A photometrically and kinematically distinct core in the Sextans dwarf spheroidal galaxy     

Jan T. Kleyna  Mark I. Wilkinson  N. Wyn Evans  Gerard Gilmore 《Monthly notices of the Royal Astronomical Society》2004,354(4):L66-L72

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Distant field blue horizontal branch stars – III. Identification of a probable outer halo stream at Galactocentric distance  r= 70 kpc      

L. Clewley  S. J. Warren  P. C. Hewett  John. E. Norris  M. I. Wilkinson  N. W. Evans 《Monthly notices of the Royal Astronomical Society》2005,362(1):349-360

We present FOcal Reducer/low dispersion Spectrograph-1 spectra (from the European Southern Observatory's Very Large Telescope) of a sample of 34 faint  20.0 < g * < 21.1  A-type stars selected from the Sloan Digital Sky Survey Early Data Release, with the goal of measuring the velocity dispersion of blue horizontal branch (BHB) stars in the remote Galactic halo,   R ∼ 80 kpc  . We show that colour selection with  1.08 < u *− g * < 1.40  and  −0.2 < g *− r * < −0.04  minimizes contamination of the sample by less luminous blue stragglers. In classifying the stars we confine our attention to the 20 stars with spectra of signal-to-noise ratio >15 Å⁻¹. Classification produces a sample of eight BHB stars at distances  65–102 kpc  from the Sun (mean 80 kpc), which represents the most distant sample of Galactic stars with measured radial velocities. The dispersion of the measured radial component of the velocity with respect to the centre of the Galaxy is  58 ± 15 km s⁻¹  . This value is anomalously low in comparison with measured values for stars at smaller distances, as well as for satellites at similar distances. Seeking an explanation for the low measured velocity dispersion, further analysis reveals that six of the eight remote BHB stars are plausibly associated with a single orbit. Three previously known outer halo carbon stars also appear to belong to this stream. The velocity dispersion of all nine stars relative to the orbit is only  15 ± 4 km s⁻¹  . Further observations along the orbit are required to trace the full extent of this structure on the sky.  相似文献   

On the Forces Driving Plate Tectonics: Inferences from Absolute Plate Velocities and Intraplate Stress   总被引：1，自引：0，他引：1  

Sean C. Solomon  Norman H. Sleep  Randall M. Richardson 《Geophysical Journal International》1975,42(2):769-801

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First results from the Very Small Array – I. Observational methods     

Robert A. Watson  Pedro Carreira  Kieran Cleary  Rod D. Davies  Richard J. Davis  Clive Dickinson  Keith Grainge †  Carlos M. Gutiérrez  Michael P. Hobson  Michael E. Jones  Rüdiger Kneissl  Anthony Lasenby  Klaus Maisinger  Guy G. Pooley  Rafael Rebolo  José Alberto Rubiño-Martin ‡  Ben Rusholme §  Richard D. E. Saunders  Richard Savage  Paul F. Scott  An&#;e Slosar  Pedro J. Sosa Molina  Angela C. Taylor  David Titterington  Elizabeth Waldram  Althea Wilkinson 《Monthly notices of the Royal Astronomical Society》2003,341(4):1057-1065

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Developing the Gaia Theory. A Response to the Criticisms of Kirchner and Volk     

Timothy M. Lenton  David M. Wilkinson 《Climatic change》2003,58(1-2):1-12

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Tracing the star stream through M31 using planetary nebula kinematics     

H. R. Merrett  K. Kuijken  M. R. Merrifield  A. J. Romanowsky  N. G. Douglas  N. R. Napolitano  M. Arnaboldi  M. Capaccioli  K. C. Freeman  O. Gerhard  N. W. Evans  M. I. Wilkinson  C. Halliday  T. J. Bridges  D. Carter 《Monthly notices of the Royal Astronomical Society》2003,346(4):L62-L66

We present a possible orbit for the Southern Stream of stars in M31, which connects it to the Northern Spur. Support for this model comes from the dynamics of planetary nebulae (PNe) in the disc of M31: analysis of a new sample of 2611 PNe obtained using the Planetary Nebula Spectrograph reveals ∼20 objects with kinematics inconsistent with the normal components of the galaxy, but which lie at the right positions and velocities to connect the two photometric features via this orbit. The satellite galaxy M32 is coincident with the stream both in position and velocity, adding weight to the hypothesis that the stream comprises its tidal debris.  相似文献   

The treatment of observational radio-meteor wind data     

W.J. Baggaley  P.J. Wilkinson 《Planetary and Space Science》1974,22(5):777-787

Contributions to the observed scatter in wind velocity measurement from radiometeors in the 80–110 km height region are investigated in the light of results obtained with a phase coherent pulsed radar system. The major sources of variance considered are the analysis technique, aerial effects and atmospheric variations. It is of importance for published wind data to indicate the significance of derived mean wind velocity values.  相似文献   

Observations of the infrared triplet of singly ionized calcium     

Jeffrey L. Linsky  Richard G. Teske  Carol W. Wilkinson 《Solar physics》1970,11(3):374-383

Observations are presented of the Caii infrared triplet (8498 Å, 8542 Å, and 8662 Å) at three positions on the solar disk to make possible direct analyses of the lines and comparisons with theoretical computations. The source functions for the two strongest lines (8542 Å and 8662 Å) are equal at those heights corresponding to the wings of the lines (¦¦ > 0.4 Å) but not to those of the cores. We suggest that the apparent source function inequality in the cores is due to limb darkening caused by inhomogeneities in the chromosphere.Of the National Bureau of Standards and University of Colorado.  相似文献   

The explosion craters of Basotu,Tanganyika Territory     

C. Downie  P. Wilkinson 《Bulletin of Volcanology》1962,24(1):389-420

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Determination of the properties of Mercury's magnetic field by the MESSENGER mission     

Haje Korth  Brian J. Anderson  James A. Slavin  Sean C. Solomon 《Planetary and Space Science》2004,52(8):733-746

The MESSENGER mission to Mercury, to be launched in 2004, will provide an opportunity to characterize Mercury's internal magnetic field during an orbital phase lasting one Earth year. To test the ability to determine the planetary dipole and higher-order moments from measurements by the spacecraft's fluxgate magnetometer, we simulate the observations along the spacecraft trajectory and recover the internal field characteristics from the simulated observations. The magnetic field inside Mercury's magnetosphere is assumed to consist of an intrinsic multipole component and an external contribution due to magnetospheric current systems described by a modified Tsyganenko 96 model. Under the axis-centered-dipole approximation without correction for the external field the moment strength is overestimated by ∼4% for a simulated dipole moment of , and the error depends strongly on the magnitude of the simulated moment, rising as the moment decreases. Correcting for the external field contributions can reduce the error in the dipole term to a lower limit of ∼1-2% without a solar wind monitor. Dipole and quadrupole terms, although highly correlated, are then distinguishable at the level equivalent to an error in the position of an offset dipole of a few tens of kilometers. Knowledge of the external magnetic field is therefore the primary limiting factor in extracting reliable knowledge of the structure of Mercury's magnetic field from the MESSENGER observations.  相似文献