The low-luminosity galaxy population in the NGC 5044 Group     

Sergio A. Cellone  Alberto Buzzoni 《Monthly notices of the Royal Astronomical Society》2005,356(1):41-53

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Kinematics of ionized gas in the barred Seyfert galaxy NGC 4151     

M. W. Asif  C. G. Mundell  A. Pedlar 《Monthly notices of the Royal Astronomical Society》2005,359(2):408-416

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Effects of dynamical evolution on the distribution of substructures     

Jorge Peñarrubia  Andrew J. Benson 《Monthly notices of the Royal Astronomical Society》2005,364(3):977-989

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A complex analytic solution for the attitude motion of a near-symmetric rigid body under body-fixed torques     

P. Tsiotras  J. M. Longuski 《Celestial Mechanics and Dynamical Astronomy》1991,51(3):281-301

Although analytic solutions for the attitude motion of a rigid body are available for several special cases, a comprehensive theory does not exist in the literature for the more complicated problems found in spacecraft dynamics. In the present paper, analytic solutions in complex form are derived for the attitude motion of a near-symmetric rigid body under the influence of constant body-fixed torques. The solution is very compact, which enables efficient and rapid machine computation. Numerical simulations reveal that the solution is very accurate when applied to typical spinning spacecraft problems.  相似文献   

Galactosynthesis: halo histories, star formation and discs     

Ari Buchalter  Raul Jimenez  Marc Kamionkowski 《Monthly notices of the Royal Astronomical Society》2001,322(1):43-66

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The angular momentum content of dwarf galaxies: new challenges for the theory of galaxy formation     

Frank C. van den Bosch  reas Burkert  Rob A. Swaters 《Monthly notices of the Royal Astronomical Society》2001,326(3):1205-1215

We compute the specific angular momentum distributions for a sample of low-mass disc galaxies observed by Swaters. We compare these distributions to those of dark matter haloes obtained by Bullock et al. from high-resolution N -body simulations of structure formation in a ΛCDM universe. We find that although the disc mass fractions are significantly smaller than the universal baryon fraction, the total specific angular momenta of the discs are in good agreement with those of dark matter haloes. This suggests that discs form out of only a small fraction of the available baryons, but yet manage to draw most of the available angular momentum. In addition we find that the angular momentum distributions of discs are clearly distinct from those of the dark matter; discs lack predominantly both low and high specific angular momenta. Understanding these findings in terms of a coherent picture for disc formation is challenging. Cooling, feedback and stripping, which are the main mechanisms to explain the small disc mass fractions found, seem unable to simultaneously explain the angular momentum distributions of the discs. In fact, it seems that the baryons that make up the discs must have been born out of angular momentum distributions that are clearly distinct from those of ΛCDM haloes. However, the dark and baryonic mass components experience the same tidal forces, and it is therefore expected that they should have similar angular momentum distributions. Therefore, understanding the angular momentum content of disc galaxies remains an important challenge for our picture of galaxy formation.  相似文献   

Regular and chaotic motion in softened gravitational systems     

Amr A.El-Zant† 《Monthly notices of the Royal Astronomical Society》2002,331(1):23-39

The stability of the dynamical trajectories of softened spherical gravitational systems is examined, both in the case of the full N -body problem and that of trajectories moving in the gravitational field of non-interacting background particles. In the latter case, for   N 10 000  , some trajectories, even if unstable, had exceedingly long diffusion times, which correlated with the characteristic e-folding time-scale of the instability. For trajectories of   N ≈100 000  systems this time-scale could be arbitrarily large – and thus appear to correspond to regular orbits. For centrally concentrated systems, low angular momentum trajectories were found to be systematically more unstable. This phenomenon is analogous to the well-known case of trajectories in generic centrally concentrated non-spherical smooth systems, where eccentric trajectories are found to be chaotic. The exponentiation times also correlate with the conservation of the angular momenta along the trajectories. For N up to a few hundred, the instability time-scales of N -body systems and their variation with particle number are similar to those of the most chaotic trajectories in inhomogeneous non-interacting systems. For larger N (up to a few thousand) the values of the these time-scales were found to saturate, increasing significantly more slowly with N . We attribute this to collective effects in the fully self-gravitating problem, which are apparent in the time variations of the time-dependent Liapunov exponents. The results presented here go some way towards resolving the long-standing apparent paradoxes concerning the local instability of trajectories. This now appears to be a manifestation of mechanisms driving evolution in gravitational systems and their interactions – and may thus be a useful diagnostic of such processes.  相似文献   

Orbital dynamics of three-dimensional bars – I. The backbone of three-dimensional bars. A fiducial case     

Ch. Skokos  P. A. Patsis  E. Athanassoula 《Monthly notices of the Royal Astronomical Society》2002,333(4):847-860

In this series of papers we investigate the orbital structure of three-dimensional (3D) models representing barred galaxies. In the present introductory paper we use a fiducial case to describe all families of periodic orbits that may play a role in the morphology of three-dimensional bars. We show that, in a 3D bar, the backbone of the orbital structure is not just the x1 family, as in two-dimensional (2D) models, but a tree of 2D and 3D families bifurcating from x1. Besides the main tree we have also found another group of families of lesser importance around the radial 3:1 resonance. The families of this group bifurcate from x1 and influence the dynamics of the system only locally. We also find that 3D orbits elongated along the bar minor axis can be formed by bifurcations of the planar x2 family. They can support 3D bar-like structures along the minor axis of the main bar. Banana-like orbits around the stable Lagrangian points build a forest of 2D and 3D families as well. The importance of the 3D x1-tree families at the outer parts of the bar depends critically on whether they are introduced in the system as bifurcations in z or in   z˙   .  相似文献   

Edge-on boxy profiles in non-barred disc galaxies     

P. A. Patsis  E. Athanassoula  P. Grosbøl  Ch. Skokos 《Monthly notices of the Royal Astronomical Society》2002,335(4):1049-1053

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Scalar field haloes as gravitational lenses     

Franz E. Schunck  Burkhard Fuchs  Eckehard W. Mielke 《Monthly notices of the Royal Astronomical Society》2006,369(1):485-491

A non-topological soliton model with a repulsive scalar self-interaction of the Emden type provides a constant-density core, similarly as the empirical Burkert profile of dark matter (DM) haloes. As a further test, we derive the gravitational lens properties of our model, in particular, the demarcation curves between 'weak' and 'strong' lensing. Accordingly, strong lensing with typically three images is almost three times more probable for our solitonic model than for the Burkert fit. Moreover, some prospective consequences of a possible flattening of DM haloes are indicated.  相似文献