A bivariate gamma distribution for use in multivariate flood frequency analysis     

Sheng Yue 《水文研究》2001,15(6):1033-1045

A gamma distribution is one of the most frequently selected distribution types for hydrological frequency analysis. The bivariate gamma distribution with gamma marginals may be useful for analysing multivariate hydrological events. This study investigates the applicability of a bivariate gamma model with five parameters for describing the joint probability behavior of multivariate flood events. The parameters are proposed to be estimated from the marginal distributions by the method of moments. The joint distribution, the conditional distribution, and the associated return periods are derived from marginals. The usefulness of the model is demonstrated by representing the joint probabilistic behaviour between correlated flood peak and flood volume and between correlated flood volume and flood duration in the Madawask River basin in the province of Quebec, Canada. Copyright © 2001 John Wiley & Sons, Ltd.  相似文献   

Star Formation in Violent and Normal Evolutionary Phases     

Uta Fritze – von Alvensleben 《Astrophysics and Space Science》2002,281(1-2):379-382

Mergers of massive gas-rich galaxies trigger violent starbursts that - over timescales of > 100 Myr and regions > 10 kpc - form massive and compact star clusters comparable in mass and radii to Galactic globular clusters. The star formation efficiency is higher by 1–2 orders of magnitude in these bursts than in undisturbed spirals, irregulars or even BCDs. We ask the question if star formation in these extreme regimes is just a scaled-up version of the normal star formation mode of if the formation of globular clusters reveals fundamentally different conditions. This revised version was published online in September 2006 with corrections to the Cover Date.  相似文献   

Multiple X-ray reflection from ionized slabs     

R. R. Ross  A. C. Fabian  D. R. Ballantyne 《Monthly notices of the Royal Astronomical Society》2002,336(1):315-318

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Molecular gas freeze-out in the pre-stellar core L1689B     

M. P. Redman  J. M. C. Rawlings  D. J. Nutter  D. Ward-Thompson  D. A. Williams 《Monthly notices of the Royal Astronomical Society》2002,337(3):L17-L21

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The quasi-steady state cosmology: Some recent developments     

Jayant V. Narlikar 《Journal of Astrophysics and Astronomy》1997,18(4):353-362

This paper summarises the recent work on the quasi-steady state cosmology. This includes, the theoretical formulation and simple exact solutions of the basic equations, their relationship to observations, the stability of solutions and the toy model for understanding the growth of structures in the universe.  相似文献   

The gravitational instability in the dust layer of a protoplanetary disk:: axisymmetric solutions for nonuniform dust density distributions in the direction vertical to the midplane     

Fumiharu Yamoto  Minoru Sekiya 《Icarus》2004,170(1):180-192

The gravitational instability in the dust layer of a protoplanetary disk with nonuniform dust density distributions in the direction vertical to the midplane is investigated. The linear analysis of the gravitational instability is performed. The following assumptions are used: (1) One fluid model is adopted, that is, difference of velocities between dust and gas are neglected. (2) The gas is incompressible. (3) Models are axisymmetric with respect to the rotation axis of the disk. Numerical results show that the critical density at the midplane is higher than the one for the uniform dust density distribution by Sekiya (1983, Prog. Theor. Phys. 69, 1116-1130). For the Gaussian dust density distribution, the critical density is 1.3 times higher, although we do not consider this dust density distribution to be realistic because of the shear instability in the dust layer. For the dust density distribution with a constant Richardson number, which is considered to be realized due to the shear instability, the critical density is 2.85 times higher and is independent of the value of the Richardson number. Further, if a constant Richardson number could decrease to the order of 0.001, the gravitational instability would be realized even for the dust to gas surface density ratio with the solar abundance. Our results give a new restriction on planetesimal formation by the gravitational instability.  相似文献   

The effect of a finite mass reservoir on the collapse of spherical isothermal clouds and the evolution of protostellar accretion     

E. I. Vorobyov  Shantanu Basu 《Monthly notices of the Royal Astronomical Society》2005,360(2):675-684

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Host galaxies of gamma-ray bursts and their cosmological evolution     

Stéphanie Courty  Gunnlaugur Björnsson  Einar H. Gudmundsson 《Monthly notices of the Royal Astronomical Society》2004,354(2):581-590

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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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Scaling up tides in numerical models of galaxy and halo formation     

C. M. Boily †  E. Athanassoula  P. Kroupa 《Monthly notices of the Royal Astronomical Society》2002,332(4):971-984

The purpose of this article is to show that when dynamically cold, dissipationless self-gravitating systems collapse, their evolution is a strong function of the symmetry in the initial distribution. We explore with a set of pressureless homogeneous fluids the time evolution of ellipsoidal distributions and map the depth of potential achieved during relaxation as function of initial ellipsoid axis ratios. We then perform a series of N -body numerical simulations and contrast their evolution with the fluid solutions. We verify an analytic relation between collapse factor and particle number N in spherical symmetry, such that  ∝ N ^1/3  . We sought a similar relation for axisymmetric configurations, and found an empirical scaling relation such that  ∝ N ^1/6  in these cases. We then show that when mass distributions do not respect spherical or axial symmetry, the ensuing gravitational collapse deepens with increasing particle number N but only slowly: 86 per cent of triaxial configurations may collapse by a factor of no more than 40 as   N →∞  . For   N ≈10⁵  and larger, violent relaxation develops fully under the Lin–Mestel–Shu instability such that numerical N -body solutions now resolve the different initial morphologies adequately.  相似文献