The pelagic foodweb in the upwelling ecosystem of Galicia (NW Spain) during spring: natural abundance of stable carbon and nitrogen isotopes   总被引：6，自引：1，他引：6  

Bode  Antonio; Carrera  Pablo; Lens  Santiago 《ICES Journal of Marine Science》2003,60(1):11-22

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SCAP meeting no.10     

Mike Bode  Phil Charles  Carlos Frenk 《Astronomy& Geophysics》2001,42(2):2.27-2.28

Mike Bode , Phil Charles and Carlos Frenk report the minutes of the tenth meeting of the Standing Conference of Astronomy Professors, held at the RAS, Burlington House on 30 January 2001.  相似文献   

Grim4-C1, -C2p: combination solutions of the global earth gravity field     

Ch. Reigber  P. Schwintzer  W. Barth  F. H. Massmann  J. C. Raimondo  A. Bode  H. Li  G. Balmino  R. Biancale  B. Moynot  J. M. Lemoine  J. C. Marty  F. Barlier  Y. Boudon 《Surveys in Geophysics》1993,14(4-5):381-393

On the basis of the GRIM4-S1 satellite-only Earth gravity model, being accomplished in a common effort by DGFI and GRGS, a combination solution, called GRIM4-C1, has been derivcd using 1° × 1° mean gravity anomalies and 1° × 1° Seasat altimeter derived mean geoid undulations. In the meantime improvements could be achieved by incorporating more tracking data (GEOSAT, SPOT2-DORIS) into the solution, resulting in the two new parallel versions, the satellite-only gravity model GRIM4-S2 and the combined solution GRIM4-C2p (preliminary). All GRIM4 Earth gravity models cover the spectral gravitational constituents complete up to degree and order 50.In this report the emphasis is on the discussion of the combined gravity models: combination and estimation techniques, capabilities for application in precise satellite orbit computation and accuracies in long wavelength geoid representation. It is shown that with the new generation of global gravity models general purpose satellite-only models are no longer inferior to combination solutions if applied to satellite orbit restitution.  相似文献   

A parameterization of the boundary layer of a tropical cyclone     

L. Bode  R. K. Smith 《Boundary-Layer Meteorology》1975,8(1):3-19

In an earlier paper by one of the authors (Smith, 1968), a momentum integral method was developed to parameterize the gross constraint imposed by the surface boundary layer of a steady, axisymmetric, tropical cyclone on the meridional circulation within the vortex itself. Specifically, the method provides an effective means of estimating the radial variation of mean upflow/downflow induced by the boundary layer, compatible with a prescribed radial variation of azimuthal velocity just above the boundary layer,V _gr. However, it relies on a judicious choice of vertical profiles of radial and azimuthal velocity components within the boundary layer. An especially suitable set of profiles is discussed herein; these are Ekman-like profiles in which turbulent mixing is characterized by a vertically constant eddy diffusivityK _M , matched to a constant stress sublayer just above the sea surface. An attractive feature of the formulation is that a suitable value forK _M as a function of radius, which is extremely difficult to extract from observational data, can be calculated when the state of the sea surface, described by a roughness lengthZ ₀, is prescribed. Although observations ofZ ₀ at high wind speeds are not yet available, the effect of radial variations in sea surface roughness can be assessed and it is shown that these affect the upflow to a significant degree.  相似文献   

Swift observations of the X-ray and UV evolution of V2491 Cyg (Nova Cyg 2008 No. 2)     

K. L. Page  J. P. Osborne  P. A. Evans  G. A. Wynn  A. P. Beardmore  R. L. C. Starling  M. F. Bode  A. Ibarra  E. Kuulkers  J.-U. Ness  G.J. Schwarz 《Monthly notices of the Royal Astronomical Society》2010,401(1):121-130

We present extensive, high-density Swift observations of V2491 Cyg (Nova Cyg 2008 No. 2). Observing the X-ray emission from only one day after the nova discovery, the source is followed through the initial brightening, the super-soft source phase and back to the pre-outburst flux level. The evolution of the spectrum throughout the outburst is demonstrated. The UV and X-ray light curves follow very different paths, although changes occur in them around the same times, indicating a link between the bands. Flickering in the late-time X-ray data indicates the resumption of accretion. We show that if the white dwarf (WD) is magnetic, it would be among the most magnetic known; the lack of a periodic signal in our later data argues against a magnetic WD, however. We also discuss the possibility that V2491 Cyg is a recurrent nova, providing recurrence time-scale estimates.  相似文献   

Interacting winds in classical nova outbursts     

H. M. Lloyd  T. J. O'Brien  M. F. Bode 《Astrophysics and Space Science》1995,233(1-2):317-321

Classical nova outbursts occur in binary systems containing a white dwarf accretor and a Roche-lobe-filling main-sequence star. The outburst is due to a thermonuclear runaway in the accreted material on the surface of the white dwarf, and results in the ejection of up to 10^–4 M of material at velocities of several hundred to a few thousand kilometres per second. There is now strong evidence that the mass ejection takes place via a wind with secularly increasing velocity. The fast ejecta catches up with slower moving material ejected earlier in the outburst, forming a layer of shock-heated gas which gives rise to a short burst of soft X-ray emission. This emission was observed in V838 Her (Nova Herculis 1991), and was succesfully accounted for by the interacting winds model. In this paper, we present 2.5-D numerical hydrodynamics calculations of interacting winds in novae which consider the effects of the binary system on shaping the mass-loss, and show that many of the features seen in the optical shells of novae many years after outburst can be accounted for.This author is supported by a PPARC research assistantship  相似文献   

Thermal and non-thermal radio variations in WR 147     

S. K. Watson  R. J. Davis  P. M. Williams  M. F. Bode 《Monthly notices of the Royal Astronomical Society》2002,334(3):631-636

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The symbiotic star CH Cygni – I. Non-thermal bipolar jets     

M.M. Crocker  R.J. Davis  S.P.S. Eyres  M.F. Bode  A.R. Taylor  A. Skopal  H.T. Kenny 《Monthly notices of the Royal Astronomical Society》2001,326(2):781-787

Very Large Array surface brightness and spectral index maps of the evolving extended emission of the triple symbiotic star CH Cygni are presented. These are derived from observations at 4.8, 8.4 and 14 GHz between 1985 and 1999. The maps are dominated by thermal emission around the central bright peak of the nebula, but we also find unambiguous non-thermal emission associated with the extended regions. Our observations confirm that this is a jet. The central region has been associated with the stellar components through Hubble Space Telescope imaging. If the jets are the result of ejection events at outburst, expansion velocities are consistent with those from other measurement methods. We propose that the non-thermal emission is caused by material ejected in the bipolar jets interacting with the circumstellar wind envelope. The resulting shocks lead to local enhancements in the magnetic field from the compact component of the order of 3 mG.  相似文献   

Tenders: an option for developing countries to support renewable energies under the CDM     

Sven Bode 《Climate Policy》2013,13(2):221-228

Abstract

Renewable energy sources are generally considered as an important tool on the way towards sustainable development. However, if developing countries want to actively promote renewable energies, they may need to face the problem that current legislation conflicts with the clean development mechanism (CDM) rules, and especially with the additionality concept. Thus, CDM projects may become impossible to implement. This article presents an approach to overcoming these potential difficulties. One solution lies in offering a tender specifically for RE-CDM-projects.  相似文献   

Fast identification of bound structures in large N-body simulations     

J. Weller  J. P. Ostriker  P. Bode  L. Shaw 《Monthly notices of the Royal Astronomical Society》2005,364(3):823-732

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