Energy relaxation in galaxies induced by an external environment and/or incoherent internal pulsations     

Henry E. Kandrup 《Monthly notices of the Royal Astronomical Society》2001,323(3):681-687

This paper explores the phenomenon of energy relaxation for stars in a galaxy embedded in a high-density environment that is subjected continually to perturbations reflecting the presence of other nearby galaxies and/or incoherent internal pulsations. The analysis is similar to earlier analyses of energy relaxation induced by binary encounters between nearby stars and between stars and giant molecular clouds in that the perturbations are idealized as a sum of near-random events which can be modelled as diffusion and dynamical friction. However, the analysis differs in one important respect: because the time-scale associated with these perturbations need not be short compared with the characteristic dynamical time t _D for stars in the original galaxy, the diffusion process cannot be modelled as resulting from a sequence of instantaneous kicks, i.e. white noise. Instead, the diffusion is modelled as resulting from random kicks of finite duration, i.e. coloured noise, characterized by a non-zero autocorrelation time t _c. A detailed analysis of coloured noise generated by sampling an Ornstein–Uhlenbeck process leads to a simple scaling in terms of t _c and an effective diffusion constant D . Interpreting D and t _c following early work by Chandrasekhar (the 'nearest neighbour approximation') implies that, for realistic choices of parameter values, energy relaxation associated with an external environment and/or internal pulsations could be important on times short compared with the age of the Universe.  相似文献   

Morphological and kinematic signatures of a binary central star in the planetary nebula Hu 2-1     

Luis F. Miranda  José M. Torrelles  Martín A. Guerrero  Roberto Vázquez  Yolanda Gómez 《Monthly notices of the Royal Astronomical Society》2001,321(3):487-496

We present H α , [N  ii ] and [O  iii ] ground-based and HST archive images, VLA–A 3.6-cm continuum and H92 α emission-line data and high-resolution long-slit [N  ii ] spectra of the planetary nebula Hu 2-1. A large number of structural components are identified in the nebula: an outer bipolar and an inner shell, two pairs of collimated bipolar structures at different directions, monopolar bow-shock-like structures, and an extended equatorial structure within a halo. The formation of Hu 2-1 appears to be dominated by anisotropic mass ejection during the late-AGB stage of the progenitor and by variable, 'precessing' collimated bipolar outflows during the protoplanetary nebula and/or early planetary nebula phases. Different observational results strongly support the existence of a binary central star in Hu 2-1, among them (1) the observed point-symmetry of the bipolar lobes and inner shell, and the departures from axial symmetry of the bipolar lobes, (2) the off-centre position of the central star, (3) the detection of mass ejection towards the equatorial plane, and (4) the presence of 'precessing' collimated outflows. In addition, (5) an analysis of the kinematics shows that the systemic velocity of the bipolar outflows does not coincide with the systemic velocity of the bipolar shell. We propose that this velocity difference is a direct evidence of orbital motion of the ejection source in a binary system. From a deduced orbital velocity of ∼10 km s⁻¹, a semimajor axis of ∼ 9–27 au and period of ∼ 25–80 yr are obtained, assuming a reasonable range of masses. These parameters are used to analyse the formation of Hu 2-1 within current scenarios of planetary nebulae with binary central stars.  相似文献   

Mass-to-light ratios from the fundamental plane of spiral galaxy discs     

Alister W. Graham † 《Monthly notices of the Royal Astronomical Society》2002,334(4):721-734

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On a matrix method for the study of small perturbations in galaxies     

Peter O. Vandervoort 《Monthly notices of the Royal Astronomical Society》2004,348(2):482-514

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Three-dimensional evolution of worms and chimneys in the Galactic disc     

Miguel A. de Avillez  David L. Berry 《Monthly notices of the Royal Astronomical Society》2001,328(3):708-718

Three-dimensional modelling of the flow of gas and plasma in a section of the Galaxy has been carried out to study the evolution and formation of Galactic chimneys and worms. It is found that clustered supernovae located on either side of the Galactic plane are sources for the formation of well-collimated chimneys, having widths of ∼     . The thick gas disc may have a role in the collimation of chimneys. Channel maps of disc gas, obtained from the simulations, show the presence of sheet-like structures running perpendicular to the Galactic plane and resembling worms. Worms are believed to result from the break-up of the shells and supershells. However, the simulations show that although some worms correlate well with the debris of broken shells/supershells, others do not. They are cold gas that has been accelerated in the disc and rise on to the thick gas disc.  相似文献   

Active tectonics of the north and central Aegean Sea   总被引：20，自引：0，他引：20  

Tuncay Taymaz  James Jackson  Dan McKenzie 《Geophysical Journal International》1991,106(2):433-490

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The evidence for jet–cloud interactions in a sample of high-redshift radio galaxies     

C. Solórzano-Iñarrea  C. N. Tadhunter  D. J. Axon 《Monthly notices of the Royal Astronomical Society》2001,323(4):965-987

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Kinematics of O-B5 giants     

Richard L. Branham Jr  &#; 《Monthly notices of the Royal Astronomical Society》2006,370(3):1393-1400

To study the kinematics of O-B5 giant stars (luminosity class III), 290 non-Gould belt stars with proper motions taken from the Hipparcos catalogue are used, of which 107 have radial velocities taken from other sources. Semidefinite programming solves for the kinematical parameters and the coefficients of the velocity ellipsoid. The condition that both solutions must yield the same solar velocity is enforced. The results obtained are reasonable: solar velocity of 13.83 ± 0.17 km s⁻¹; Oort's constants, in units of km s⁻¹ kpc⁻¹, A = 16.08 ± 0.72 and   B =−10.74 ± 0.65,  implying a rotational velocity of 228.0 ± 21.4 km s⁻¹ if we take the distance to the Galactic Centre as 8.5 ± 1.1 kpc; velocity dispersions, in units of km s⁻¹, of  σ _x = 32.44 ± 5.04, σ _y = 26.16 ± 2.75, σ _z = 18.71 ± 2.39  with a vertex deviation of      相似文献   

Monte Carlo simulations of star clusters – II. Tidally limited, multimass systems with stellar evolution     

Mirek Giersz 《Monthly notices of the Royal Astronomical Society》2001,324(1):218-230

A revision of Stodółkiewicz's Monte Carlo code is used to simulate evolution of large star clusters. The new method treats each superstar as a single star and follows the evolution and motion of all individual stellar objects. A survey of the evolution of N -body systems influenced by the tidal field of a parent galaxy and by stellar evolution is presented. The process of energy generation is realized by means of appropriately modified versions of Spitzer's and Mikkola's formulae for the interaction cross-section between binaries and field stars and binaries themselves. The results presented are in good agreement with theoretical expectations and the results of other methods (Fokker–Planck, Monte Carlo and N -body). The initial rapid mass loss, resulting from stellar evolution of the most massive stars, causes expansion of the whole cluster and eventually leads to the disruption of less bound systems ( W ₀=3). Models with larger W ₀ survive this phase of evolution and then undergo core collapse and subsequent post-collapse expansion, like isolated models. The expansion phase is eventually reversed when tidal limitation becomes important. The results presented are the first major step in the direction of simulating evolution of real globular clusters by means of the Monte Carlo method.  相似文献   

Maximum likelihood estimation of the mean parallax and kinematic parameters of the Pleiades     

Li Chen  Jun-liang Zhao 《Chinese Astronomy and Astrophysics》1997,21(4):471-437

A simultaneous, maximum-likelihood determination of the distance and kinematic parameters of the Pleiades is made. The results are: distance of the cluster d = 135.56 ± 0.72 pc, dispersion σ_d = 7.66 ± 0.80 pc; space velocity V = 25.94 ± 0.13 km/s, dispersion σ_v = 0.58 ± 0.09 km/s coordinates of the convergent point A = 101.95° ± 0.47°, D = −41.36° ± 0.29°.  相似文献