Dust formation in early galaxies     

H. L. Morgan  M. G. Edmunds 《Monthly notices of the Royal Astronomical Society》2003,343(2):427-442

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Are there brown dwarfs in globular clusters?     

I. A. Bonnell  C. J. Clarke  M. R. Bate  M. J. McCaughrean  J. E. Pringle  H. Zinnecker 《Monthly notices of the Royal Astronomical Society》2003,343(3):L53-L57

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The nature, evolution, clustering and X-ray properties of extremely red galaxies in the Chandra Deep Field South/Great Observatories Origins Deep Survey field     

Nathan D. Roche  James Dunlop  Omar Almaini 《Monthly notices of the Royal Astronomical Society》2003,346(3):803-817

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Geometric Derivation of the Delaunay Variables and Geometric Phases     

Dong Eui Chang  Jerrold E. Marsden 《Celestial Mechanics and Dynamical Astronomy》2003,86(2):185-208

We derive the classical Delaunay variables by finding a suitable symmetry action of the three torus T³ on the phase space of the Kepler problem, computing its associated momentum map and using the geometry associated with this structure. A central feature in this derivation is the identification of the mean anomaly as the angle variable for a symplectic S ¹ action on the union of the non-degenerate elliptic Kepler orbits. This approach is geometrically more natural than traditional ones such as directly solving Hamilton–Jacobi equations, or employing the Lagrange bracket. As an application of the new derivation, we give a singularity free treatment of the averaged J ₂-dynamics (the effect of the bulge of the Earth) in the Cartesian coordinates by making use of the fact that the averaged J ₂-Hamiltonian is a collective Hamiltonian of the T³ momentum map. We also use this geometric structure to identify the drifts in satellite orbits due to the J ₂ effect as geometric phases.  相似文献   

Spectroscopic identification of the infrared counterpart to GX5-1     

R. M. Bandyopadhyay  T. Shahbaz  P. A. Charles 《Monthly notices of the Royal Astronomical Society》2003,340(3):L13-L16

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The nature and space density of fossil groups of galaxies     

L. R. Jones  T. J. Ponman  A. Horton  A. Babul †  H. Ebeling  D. J. Burke 《Monthly notices of the Royal Astronomical Society》2003,343(2):627-638

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Dwarf nova oscillations and quasi-periodic oscillations in cataclysmic variables – III. A new kind of dwarf nova oscillation, and further examples of the similarities to X-ray binaries     

Brian Warner  Patrick A. Woudt  Magaretha L. Pretorius 《Monthly notices of the Royal Astronomical Society》2003,344(4):1193-1209

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Photometric study of new southern SU UMa-type dwarf novae and candidates: V877 Ara, KK Tel and PU CMa     

Taichi Kato  Roland Santallo  Greg Bolt  Tom Richards  Peter Nelson  Berto Monard  Makoto Uemura  Seiichiro Kiyota  Rod Stubbings  rew Pearce  Tsutomu Watanabe  Patrick Schmeer  Hitoshi Yamaoka 《Monthly notices of the Royal Astronomical Society》2003,339(3):861-871

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Core dissolution and the dynamics of massive stars in young stellar clusters     

S. G. Vine  I. A. Bonnell 《Monthly notices of the Royal Astronomical Society》2003,342(1):314-320

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Strong interplanetary field enhancements at Ulysses—evidence of dust trails' interaction with the solar wind?     

Geraint H Jones  André Balogh  Robert J MacDowall 《Icarus》2003,166(2):297-310

Interplanetary field enhancements were first discovered in the vicinity of Venus. These events are characterised by an increase in the magnitude of the heliospheric magnetic field with a near-symmetrical, sometimes thorn-shaped profile, and last from minutes to hours. Surveys of the events near Venus and Earth indicated clustering of the events in inertial space, which suggested that their sources were Solar System objects other than the Sun. A survey is presented of strong events of this type detected by the Ulysses spacecraft from 1990 to late 2001. Most of the events are accompanied by a discontinuity in the field direction near the events' centres. Other discontinuities are often symmetrical about the enhancement. The majority of events last less than two hours. When examined as a whole, the events tend to be accompanied by subtle changes in some plasma parameters. The majority of the enhancements are accompanied by magnetic holes on their fringes. The enhancements' occurrence rate increases with decreasing heliocentric distance. Possible formation mechanisms are discussed. No link was found with solar, or solar wind sources. Several aspects of the survey results are consistent with an origin related to cometary dust trails. Possible processes associated with a dust-solar wind interaction are discussed.  相似文献