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Lei Zhu Yue-Fang Wu Yue Wei Department of Astronomy Peking University Beijing 《中国天文和天体物理学报》2006,6(1)
We report on a study of the molecular cloud S64 with observations at millimeter wavelengths of multiple molecular lines of CO isotopes.A weak outflow is found,and its physical parameters are estimated.The departure of the core of S64 from the S64 HII region indicates that there are still other star formation activities in that region. 相似文献
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简要综述了近年来对于星际CH3OH脉泽的观测和研究成果,对CH3OH脉泽的性质从分类,生成区域及分布,辐射特性,运动状况等方面做了介绍,并阐明了理论上对其时变特性,激发机制及河外脉泽的探讨,最后对两种类型的CH3OH脉泽作了对比和讨论。 相似文献
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Abstract We discuss the steady states of the αω-dynamo in a thin disc which arise due to α-quenching. Two asymptotic regimes are considered, one for the dynamo numberD near the generation thresholdD 0, and the other for |D| ? 1. Asymptotic solutions for |D—D 0| ? |D 0| have a rather universal character provided only that the bifurcation is supercritical. For |D| ? 1 the asymptotic solution crucially depends on whether or not the mean helicity α, as a function ofB, has a positive root (hereB is the mean magnetic field). When such a root exists, the field value in the major portion of the disc is O(l), while near the disc surface thin boundary layers appear where the field rapidly decreases to zero (if the disc is surrounded by vacuum). Otherwise, when α = O(|B|?s) for |B| → ∞, we demonstrate that |B| = O(|D|1/s ) and the solution is free of boundary layers. The results obtained here admit direct comparison with observations of magnetic fields in spiral galaxies, so that an appropriate model of nonlinear galactic dynamos hopefully could be specified. 相似文献
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John J. Matese Patrick G. Whitman Daniel P. Whitmire 《Celestial Mechanics and Dynamical Astronomy》1997,69(1-2):77-87
We investigate the distribution of Oort cloud comet perihelia. The data considered includes comets having orbital elements
of the two highest quality classes with original energies designated as new or young. Perihelion directions are determined
in galactic, ecliptic and geocentric equatorial coordinates. Asymmetries are detected in the scatter and are studied statistically
for evidence of adiabatic galactic tidal dynamics, an impulse-induced shower and observational bias. The only bias detected
is the well-known deficiency of observations with perihelion distances q > 2.5 AU. There is no significant evidence of a seasonal
dependence. Nor is there a substantive hemispherical bias in either ecliptic or equatorial coordinates. There is evidence
for a weak stellar shower previously detected by Biermann which accounts for ≈ 10% of the total observations. Both the q bias
and the Biermann star track serve to weaken the evidence for a galactic tidal imprint. Nevertheless, statistically significant
asymmetries in galactic latitude and longitude of perihelia remain. A latitude asymmetry is produced by a dominant tidal component
perpendicular to the galactic disk. The longitude signal implies that ≈ 20% of new comets need an additional dynamical mechanism.
Known disk non-uniformities and an hypothetical bound perturber are discussed as potential explanations. We conclude that
the detected dynamical signature of the galactic tide is real and is not an artifact of observational bias, impulsive showers
or poor data.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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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
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