518

An analysis of X-ray and optical light curves of the magnetic cataclysmic variable (MCV) BY Cam is presented. This system is one of three MCVs in which the spin period of the white dwarf and the binary orbital period differ by ∼1 per cent. As such these 'BY Cam' stars are important objects with which to probe the field structure of the magnetic white dwarf and ultimately the nature of synchronization of AM Her binaries. We confirm asynchronous rotation of the magnetic white dwarf with respect to the binary. We find evidence that the accretion stream accretes directly on to the white dwarf as in AM Her systems, but further, the stream impacts on to different magnetic poles over the course of the beat period. We present evidence that the optical and hard X-ray light curves modulate in phase, but together they are out of phase with the soft X-ray light curve. We confirm the spin down of the white dwarf which is expected to lead to the synchronization of the spin and orbital periods of BY Cam.  相似文献   

Variation in the Sizes of Chthamalid ­Barnacle Post-Settlement Cyprids on European Shores     

Ruth M. O'Riordan  Jane Delany    David McGrath    Alan A. Myers  Anne Marie Power    Neil F. Ramsay  Damaso Alvarez  Teresa Cruz  Federica G. Pannacciulli    Pedro Range  & Giulio Relini 《Marine Ecology》2001,22(4):307-322

Abstract. As part of a wider study on the settlement and recruitment of Chthamalus spp. in Europe, this study investigated whether chthamalid cyprids can be separated by length on a European scale. Variation in cyprid length with latitude and temporal variation at selected localities were also examined. The lengths of cyprids collected between 1996 – 1999 on nine rocky shores in Europe are reported. Elminius modestus cyprids were found only at Roscoff, NW France and could be distinguished due to their carapace shape and length. They showed a unimodal length distribution, measuring between 450 and 625 µm, with no variation in length between the two sampling dates (1997 and 1998). Based on carapace shape and length, the remaining cyprids in the collections were identified as one of three chthamalid species, Chthamalus montagui, Chthamalus stellatus or Euraphia depressa. Bimodal length distributions of chthamalid cyprids were seen on some shores, while others had a single small‐sized modal group (representing C. montagui on Atlantic shores and/or E. depressa in the Mediterranean) separated from a few distinctly larger cyprids (C. stellatus). Metamorphs collected simultaneously with cyprid collections were identified as C. stellatus or C. montagui, except at Roscoff, where E. modestus were also found. In southern Portugal, where all metamorphs collected were C. montagui and adult C. montagui were the dominant barnacles, most cyprids measured between 350 and 550 µm long and this size distribution coincides with the distribution expected for C. montagui. Cyprids collected on these four more southerly Portuguese shores had the same modal length class (475 µm) and this remained constant between successive years at Luz and Albufeira, Algarve. The smallest (350 µm long) wild chthamalid cyprids found were from southern Portugal and Italy. In Spain, France and Ireland the smallest chthamalid cyprid was 425 µm long. The results from the present study support the hypothesis that on Atlantic shores cyprids of C. montagui can be separated from those of C. stellatus based on size, although there is some variation in cyprid length with latitude as well as temporal variation at selected localities.  相似文献   

Field setting,mineralogy, chemistry,and genesis of arc picrites,New Georgia,Solomon Islands   总被引：5，自引：0，他引：5  

W. R. H. Ramsay  A. J. Crawford  J. D. Foden 《Contributions to Mineralogy and Petrology》1984,88(4):386-402

The field setting, petrography, mineralogy, and geochemistry of a suite of picrite basalts and related magnesian olivine tholeiites (New Georgia arc picrites) from the New Georgia Volcanics, Kolo caldera in the active ensimatic Solomon Islands arc are presented. These lavas, with an areal extent in the order of 100² km and almost 1 km thick in places, are located close to the intersection of the Woodlark spreading zone with the Pacific plate margin. They contain abundant olivine (Fo_94-75) and diopside (Cr₂O₃ 1.1-0.4%, Al₂O₃ 1–3%), and spinels characterised by a large range in Cr/(Cr+Al) (0.85–0.46) and Mg/(Mg+ Fe⁺⁺) (0.65–0.1). The spinels are Fe⁺⁺⁺ rich, with Fe⁺⁺⁺/ (Fe⁺⁺⁺+Cr+Al) varying from 0.06 to 1.0. A discrete group of spinels with the highest Cr/(Cr+Al) (0.83–0.86) and lowest Fe⁺⁺⁺ contents are included in the most Mg-rich olivine (Fo_91–94) and both may be xenocrystal in origin.The lavas, which range between 10–28% MgO, define linear trends on oxide (element) — MgO diagrams and these trends are interpreted as olivine (0.9) clinopyroxene (0.1) control lines. For the reconstructed parent magma composition of these arc picrites, ratios involving CaO, Al₂O₃, TiO₂, Zr, V and Sc are very close to chondritic. REE patterns are slightly LREE — enriched ((La/Sm)^N 1.3–1.43) and HREE are flat. All lavas show marked enrichments in K, Rb, Sr, Ba, and LREE relative to MORB with similar MgO contents, but the TiO₂ content of the proposed parent magma is close to those of postulated primary MORB liquids. It is proposed that the arc parent magma was produced by partial melting of sub-oceanic upper mantle induced by the introduction of LILE — enriched hydrous fluids derived by dehydration and/or partial melting of subducted ocean crust and possibly minor sediments.  相似文献   

The origin of biotite in Archaean meta-sediments near Yellowknife,N.W.T., Canada: A reply to E. H. Brown     

C. R. Ramsay 《Contributions to Mineralogy and Petrology》1974,46(1):77-79

Conclusion Dr. Brown's perceptive criticism has emphasised that problems of detail remain and pointed out some deficiencies of presentation in my paper. I hope these have now been rectified. I believe, however, that the above examination of the reaction in the light of his criteria has served only to substantiate its general validity.  相似文献   

Metamorphic patterns in Zambia and their bearing on problems of Zambian tectonic history     

C.R. Ramsay  J. Ridgway 《Precambrian Research》1977,4(4):321-337

Metamorphic mineral assemblages determined in thin-sections have been used to compile metamorphic maps showing the distribution of metamorphic facies and minerals in Zambia. These maps lead to the recognition of two non-parallel metamorphic belts. The Lufilian Belt curves along the southern margin of the Lufilian (structural) Arc, and the Luangwa—Kariba Belt covers the entire eastern and south-eastern borders of the country. Stratigraphic and mineralogical relationships, and radiometric data, indicate that the two belts are contemporaneous and their present major features are the result of a single tectonothermal episode which ended c. 500 m.y. ago. In particular, the Irumide fold belt is not recognisable as a metamorphic entity.  相似文献   

RX J2115--5840: confirmation of a new near-synchronous polar     

Gavin Ramsay  David A. H. Buckley  Mark Cropper  M. K. Harrop-Allin 《Monthly notices of the Royal Astronomical Society》1999,303(1):96-100

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