Limits on the 2.2-μm contrast ratio of the close-orbiting planet HD 189733b     

J. R. Barnes  Travis S. Barman  L. Prato  D. Segransan  H. R. A. Jones  C. J. Leigh  A. Collier Cameron  D. J. Pinfield 《Monthly notices of the Royal Astronomical Society》2007,382(1):473-480

We obtained 238 spectra of the close-orbiting extrasolar giant planet HD 189733b with resolution   R ∼ 15 000  during one night of observations with the Near-Infrared High-Resolution Spectrograph (NIRSPEC), at the Keck II Telescope. We have searched for planetary absorption signatures in the  2.0–2.4 μm  region where H₂O and CO are expected to be the dominant atmospheric opacities. We employ a phase-dependent orbital model and tomographic techniques to search for the planetary absorption signatures in the combined stellar and planetary spectra. Because potential absorption signatures are hidden in the noise of each single exposure, we use a model list of lines to apply a spectral deconvolution. The resulting mean profile possesses a signal-to-noise ratio (S/N) that is 20 times greater than that found in individual lines. Our spectral time series thus yields spectral signatures with a mean S/N = 2720. We are unable to detect a planetary signature at a contrast ratio of  log₁₀( F _p/ F _*) =−3.40  , with 63.8 per cent confidence. Our findings are not consistent with model predictions which nevertheless give a good fit to mid-infrared observations of HD 189733b. The 1σ result is a factor of 1.7 times less than the predicted 2.185-μm planet/star flux ratio of  log₁₀( F _p/ F _*) ∼−3.16  .  相似文献   

Eighth voyage of the dragon A history of China's quest for seapower: Bruce SwansonUS Naval Institute Press,Annapolis, MD, 1982, 348 pp     

Donald Cameron Watt 《Marine Policy》1984,8(1):69-71

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Formation of the prelunar accretion disk     

A.G.W. Cameron 《Icarus》1985,62(2):319-327

According to the single-impact hypothesis for forming the Moon, the angular momentum needed for the present Earth-Moon system can be imparted to the proto-Earth by a collision with a body having one-tenth of the mass or more. The collision must vaporize a large amount of rock which must stay in the form of vapor after expanding in density by a factor of several, so that pressure gradients can accelerate significant amounts of the matter into orbital motion about the proto-Earth. A successful theory must put considerably more than a lunar mass into orbit, having considerably more angular momentum than is needed to assemble a lunar mass in orbit at 3 Earth radii. Such a collision has been simulated by a particular form of a particle-in-cell representation of hydrodynamics and 78 cases have been run representing variations in a variety of parameters. A significant fraction of the cases were successful in creating a satisfactory prelunar accretion disk. A fairly common characteristic of these cases was the presence of an excess velocity in the collision (above that of a parabolic orbit), implying that the projectile involved in the collision existed in an Earth-crossing orbit of significant ellipticity. A majority of the mass of the prelunar accretion disk is contributed by the projectile.  相似文献   

Temporal fluctuations in the differential rotation of cool active stars     

J.-F. Donati  A. Collier Cameron  P. Petit 《Monthly notices of the Royal Astronomical Society》2003,345(4):1187-1199

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INGRID: A near-infrared camera for the William Herschel Telescope     

Christopher Packham  Keith L. Thompson  Almudena Zurita  Johan H. Knapen  Ian Smail  Robert Greimel  Daniel F. M. Folha  Chris Benn  rew Humphrey  Rene Rutten  David Ciardi  Matthieu Bec  Richard Bingham  Simon Craig  Kevin Dee  Derek Ives  Paul Jolley  Peter Moore  Marti Pi i Puig  Simon Rees  Gordon Talbot  Sue Worswick 《Monthly notices of the Royal Astronomical Society》2003,345(2):395-405

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Possible influence of comets on the chemical evolution of the galaxy     

Beatrice M. Tinsley  A. G. W. Cameron 《Astrophysics and Space Science》1974,31(1):31-35

It has been suggested by Cameron that a cloud of comets containing a mass of condensable elements, comparable to the mass of such elements in the sun, formed on the outskirts of the solar system. If the formation of such comet clouds is a general feature of star formation, they constitute a significant sink of elements heavier than helium. It is shown here that this process provides a possible explanation for the very slow rate at which the mean metal abundance of disk stars has increased during the lifetime of the Galaxy.  相似文献   

International Conference for Ocean Mining: Düsseldorf,FR Germany, 15 May 1981     

Hugh Cameron  Jonathan Simnett 《Marine Policy》1982,6(2):156-157

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An equation of state at subnuclear densities     

William D. Langer  Leonard C. Rosen  Jeffrey M. Cohen  A. G. W. Cameron 《Astrophysics and Space Science》1969,5(3):259-271

An equation of state for cold matter above white dwarf densities is evaluated. The gas is considered to be a mixture of degenerate neutrons, protons and electrons combined with nuclei of one type (that is only oneA andZ value). We derive the equilibrium equations for the mixture and calculate the number densities as well as theA andZ of the nucleus. Finally we calculate an equation of state, which smoothly goes over to that of a neutron, proton electron gas mixture at a density of 5×10¹³ g/cm³.  相似文献   

Pregalactic nucleosynthesis     

T. W. Hartquist  A. G. W. Cameron 《Astrophysics and Space Science》1977,48(1):145-158

We discuss the behavior of density fluctuations in an expanding universe and show that these should lead to the early formation of pregalactic hydrogen-helium stars of several hundred to several thousand solar masses. These stars flood the universe with radiation having a color temperature ≳10⁵ K; this terminates star formation but permits galaxy formation to continue. About 10⁻² of the mass of the galaxies is converted into heavy elements by pregalactic nucleosynthesis, with an error factor of a few.  相似文献   

Neutron star models based on an improved equation of state     

Jeffrey M. Cohen  William D. Langer  Leonard C. Rosen  A. G. W. Cameron 《Astrophysics and Space Science》1970,6(2):228-239

Using an equation of state for cold degenerate matter which takes nuclear forces and nuclear clustering into account, neutron star models are constructed. Stable models were obtained in the mass range above 0.065M and density range 10^14.08 to 10^15.4 gm/cm³. All of these models were found to be bound. The outer crystalline layer of the star was found to have a thickness of 200 m or more depending on the mass of the model.  相似文献